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Author name code: zuccarello
ADS astronomy entries on 2022-09-14
author:"Zuccarello, Francesca"
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Title: The umbral filament of active region NOAA 12529
Authors: Guglielmino, Salvatore Luigi; Romano, Paolo; Zuccarello,
Francesca; Murabito, Mariarita; Ruiz Cobo, Basilio
2022cosp...44.2453G Altcode:
Umbral filaments are elongated, filamentary bright structures inside
sunspot umbrae, which differ in morphology, magnetic configuration,
and evolution from light bridges usually observed in sunspots. We
investigated an umbral filament (UF) observed in the umbra of the giant
leading sunspot of active region NOAA 12529, analyzing high-resolution
observations taken in the photosphere with the spectropolarimeter
aboard the \textit{Hinode} satellite and in the upper chromosphere and
transition region with the \textit{IRIS} telescope. We recognize in
the UF the presence of a strong horizontal field larger than 2500 G,
a significant portion of the UF with opposite polarity with respect
to the surroundings, and filaments in the upper atmospheric layers
corresponding to the UF in the photosphere. These findings suggest
that this UF is the photospheric manifestation of a flux rope hanging
above the sunspot and forming penumbral-like filaments within the
umbra via magneto-convection.
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Title: Quantifying Properties of Photospheric Magnetic Cancellations
in the Quiet Sun Internetwork
Authors: Ledvina, Vincent E.; Kazachenko, Maria D.; Criscuoli, Serena;
Tilipman, Dennis; Ermolli, Ilaria; Falco, Mariachiara; Guglielmino,
Salvatore; Jafarzadeh, Shahin; van der Voort, Luc Rouppe; Zuccarello,
Francesca
2022ApJ...934...38L Altcode: 2022arXiv220604644L
We analyzed spectropolarimetric data from the Swedish 1 m Solar
Telescope to investigate the physical properties of small-scale magnetic
cancellations in the quiet Sun photosphere. Specifically, we looked at
the full Stokes polarization profiles along the Fe I 557.6 nm and of the
Fe I 630.1 nm lines measured by the CRisp Imaging SpectroPolarimeter to
study the temporal evolution of the line-of-sight magnetic field during
42.5 minutes of quiet Sun evolution. From this magnetogram sequence, we
visually identified 38 cancellation events. We then used the Yet Another
Feature Tracking Algorithm to characterize the physical properties of
these magnetic cancellations. We found on average 1.6 × 10<SUP>16</SUP>
Mx of magnetic flux canceled in each event with an average cancellation
rate of 3.8 × 10<SUP>14</SUP> Mx s<SUP>-1</SUP>. The derived canceled
flux is associated with strong downflows, with an average speed of V
<SUB>LOS</SUB> ≍ 1.1 km s<SUP>-1</SUP>. Our results show that the
average lifetime of each event is 9.2 minutes with an average of 44.8%
of initial magnetic flux being canceled. Our estimates of magnetic
fluxes provide a lower limit since studied magnetic cancellation events
have magnetic field values that are very close to the instrument noise
level. We observed no horizontal magnetic fields at the cancellation
sites and therefore cannot conclude whether the events are associated
with structures that could cause magnetic reconnection.
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Title: The Solar Activity Monitor Network - SAMNet
Authors: Erdélyi, Robertus; Korsós, Marianna B.; Huang, Xin; Yang,
Yong; Pizzey, Danielle; Wrathmall, Steven A.; Hughes, Ifan G.;
Dyer, Martin J.; Dhillon, Vikram S.; Belucz, Bernadett; Brajša,
Roman; Chatterjee, Piyali; Cheng, Xuewu; Deng, Yuanyong; Domínguez,
Santiago Vargas; Joya, Raúl; Gömöry, Peter; Gyenge, Norbert G.;
Hanslmeier, Arnold; Kucera, Ales; Kuridze, David; Li, Faquan; Liu,
Zhong; Xu, Long; Mathioudakis, Mihalis; Matthews, Sarah; McAteer,
James R. T.; Pevtsov, Alexei A.; Pötzi, Werner; Romano, Paolo; Shen,
Jinhua; Temesváry, János; Tlatov, Andrey G.; Triana, Charles; Utz,
Dominik; Veronig, Astrid M.; Wang, Yuming; Yan, Yihua; Zaqarashvili,
Teimuraz; Zuccarello, Francesca
2022JSWSC..12....2E Altcode:
The Solar Activity Magnetic Monitor (SAMM) Network (SAMNet) is a
future UK-led international network of ground-based solar telescope
stations. SAMNet, at its full capacity, will continuously monitor
the Sun's intensity, magnetic, and Doppler velocity fields at
multiple heights in the solar atmosphere (from photosphere to upper
chromosphere). Each SAMM sentinel will be equipped with a cluster of
identical telescopes each with a different magneto-optical filter (MOFs)
to take observations in K I, Na D, and Ca I spectral bands. A subset
of SAMM stations will have white-light coronagraphs and emission line
coronal spectropolarimeters. The objectives of SAMNet are to provide
observational data for space weather research and forecast. The goal
is to achieve an operationally sufficient lead time of e.g., flare
warning of 2-8 h and provide many sought-after continuous synoptic
maps (e.g., LoS magnetic and velocity fields, intensity) of the lower
solar atmosphere with a spatial resolution limited only by seeing or
diffraction limit, and with a cadence of 10 min. The individual SAMM
sentinels will be connected to their master HQ hub where data received
from all the slave stations will be automatically processed and flare
warning issued up to 26 h in advance.
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Title: HiRISE - High-Resolution Imaging and Spectroscopy Explorer
- Ultrahigh resolution, interferometric and external occulting
coronagraphic science
Authors: Erdélyi, Robertus; Damé, Luc; Fludra, Andrzej; Mathioudakis,
Mihalis; Amari, T.; Belucz, B.; Berrilli, F.; Bogachev, S.; Bolsée,
D.; Bothmer, V.; Brun, S.; Dewitte, S.; de Wit, T. Dudok; Faurobert,
M.; Gizon, L.; Gyenge, N.; Korsós, M. B.; Labrosse, N.; Matthews,
S.; Meftah, M.; Morgan, H.; Pallé, P.; Rochus, P.; Rozanov, E.;
Schmieder, B.; Tsinganos, K.; Verwichte, E.; Zharkov, S.; Zuccarello,
F.; Wimmer-Schweingruber, R.
2022ExA...tmp...21E Altcode:
Recent solar physics missions have shown the definite role of waves and
magnetic fields deep in the inner corona, at the chromosphere-corona
interface, where dramatic and physically dominant changes occur. HiRISE
(High Resolution Imaging and Spectroscopy Explorer), the ambitious new
generation ultra-high resolution, interferometric, and coronagraphic,
solar physics mission, proposed in response to the ESA Voyage 2050
Call, would address these issues and provide the best-ever and most
complete solar observatory, capable of ultra-high spatial, spectral,
and temporal resolution observations of the solar atmosphere, from the
photosphere to the corona, and of new insights of the solar interior
from the core to the photosphere. HiRISE, at the L1 Lagrangian
point, would provide meter class FUV imaging and spectro-imaging,
EUV and XUV imaging and spectroscopy, magnetic fields measurements,
and ambitious and comprehensive coronagraphy by a remote external
occulter (two satellites formation flying 375 m apart, with a
coronagraph on a chaser satellite). This major and state-of-the-art
payload would allow us to characterize temperatures, densities, and
velocities in the solar upper chromosphere, transition zone, and inner
corona with, in particular, 2D very high resolution multi-spectral
imaging-spectroscopy, and, direct coronal magnetic field measurement,
thus providing a unique set of tools to understand the structure and
onset of coronal heating. HiRISE's objectives are natural complements
to the Parker Solar Probe and Solar Orbiter-type missions. We present
the science case for HiRISE which will address: i) the fine structure
of the chromosphere-corona interface by 2D spectroscopy in FUV at
very high resolution; ii) coronal heating roots in the inner corona by
ambitious externally-occulted coronagraphy; iii) resolved and global
helioseismology thanks to continuity and stability of observing at the
L1 Lagrange point; and iv) solar variability and space climate with,
in addition, a global comprehensive view of UV variability.
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Title: On the Evolution of a Sub-C Class Flare: A Showcase for the
Capabilities of the Revamped Catania Solar Telescope
Authors: Romano, Paolo; Guglielmino, Salvo L.; Costa, Pierfrancesco;
Falco, Mariachiara; Buttaccio, Salvatore; Costa, Alessandro;
Martinetti, Eugenio; Occhipinti, Giovanni; Spadaro, Daniele; Ventura,
Rita; Capuano, Giuseppe E.; Zuccarello, Francesca
2022SoPh..297....7R Altcode: 2021arXiv211108972R
Solar flares are occasionally responsible for severe space-weather
events, which can affect space-borne and ground-based infrastructures,
endangering anthropic technological activities and even human health and
safety. Thus, an essential activity in the framework of space-weather
monitoring is devoted to the observation of the activity level on
the Sun. In this context, the acquisition system of the Catania
Solar Telescope has been recently upgraded in order to improve its
contribution to the European Space Agency (ESA) - Space Weather Service
Network through the ESA Portal, which represents the main asset for
space weather in Europe. Here, we describe the hardware and software
upgrades of the Catania Solar Telescope and the main data products
provided by this facility, which include full-disk images of the
photosphere and chromosphere, together with a detailed characterization
of sunspot groups. As a showcase of the observational capabilities of
the revamped Catania Solar Telescope, we report the analysis of a B5.4
class flare that occurred on 7 December 2020, simultaneously observed
by the Interface Region Imaging Spectrograph and the Solar Dynamics
Observatory satellites.
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Title: Comparative case study of two methods to assess the eruptive
potential of selected active regions
Authors: Zuccarello, Francesca; Ermolli, Ilaria; Korsós, Marianna
B.; Giorgi, Fabrizio; Guglielmino, Salvo L.; Erdélyi, Robertus;
Romano, Paolo
2021RAA....21..313Z Altcode: 2022RAA....21..313Z; 2021arXiv211001272Z
Solar eruptive events, like flares and coronal mass ejections, are
characterized by the rapid release of energy that can give rise to
emission of radiation across the entire electromagnetic spectrum and to
an abrupt significant increase in the kinetic energy of particles. These
energetic phenomena can have important effects on the space weather
conditions and therefore it is necessary to understand their origin, in
particular, what is the eruptive potential of an active region (AR). In
these case studies, we compare two distinct methods that were used in
previous works to investigate the variations of some characteristic
physical parameters during the pre-flare states of flaring ARs. These
methods consider: i) the magnetic flux evolution and magnetic helicity
accumulation, and ii) the fractal and multi-fractal properties of
flux concentrations in ARs. Our comparative analysisis based on time
series of photospheric data obtained bythe Solar Dynamics Observatory
between March 2011 and June 2013. We selected two distinct samples
of ARs: one is distinguished by the occurrence of more energetic M-
and X-class flare events, that may have a rapid effect on not just the
near-Earth space, but also on the terrestrial environment; the second
is characterized by no-flares or having just a few C- and B-class
flares. We foundthat the two tested methods complement each other
in their ability to assess the eruptive potentials of ARs and could
be employed to identify ARs prone to flaring activity. Based on the
presented case study, we suggest that using a combination of different
methods may aid to identify more reliably the eruptive potentials of
ARs and help to better understand the pre-flare states.
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Title: Quo vadis, European Space Weather community?
Authors: Lilensten, Jean; Dumbović, Mateja; Spogli, Luca; Belehaki,
Anna; Van der Linden, Ronald; Poedts, Stefaan; Barata, Teresa; Bisi,
Mario M.; Cessateur, Gaël; De Donder, Erwin; Guerrero, Antonio;
Kilpua, Emilia; Korsos, Marianna B.; Pinto, Rui F.; Temmer, Manuela;
Tsagouri, Ioanna; Urbář, Jaroslav; Zuccarello, Francesca
2021JSWSC..11...26L Altcode:
This paper was written by a group of European researchers believing
that now is the right time to frame the Space Weather and Space
Climate discipline in Europe for future years. It is devoted to
openly discussing the organisation and sustainability of the European
Space Weather community and its assets in the (near) future. More
specifically, we suggest that the European Space Weather community
lacks a uniting organisation to help the community to sustain and
develop the successful efforts made thus far. Our aim is not to draw
a complete and exhaustive panorama of Space Weather throughout the
world, nor even throughout Europe. It is not a new white paper on the
science and applications: there exist many (e.g. Tsurutani et al.,
2020 Nonlinear Processes Geophys 27(1): 75-119); nor another roadmap:
several important have been published recently (e.g. Schrijver et al.,
2015. Adv Space Res 55(12): 2745-2807; Opgenoorth et al., 2019. J Space
Weather Space Clim 9: A37). Our aim is to question our practices and
organisation in front of several changes that have occurred in the
recent years and to set the ground to provide coordinated answers
to these questions being posed in Europe, and to make these answers
discussed throughout the world. This group was assembled first through
a series of sessions devoted to the sustainability of Space Weather
research during the European Space Weather Week (ESWW) series of
meetings, specifically: ESWW 14 (2017), ESWW 15 (2018), and ESWW 16
(2019). It then grew from discussions and personal contacts. The authors
do not pretend to identify the full range of opinions in Europe,
although they do come from 13 different European countries with a
large span of ages (around half are below the age of 40 years old at
the time of writing) with a good gender balance ending with a diverse
mix of young and motivated scientists and senior people who have played
a role in shaping the Space Weather community in Europe. The questions
and the propositions to organise Space Weather in Europe in the future
result from their discussions through these meetings and through remote
meetings during the pandemic. We wish to share them with all those who
consider themselves as members of the European Space Weather community
and/or are interested in its future and to propose actions. We do this,
bearing in mind that Europe plays a key international role in Space
Weather which extends beyond the ESA and EU/EC geographic area.
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Title: Investigation of the X1.6 Flare Occurred in the Great Active
Region 12192
Authors: Zuccarello, F.; Guglielmino, S. L.; Ferrente, F.; Criscuoli,
S.; Romano, P.
2020AGUFMSH0430003Z Altcode:
The X1.6 flare observed on 22 October 2014 (SOL2014-10-22T14:28)
was among the strongest flares occurred in the magnetically complex,
great active region NOAA 12192. It was a confined flare, without an
accompanying CME, despite the large amount of released energy. Here,
we report on full spectro-polarimetric observations acquired by
the IBIS/DST instrument along the Ca II 8542 line, analyzing the
polarization signatures during the flare, together with complementary
data from SDO and IRIS. We attempt to derive new information about
the chromospheric magnetic field topology, which can help to explain
the lack of ejecta.
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Title: IBIS2.0: The new Interferometric BIdimensional Spectrometer
Authors: Ermolli, Ilaria; Cirami, Roberto; Calderone, Giorgio; Del
Moro, Dario; Romano, Paolo; Viavattene, Giorgio; Coretti, Igor; Giorgi,
Fabrizio; Baldini, Veronica; Di Marcantonio, Paolo; Giovannelli, Luca;
Guglielmino, Salvatore Luigi; Murabito, Mariarita; Pedichini, Fernando;
Piazzesi, Roberto; Aliverti, Matteo; Redaelli, Edoardo Maria Alberto;
Berrilli, Francesco; Zuccarello, Francesca
2020SPIE11447E..0ZE Altcode:
We present the IBIS2.0 project, which aims to upgrade and to install
the Interferometric BIdimensional Spectrometer at the solar Vacuum Tower
Telescope (Tenerife, Spain) after its disassembling from the Dunn Solar
Telescope (New Mexico, USA). The instrument is undergoing a hardware and
software revision that will allow it to perform new spectropolarimetric
measurements of the solar atmosphere at high spatial, spectral and
temporal resolution in coordination with other ground- and space-based
instruments. Here we present the new opto-mechanical layout and control
system designed for the instrument, and describe future steps.
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Title: Reconstruction of events recorded with the surface detector
of the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albury, J. M.; Allekotte,
I.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves
Batista, R.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.; Andringa,
S.; Aramo, C.; Araújo Ferreira, P. R.; Asorey, H.; Assis, P.; Avila,
G.; Badescu, A. M.; Bakalova, A.; Balaceanu, A.; Barbato, F.; Barreira
Luz, R. J.; Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.;
Bertou, X.; Biermann, P. L.; Billoir, P.; Bister, T.; Biteau, J.;
Blanco, A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.;
Bonifazi, C.; Bonneau Arbeletche, L.; Borodai, N.; Botti, A. M.;
Brack, J.; Bretz, T.; Bridgeman, A.; Briechle, F. L.; Buchholz,
P.; Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.;
Caccianiga, L.; Calcagni, L.; Cancio, A.; Canfora, F.; Caracas, I.;
Carceller, J. M.; Caruso, R.; Castellina, A.; Catalani, F.; Cataldi,
G.; Cazon, L.; Cerda, M.; Chinellato, J. A.; Choi, K.; Chudoba, J.;
Chytka, L.; Clay, R. W.; Cobos Cerutti, A. C.; Colalillo, R.; Coleman,
A.; Coluccia, M. R.; Conceição, R.; Condorelli, A.; Consolati, G.;
Contreras, F.; Convenga, F.; Covault, C. E.; Dasso, S.; Daumiller,
K.; Dawson, B. R.; Day, J. A.; de Almeida, R. M.; de Jesús, J.;
de Jong, S. J.; De Mauro, G.; de Mello Neto, J. R. T.; De Mitri, I.;
de Oliveira, J.; de Oliveira Franco, D.; de Souza, V.; De Vito, E.;
Debatin, J.; del Río, M.; Deligny, O.; Dhital, N.; Di Matteo, A.;
Díaz Castro, M. L.; Dobrigkeit, C.; D'Olivo, J. C.; Dorosti, Q.; dos
Anjos, R. C.; Dova, M. T.; Ebr, J.; Engel, R.; Epicoco, I.; Erdmann,
M.; Escobar, C. O.; Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar,
G.; Fauth, A. C.; Fazzini, N.; Feldbusch, F.; Fenu, F.; Fick, B.;
Figueira, J. M.; Filipčič, A.; Fodran, T.; Freire, M. M.; Fujii, T.;
Fuster, A.; Galea, C.; Galelli, C.; García, B.; Garcia Vegas, A. L.;
Gemmeke, H.; Gesualdi, F.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari,
U.; Giammarchi, M.; Giller, M.; Glombitza, J.; Gobbi, F.; Gollan, F.;
Golup, G.; Gómez Berisso, M.; Gómez Vitale, P. F.; Gongora, J. P.;
González, N.; Goos, I.; Góra, D.; Gorgi, A.; Gottowik, M.; Grubb,
T. D.; Guarino, F.; Guedes, G. P.; Guido, E.; Hahn, S.; Halliday, R.;
Hampel, M. R.; Hansen, P.; Harari, D.; Harvey, V. M.; Haungs, A.;
Hebbeker, T.; Heck, D.; Hill, G. C.; Hojvat, C.; Hörandel, J. R.;
Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman, J.; Insolia, A.; Isar,
P. G.; Johnsen, J. A.; Jurysek, J.; Kääpä, A.; Kampert, K. H.;
Keilhauer, B.; Kemp, J.; Klages, H. O.; Kleifges, M.; Kleinfeller,
J.; Köpke, M.; Kukec Mezek, G.; Lago, B. L.; LaHurd, D.; Lang,
R. G.; Leigui de Oliveira, M. A.; Lenok, V.; Letessier-Selvon, A.;
Lhenry-Yvon, I.; Lo Presti, D.; Lopes, L.; López, R.; Lorek, R.; Luce,
Q.; Lucero, A.; Machado Payeras, A.; Malacari, M.; Mancarella, G.;
Mandat, D.; Manning, B. C.; Manshanden, J.; Mantsch, P.; Marafico, S.;
Mariazzi, A. G.; Mariş, I. C.; Marsella, G.; Martello, D.; Martinez,
H.; Martínez Bravo, O.; Mastrodicasa, M.; Mathes, H. J.; Matthews,
J.; Matthiae, G.; Mayotte, E.; Mazur, P. O.; Medina-Tanco, G.; Melo,
D.; Menshikov, A.; Merenda, K. -D.; Michal, S.; Micheletti, M. I.;
Miramonti, L.; Mockler, D.; Mollerach, S.; Montanet, F.; Morello,
C.; Mostafá, M.; Müller, A. L.; Muller, M. A.; Mulrey, K.; Mussa,
R.; Muzio, M.; Namasaka, W. M.; Nellen, L.; Niculescu-Oglinzanu,
M.; Niechciol, M.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.;
Nucita, A.; Núñez, L. A.; Palatka, M.; Pallotta, J.; Panetta,
M. P.; Papenbreer, P.; Parente, G.; Parra, A.; Pech, M.; Pedreira,
F.; Pȩkala, J.; Pelayo, R.; Peña-Rodriguez, J.; Perez Armand, J.;
Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.; Pierog, T.; Pimenta,
M.; Pirronello, V.; Platino, M.; Pont, B.; Pothast, M.; Privitera, P.;
Prouza, M.; Puyleart, A.; Querchfeld, S.; Rautenberg, J.; Ravignani,
D.; Reininghaus, M.; Ridky, J.; Riehn, F.; Risse, M.; Ristori, P.;
Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Rojo, J.; Roncoroni,
M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl, P.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Salina, G.; Sanabria Gomez,
J. D.; Sánchez, F.; Santos, E. M.; Santos, E.; Sarazin, F.; Sarmento,
R.; Sarmiento-Cano, C.; Sato, R.; Savina, P.; Schäfer, C.; Scherini,
V.; Schieler, H.; Schimassek, M.; Schimp, M.; Schlüter, F.; Schmidt,
D.; Scholten, O.; Schovánek, P.; Schröder, F. G.; Schröder, S.;
Schulz, A.; Sciutto, S. J.; Scornavacche, M.; Shellard, R. C.; Sigl,
G.; Silli, G.; Sima, O.; Šmída, R.; Sommers, P.; Soriano, J. F.;
Souchard, J.; Squartini, R.; Stadelmaier, M.; Stanca, D.; Stanič, S.;
Stasielak, J.; Stassi, P.; Streich, A.; Suárez-Durán, M.; Sudholz,
T.; Suomijärvi, T.; Supanitsky, A. D.; Šupík, J.; Szadkowski,
Z.; Taboada, A.; Tapia, A.; Timmermans, C.; Tkachenko, O.; Tobiska,
P.; Todero Peixoto, C. J.; Tomé, B.; Torralba Elipe, G.; Travaini,
A.; Travnicek, P.; Trimarelli, C.; Trini, M.; Tueros, M.; Ulrich, R.;
Unger, M.; Urban, M.; Vaclavek, L.; Vacula, M.; Valdés Galicia, J. F.;
Valiño, I.; Valore, L.; van Vliet, A.; Varela, E.; Vargas Cárdenas,
B.; Vásquez-Ramírez, A.; Veberič, D.; Ventura, C.; Vergara Quispe,
I. D.; Verzi, V.; Vicha, J.; Villaseñor, L.; Vink, J.; Vorobiov,
S.; Wahlberg, H.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.;
Wilczyński, H.; Winchen, T.; Wirtz, M.; Wittkowski, D.; Wundheiler,
B.; Yushkov, A.; Zapparrata, O.; Zas, E.; Zavrtanik, D.; Zavrtanik,
M.; Zehrer, L.; Zepeda, A.; Ziolkowski, M.; Zuccarello, F.
2020JInst..15P0021A Altcode: 2020arXiv200709035T
Cosmic rays arriving at Earth collide with the upper parts of the
atmosphere, thereby inducing extensive air showers. When secondary
particles from the cascade arrive at the ground, they are measured
by surface detector arrays. We describe the methods applied to the
measurements of the surface detector of the Pierre Auger Observatory to
reconstruct events with zenith angles less than 60<SUP>o</SUP> using
the timing and signal information recorded using the water-Cherenkov
detector stations. In addition, we assess the accuracy of these methods
in reconstructing the arrival directions of the primary cosmic ray
particles and the sizes of the induced showers.
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Title: Features of the Energy Spectrum of Cosmic Rays above 2.5
×10<SUP>18</SUP> eV Using the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albury, J. M.; Allekotte,
I.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves
Batista, R.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.; Andringa,
S.; Aramo, C.; Araújo Ferreira, P. R.; Asorey, H.; Assis, P.;
Avila, G.; Badescu, A. M.; Bakalova, A.; Balaceanu, A.; Barbato,
F.; Barreira Luz, R. J.; Becker, K. H.; Bellido, J. A.; Berat, C.;
Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Bister, T.; Biteau,
J.; Blanco, A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.;
Bonifazi, C.; Bonneau Arbeletche, L.; Borodai, N.; Botti, A. M.; Brack,
J.; Bretz, T.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink,
S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, L.; Calcagni,
L.; Cancio, A.; Canfora, F.; Caracas, I.; Carceller, J. M.; Caruso,
R.; Castellina, A.; Catalani, F.; Cataldi, G.; Cazon, L.; Cerda,
M.; Chinellato, J. A.; Choi, K.; Chudoba, J.; Chytka, L.; Clay,
R. W.; Cobos Cerutti, A. C.; Colalillo, R.; Coleman, A.; Coluccia,
M. R.; Conceição, R.; Condorelli, A.; Consolati, G.; Contreras,
F.; Convenga, F.; Covault, C. E.; Dasso, S.; Daumiller, K.; Dawson,
B. R.; Day, J. A.; de Almeida, R. M.; de Jesús, J.; de Jong, S. J.;
De Mauro, G.; de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira,
J.; de Oliveira Franco, D.; de Souza, V.; De Vito, E.; Debatin, J.;
del Río, M.; Deligny, O.; Dembinski, H.; Dhital, N.; Di Giulio, C.;
Di Matteo, A.; Díaz Castro, M. L.; Dobrigkeit, C.; D'Olivo, J. C.;
Dorosti, Q.; dos Anjos, R. C.; Dova, M. T.; Ebr, J.; Engel, R.;
Epicoco, I.; Erdmann, M.; Escobar, C. O.; Etchegoyen, A.; Falcke, H.;
Farmer, J.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Feldbusch, F.; Fenu,
F.; Fick, B.; Figueira, J. M.; Filipčič, A.; Fodran, T.; Freire,
M. M.; Fujii, T.; Fuster, A.; Galea, C.; Galelli, C.; García, B.;
Garcia Vegas, A. L.; Gemmeke, H.; Gesualdi, F.; Gherghel-Lascu, A.;
Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Glombitza, J.;
Gobbi, F.; Gollan, F.; Golup, G.; Gómez Berisso, M.; Gómez Vitale,
P. F.; Gongora, J. P.; González, N.; Goos, I.; Góra, D.; Gorgi, A.;
Gottowik, M.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Guido, E.;
Hahn, S.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari, D.; Harvey,
V. M.; Haungs, A.; Hebbeker, T.; Heck, D.; Hill, G. C.; Hojvat, C.;
Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman, J.;
Insolia, A.; Isar, P. G.; Johnsen, J. A.; Jurysek, J.; Kääpä, A.;
Kampert, K. H.; Keilhauer, B.; Kemp, J.; Klages, H. O.; Kleifges, M.;
Kleinfeller, J.; Köpke, M.; Kukec Mezek, G.; Lago, B. L.; LaHurd, D.;
Lang, R. G.; Leigui de Oliveira, M. A.; Lenok, V.; Letessier-Selvon,
A.; Lhenry-Yvon, I.; Lo Presti, D.; Lopes, L.; López, R.; Lorek, R.;
Luce, Q.; Lucero, A.; Machado Payeras, A.; Malacari, M.; Mancarella,
G.; Mandat, D.; Manning, B. C.; Manshanden, J.; Mantsch, P.; Marafico,
S.; Mariazzi, A. G.; Mariş, I. C.; Marsella, G.; Martello, D.;
Martinez, H.; Martínez Bravo, O.; Mastrodicasa, M.; Mathes, H. J.;
Matthews, J.; Matthiae, G.; Mayotte, E.; Mazur, P. O.; Medina-Tanco,
G.; Melo, D.; Menshikov, A.; Merenda, K. -D.; Michal, S.; Micheletti,
M. I.; Miramonti, L.; Mockler, D.; Mollerach, S.; Montanet, F.;
Morello, C.; Mostafá, M.; Müller, A. L.; Muller, M. A.; Mulrey,
K.; Mussa, R.; Muzio, M.; Namasaka, W. M.; Nellen, L.; Nguyen, P. H.;
Niculescu-Oglinzanu, M.; Niechciol, M.; Nitz, D.; Nosek, D.; Novotny,
V.; Nožka, L.; Nucita, A.; Núñez, L. A.; Palatka, M.; Pallotta,
J.; Panetta, M. P.; Papenbreer, P.; Parente, G.; Parra, A.; Pech, M.;
Pedreira, F.; PÈ©kala, J.; Pelayo, R.; Peña-Rodriguez, J.; Perez
Armand, J.; Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.; Pierog,
T.; Pimenta, M.; Pirronello, V.; Platino, M.; Pont, B.; Pothast, M.;
Privitera, P.; Prouza, M.; Puyleart, A.; Querchfeld, S.; Rautenberg,
J.; Ravignani, D.; Reininghaus, M.; Ridky, J.; Riehn, F.; Risse, M.;
Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Fernandez,
G.; Rodriguez Rojo, J.; Roncoroni, M. J.; Roth, M.; Roulet, E.; Rovero,
A. C.; Ruehl, P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar,
H.; Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Santos, E. M.;
Santos, E.; Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.;
Savina, P.; Schäfer, C.; Scherini, V.; Schieler, H.; Schimassek, M.;
Schimp, M.; Schlüter, F.; Schmidt, D.; Scholten, O.; Schovánek,
P.; Schröder, F. G.; Schröder, S.; Schulz, A.; Sciutto, S. J.;
Scornavacche, M.; Shellard, R. C.; Sigl, G.; Silli, G.; Sima, O.;
Šmída, R.; Sommers, P.; Soriano, J. F.; Souchard, J.; Squartini,
R.; Stadelmaier, M.; Stanca, D.; Stanič, S.; Stasielak, J.; Stassi,
P.; Streich, A.; Suárez-Durán, M.; Sudholz, T.; Suomijärvi, T.;
Supanitsky, A. D.; Šupík, J.; Szadkowski, Z.; Taboada, A.; Tapia,
A.; Timmermans, C.; Tkachenko, O.; Tobiska, P.; Todero Peixoto, C. J.;
Tomé, B.; Torralba Elipe, G.; Travaini, A.; Travnicek, P.; Trimarelli,
C.; Trini, M.; Tueros, M.; Ulrich, R.; Unger, M.; Urban, M.; Vaclavek,
L.; Vacula, M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.;
van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Vásquez-Ramírez,
A.; Veberič, D.; Ventura, C.; Vergara Quispe, I. D.; Verzi, V.;
Vicha, J.; Villaseñor, L.; Vink, J.; Vorobiov, S.; Wahlberg, H.;
Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński, H.;
Winchen, T.; Wirtz, M.; Wittkowski, D.; Wundheiler, B.; Yushkov, A.;
Zapparrata, O.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zehrer, L.;
Zepeda, A.; Ziolkowski, M.; Zuccarello, F.; Pierre Auger Collaboration
2020PhRvL.125l1106A Altcode: 2020arXiv200806488T
We report a measurement of the energy spectrum of cosmic rays above
2.5 ×10<SUP>18</SUP> eV based on 215 030 events. New results are
presented: at about 1.3 ×10<SUP>19</SUP> eV , the spectral index
changes from 2.51 ±0.03 (stat ) ±0.05 (syst ) to 3.05 ±0.05
(stat ) ±0.10 (syst ) , evolving to 5.1 ±0.3 (stat ) ±0.1 (syst
) beyond 5 ×10<SUP>19</SUP> eV , while no significant dependence
of spectral features on the declination is seen in the accessible
range. These features of the spectrum can be reproduced in models with
energy-dependent mass composition. The energy density in cosmic rays
above 5 ×10<SUP>18</SUP> eV is [5.66 ±0.03 (stat ) ±1.40 (syst )
]×10<SUP>53</SUP> erg Mpc<SUP>-3</SUP> .
---------------------------------------------------------
Title: Measurement of the cosmic-ray energy spectrum above 2.5
×10<SUP>18</SUP> eV using the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albury, J. M.; Allekotte,
I.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves
Batista, R.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.; Andringa,
S.; Aramo, C.; Araújo Ferreira, P. R.; Asorey, H.; Assis, P.;
Avila, G.; Badescu, A. M.; Bakalova, A.; Balaceanu, A.; Barbato,
F.; Barreira Luz, R. J.; Becker, K. H.; Bellido, J. A.; Berat, C.;
Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Bister, T.; Biteau,
J.; Blanco, A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.;
Bonifazi, C.; Bonneau Arbeletche, L.; Borodai, N.; Botti, A. M.; Brack,
J.; Bretz, T.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink,
S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, L.; Calcagni,
L.; Cancio, A.; Canfora, F.; Caracas, I.; Carceller, J. M.; Caruso,
R.; Castellina, A.; Catalani, F.; Cataldi, G.; Cazon, L.; Cerda,
M.; Chinellato, J. A.; Choi, K.; Chudoba, J.; Chytka, L.; Clay,
R. W.; Cobos Cerutti, A. C.; Colalillo, R.; Coleman, A.; Coluccia,
M. R.; Conceição, R.; Condorelli, A.; Consolati, G.; Contreras,
F.; Convenga, F.; Covault, C. E.; Dasso, S.; Daumiller, K.; Dawson,
B. R.; Day, J. A.; de Almeida, R. M.; de Jesús, J.; de Jong, S. J.;
De Mauro, G.; de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira,
J.; de Oliveira Franco, D.; de Souza, V.; De Vito, E.; Debatin, J.;
del Río, M.; Deligny, O.; Dembinski, H.; Dhital, N.; Di Giulio, C.;
Di Matteo, A.; Díaz Castro, M. L.; Dobrigkeit, C.; D'Olivo, J. C.;
Dorosti, Q.; dos Anjos, R. C.; Dova, M. T.; Ebr, J.; Engel, R.;
Epicoco, I.; Erdmann, M.; Escobar, C. O.; Etchegoyen, A.; Falcke, H.;
Farmer, J.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Feldbusch, F.; Fenu,
F.; Fick, B.; Figueira, J. M.; Filipčič, A.; Fodran, T.; Freire,
M. M.; Fujii, T.; Fuster, A.; Galea, C.; Galelli, C.; García, B.;
Garcia Vegas, A. L.; Gemmeke, H.; Gesualdi, F.; Gherghel-Lascu, A.;
Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Glombitza, J.;
Gobbi, F.; Gollan, F.; Golup, G.; Gómez Berisso, M.; Gómez Vitale,
P. F.; Gongora, J. P.; González, N.; Goos, I.; Góra, D.; Gorgi, A.;
Gottowik, M.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Guido, E.;
Hahn, S.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari, D.; Harvey,
V. M.; Haungs, A.; Hebbeker, T.; Heck, D.; Hill, G. C.; Hojvat, C.;
Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman, J.;
Insolia, A.; Isar, P. G.; Johnsen, J. A.; Jurysek, J.; Kääpä, A.;
Kampert, K. H.; Keilhauer, B.; Kemp, J.; Klages, H. O.; Kleifges, M.;
Kleinfeller, J.; Köpke, M.; Kukec Mezek, G.; Lago, B. L.; LaHurd, D.;
Lang, R. G.; Leigui de Oliveira, M. A.; Lenok, V.; Letessier-Selvon,
A.; Lhenry-Yvon, I.; Lo Presti, D.; Lopes, L.; López, R.; Lorek, R.;
Luce, Q.; Lucero, A.; Machado Payeras, A.; Malacari, M.; Mancarella,
G.; Mandat, D.; Manning, B. C.; Manshanden, J.; Mantsch, P.; Marafico,
S.; Mariazzi, A. G.; Mariş, I. C.; Marsella, G.; Martello, D.;
Martinez, H.; Martínez Bravo, O.; Mastrodicasa, M.; Mathes, H. J.;
Matthews, J.; Matthiae, G.; Mayotte, E.; Mazur, P. O.; Medina-Tanco,
G.; Melo, D.; Menshikov, A.; Merenda, K. -D.; Michal, S.; Micheletti,
M. I.; Miramonti, L.; Mockler, D.; Mollerach, S.; Montanet, F.;
Morello, C.; Mostafá, M.; Müller, A. L.; Muller, M. A.; Mulrey,
K.; Mussa, R.; Muzio, M.; Namasaka, W. M.; Nellen, L.; Nguyen, P. H.;
Niculescu-Oglinzanu, M.; Niechciol, M.; Nitz, D.; Nosek, D.; Novotny,
V.; Nožka, L.; Nucita, A.; Núñez, L. A.; Palatka, M.; Pallotta,
J.; Panetta, M. P.; Papenbreer, P.; Parente, G.; Parra, A.; Pech, M.;
Pedreira, F.; PÈ©kala, J.; Pelayo, R.; Peña-Rodriguez, J.; Perez
Armand, J.; Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.; Pierog,
T.; Pimenta, M.; Pirronello, V.; Platino, M.; Pont, B.; Pothast, M.;
Privitera, P.; Prouza, M.; Puyleart, A.; Querchfeld, S.; Rautenberg,
J.; Ravignani, D.; Reininghaus, M.; Ridky, J.; Riehn, F.; Risse, M.;
Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Fernandez,
G.; Rodriguez Rojo, J.; Roncoroni, M. J.; Roth, M.; Roulet, E.; Rovero,
A. C.; Ruehl, P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar,
H.; Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Santos, E. M.;
Santos, E.; Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.;
Savina, P.; Schäfer, C.; Scherini, V.; Schieler, H.; Schimassek, M.;
Schimp, M.; Schlüter, F.; Schmidt, D.; Scholten, O.; Schovánek,
P.; Schröder, F. G.; Schröder, S.; Schulz, A.; Sciutto, S. J.;
Scornavacche, M.; Shellard, R. C.; Sigl, G.; Silli, G.; Sima, O.;
Šmída, R.; Sommers, P.; Soriano, J. F.; Souchard, J.; Squartini,
R.; Stadelmaier, M.; Stanca, D.; Stanič, S.; Stasielak, J.; Stassi,
P.; Streich, A.; Suárez-Durán, M.; Sudholz, T.; Suomijärvi, T.;
Supanitsky, A. D.; Šupík, J.; Szadkowski, Z.; Taboada, A.; Tapia,
A.; Timmermans, C.; Tkachenko, O.; Tobiska, P.; Todero Peixoto, C. J.;
Tomé, B.; Torralba Elipe, G.; Travaini, A.; Travnicek, P.; Trimarelli,
C.; Trini, M.; Tueros, M.; Ulrich, R.; Unger, M.; Urban, M.; Vaclavek,
L.; Vacula, M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.;
van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Vásquez-Ramírez,
A.; Veberič, D.; Ventura, C.; Vergara Quispe, I. D.; Verzi, V.;
Vicha, J.; Villaseñor, L.; Vink, J.; Vorobiov, S.; Wahlberg, H.;
Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński, H.;
Winchen, T.; Wirtz, M.; Wittkowski, D.; Wundheiler, B.; Yushkov, A.;
Zapparrata, O.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zehrer, L.;
Zepeda, A.; Ziolkowski, M.; Zuccarello, F.; Pierre Auger Collaboration
2020PhRvD.102f2005A Altcode: 2020arXiv200806486T
We report a measurement of the energy spectrum of cosmic rays for
energies above 2.5 ×10<SUP>18</SUP> eV based on 215,030 events
recorded with zenith angles below 60°. A key feature of the work is
that the estimates of the energies are independent of assumptions about
the unknown hadronic physics or of the primary mass composition. The
measurement is the most precise made hitherto with the accumulated
exposure being so large that the measurements of the flux are dominated
by systematic uncertainties except at energies above 5 ×10<SUP>19</SUP>
eV . The principal conclusions are(1) The flattening of the spectrum
near 5 ×10<SUP>18</SUP> eV , the so-called "ankle," is confirmed. <P
/>(2) The steepening of the spectrum at around 5 ×10<SUP>19</SUP> eV is
confirmed. <P />(3) A new feature has been identified in the spectrum:
in the region above the ankle the spectral index γ of the particle flux
(∝E<SUP>-γ</SUP>) changes from 2.51 ±0.03 (stat ) ±0.05 (syst )
to 3.05 ±0.05 (stat ) ±0.10 (syst ) before changing sharply to 5.1
±0.3 (stat ) ±0.1 (syst ) above 5 ×10<SUP>19</SUP> eV . <P />(4)
No evidence for any dependence of the spectrum on declination has been
found other than a mild excess from the Southern Hemisphere that is
consistent with the anisotropy observed above 8 ×10<SUP>18</SUP> eV .
---------------------------------------------------------
Title: Erratum: Search for photons with energies above 10<SUP>18</SUP>
eV using the hybrid detector of the Pierre Auger Observatory Erratum:
Search for photons with energies above <SUP>18</SUP> eV using the
hybrid detector of the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Al Samarai, I.;
Albuquerque, I. F. M.; Allekotte, I.; Almela, A.; Alvarez Castillo,
J.; Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.;
Andringa, S.; Aramo, C.; Arqueros, F.; Arsene, N.; Asorey, H.; Assis,
P.; Aublin, J.; Avila, G.; Badescu, A. M.; Balaceanu, A.; Barreira
Luz, R. J.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.; Berat, C.;
Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Billoir, P.; Biteau,
J.; Blaess, S. G.; Blanco, A.; Blazek, J.; Bleve, C.; Boháčová,
M.; Boncioli, D.; Bonifazi, C.; Borodai, N.; Botti, A. M.; Brack, J.;
Brancus, I.; Bretz, T.; Bridgeman, A.; Briechle, F. L.; Buchholz, P.;
Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga,
L.; Cancio, A.; Canfora, F.; Caramete, L.; Caruso, R.; Castellina, A.;
Cataldi, G.; Cazon, L.; Chavez, A. G.; Chinellato, J. A.; Chudoba, J.;
Clay, R. W.; Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.;
Conceičão, R.; Contreras, F.; Cooper, M. J.; Coutu, S.; Covault,
C. E.; Cronin, J.; D'Amico, S.; Daniel, B.; Dasso, S.; Daumiller,
K.; Dawson, B. R.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza,
V.; Debatin, J.; Deligny, O.; Di Giulio, C.; Di Matteo, A.; Dimathaz
Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.; Dorosti,
Q.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.;
Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.;
Falcke, H.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Fick, B.; Figueira,
J. M.; Filipčič, A.; Fratu, O.; Freire, M. M.; Fujii, T.; Fuster,
A.; Gaior, R.; Garcimatha, B.; Garcia-Pinto, D.; Gaté, F.; Gemmeke,
H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.;
Giller, M.; Głas, D.; Glaser, C.; Golup, G.; Gómez Berisso, M.;
Gómez Vitale, P. F.; González, N.; Gorgi, A.; Gorham, P.; Grillo,
A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel, M. R.; Hansen,
P.; Harari, D.; Harrison, T. A.; Harton, J. L.; Haungs, A.; Hebbeker,
T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.;
Holt, E.; Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský,
M.; Huege, T.; Hulsman, J.; Insolia, A.; Isar, P. G.; Jandt, I.;
Jansen, S.; Johnsen, J. A.; Josebachuili, M.; Kääpä, A.; Kambeitz,
O.; Kampert, K. H.; Katkov, I.; Keilhauer, B.; Kemp, E.; Kemp, J.;
Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.;
Krause, R.; Krohm, N.; Kuempel, D.; Kukec Mezek, G.; Kunka, N.; Kuotb
Awad, A.; LaHurd, D.; Lauscher, M.; Legumina, R.; Leigui de Oliveira,
M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; Lopes, L.;
López, R.; López Casado, A.; Luce, Q.; Lucero, A.; Malacari, M.;
Mallamaci, M.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Mariş,
I. C.; Marsella, G.; Martello, D.; Martinez, H.; Martimathnez Bravo,
O.; Masimathas Meza, J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.;
Matthews, J. A. J.; Matthiae, G.; Mayotte, E.; Mazur, P. O.; Medina,
C.; Medina-Tanco, G.; Melo, D.; Menshikov, A.; Micheletti, M. I.;
Middendorf, L.; Minaya, I. A.; Miramonti, L.; Mitrica, B.; Mockler,
D.; Mollerach, S.; Montanet, F.; Morello, C.; Mostafá, M.; Müller,
A. L.; Müller, G.; Muller, M. A.; Müller, S.; Mussa, R.; Naranjo,
I.; Nellen, L.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.;
Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka,
H.; Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Palatka,
M.; Pallotta, J.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.;
Pech, M.; Pedreira, F.; Pȩkala, J.; Pelayo, R.; Peña-Rodriguez, J.;
Pereira, L. A. S.; Perlimathn, M.; Perrone, L.; Peters, C.; Petrera,
S.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.;
Pirronello, V.; Platino, M.; Plum, M.; Porowski, C.; Prado, R. R.;
Privitera, P.; Prouza, M.; Quel, E. J.; Querchfeld, S.; Quinn, S.;
Ramos-Pollan, R.; Rautenberg, J.; Ravignani, D.; Revenu, B.; Ridky,
J.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.;
Rodriguez Fernandez, G.; Rodriguez Rojo, J.; Rogozin, D.; Roncoroni,
M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl, P.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santos, E. M.; Santos,
E.; Sarazin, F.; Sarmento, R.; Sarmiento, C. A.; Sato, R.; Schauer,
M.; Scherini, V.; Schieler, H.; Schimp, M.; Schmidt, D.; Scholten, O.;
Schovánek, P.; Schröder, F. G.; Schulz, A.; Schulz, J.; Schumacher,
J.; Sciutto, S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard,
R. C.; Sigl, G.; Silli, G.; Sima, O.; Śmiałkowski, A.; Vmimathda,
R.; Snow, G. R.; Sommers, P.; Sonntag, S.; Sorokin, J.; Squartini,
R.; Stanca, D.; Stanič, S.; Stasielak, J.; Stassi, P.; Strafella,
F.; Suarez, F.; Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.;
Supanitsky, A. D.; Swain, J.; Szadkowski, Z.; Taboada, A.; Taborda,
O. A.; Tapia, A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Tomankova, L.; Tomé, B.; Torralba Elipe, G.; Travnicek, P.;
Trini, M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.;
Valiño, I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg,
A. M.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner,
G.; Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Vergara Quispe,
I. D.; Verzi, V.; Vicha, J.; Villaseñor, L.; Vorobiov, S.; Wahlberg,
H.; Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weindl, A.;
Wiencke, L.; Wilczyński, H.; Winchen, T.; Wirtz, M.; Wittkowski, D.;
Wundheiler, B.; Yang, L.; Yelos, D.; Yushkov, A.; Zas, E.; Zavrtanik,
D.; Zavrtanik, M.; Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong,
Z.; Zuccarello, F.
2020JCAP...09E.002A Altcode:
Please see the PDF file for details.
---------------------------------------------------------
Title: Restoring Process of Sunspot Penumbra
Authors: Romano, P.; Murabito, M.; Guglielmino, S. L.; Zuccarello,
F.; Falco, M.
2020ApJ...899..129R Altcode: 2020arXiv200609746R
We describe the disappearance of a sector of sunspot penumbra and its
restoring process observed in the preceding sunspot of active region
NOAA 12348. The evolution of the magnetic field and the plasma flows
supports the idea that the penumbra forms due to a change of inclination
of the magnetic field of the canopy. Moving magnetic features have
been observed during the disintegration phase of that sector of sunspot
penumbra. During the restoring phase we have not observed any magnetic
flux emergence around the sunspot. The restoring process of the penumbra
sector completed in about 72 hr and it was accompanied by the transition
from the counter-Evershed flow to the classical Evershed flow. The
inversion of photospheric spectropolarimetric measurements taken by the
Interferometric Bidimensional Spectroscopic Instrument (IBIS) allowed
us to reconstruct how the uncombed configuration of the magnetic field
forms during the new settlement of the penumbra, i.e., the vertical
component of the magnetic field seems to be progressively replaced by
some horizontal field lines, corresponding to the intraspines.
---------------------------------------------------------
Title: Differences in Periodic Magnetic Helicity Injection Behavior
between Flaring and Non-flaring Active Regions: Case Study
Authors: Korsós, M. B.; Romano, P.; Morgan, H.; Ye, Y.; Erdélyi,
R.; Zuccarello, F.
2020ApJ...897L..23K Altcode: 2020arXiv200607659K
The evolution of magnetic helicity has a close relationship with solar
eruptions and is of interest as a predictive diagnostic. In this case
study, we analyze the evolution of the normalized emergence, shearing,
and total magnetic helicity components in the case of three flaring and
three non-flaring active regions (ARs) using Spaceweather Helioseismic
Magnetic Imager Active Region Patches vector magnetic field data. The
evolution of the three magnetic helicity components is analyzed with
wavelet transforms, revealing significant common periodicities of
the normalized emergence, shearing, and total helicity fluxes before
flares in the flaring ARs. The three non-flaring ARs do not show such
common periodic behavior. This case study suggests that the presence
of significant periodicities in the power spectrum of magnetic helicity
components could serve as a valuable precursor for flares.
---------------------------------------------------------
Title: Studies on the response of a water-Cherenkov detector of the
Pierre Auger Observatory to atmospheric muons using an RPC hodoscope
Authors: The Pierre Auger Collaboration; Aab, A.; Abreu, P.; Aglietta,
M.; Albury, J. M.; Allekotte, I.; Almela, A.; Alvarez Castillo, J.;
Alvarez-Muñiz, J.; Alves Batista, R.; Anastasi, G. A.; Anchordoqui,
L.; Andrada, B.; Andringa, S.; Aramo, C.; Araújo Ferreira, P. R.;
Asorey, H.; Assis, P.; Avila, G.; Badescu, A. M.; Bakalova, A.;
Balaceanu, A.; Barbato, F.; Barreira Luz, R. J.; Becker, K. H.;
Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann,
P. L.; Bister, T.; Biteau, J.; Blanco, A.; Blazek, J.; Bleve, C.;
Boháčová, M.; Boncioli, D.; Bonifazi, C.; Bonneau Arbeletche, L.;
Borodai, N.; Botti, A. M.; Brack, J.; Bretz, T.; Briechle, F. L.;
Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora,
K. S.; Caccianiga, L.; Calcagni, L.; Cancio, A.; Canfora, F.;
Caracas, I.; Carceller, J. M.; Caruso, R.; Castellina, A.; Catalani,
F.; Cataldi, G.; Cazon, L.; Cerda, M.; Chinellato, J. A.; Choi, K.;
Chudoba, J.; Chytka, L.; Clay, R. W.; Cobos Cerutti, A. C.; Colalillo,
R.; Coleman, A.; Coluccia, M. R.; Conceição, R.; Condorelli, A.;
Consolati, G.; Contreras, F.; Convenga, F.; Covault, C. E.; Dasso, S.;
Daumiller, K.; Dawson, B. R.; Day, J. A.; de Almeida, R. M.; de Jesús,
J.; de Jong, S. J.; De Mauro, G.; de Mello Neto, J. R. T.; De Mitri,
I.; de Oliveira, J.; de Oliveira Franco, D.; de Souza, V.; De Vito,
E.; Debatin, J.; del Río, M.; Deligny, O.; Dhital, N.; Di Matteo,
A.; Díaz Castro, M. L.; Dobrigkeit, C.; D'Olivo, J. C.; Dorosti,
Q.; dos Anjos, R. C.; Dova, M. T.; Ebr, J.; Engel, R.; Epicoco, I.;
Erdmann, M.; Escobar, C. O.; Etchegoyen, A.; Falcke, H.; Farmer,
J.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Feldbusch, F.; Fenu,
F.; Fick, B.; Figueira, J. M.; Filipčič, A.; Fodran, T.; Freire,
M. M.; Fujii, T.; Fuster, A.; Galea, C.; Galelli, C.; García, B.;
Garcia Vegas, A. L.; Gemmeke, H.; Gesualdi, F.; Gherghel-Lascu, A.;
Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Glombitza, J.;
Gobbi, F.; Gollan, F.; Golup, G.; Gómez Berisso, M.; Gómez Vitale,
P. F.; Gongora, J. P.; González, N.; Goos, I.; Góra, D.; Gorgi,
A.; Gottowik, M.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Guido,
E.; Hahn, S.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari, D.;
Harvey, V. M.; Haungs, A.; Hebbeker, T.; Heck, D.; Hill, G. C.;
Hojvat, C.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege,
T.; Hulsman, J.; Insolia, A.; Isar, P. G.; Johnsen, J. A.; Jurysek,
J.; Kääpä, A.; Kampert, K. H.; Keilhauer, B.; Kemp, J.; Klages,
H. O.; Kleifges, M.; Kleinfeller, J.; Köpke, M.; Kukec Mezek, G.;
Lago, B. L.; LaHurd, D.; Lang, R. G.; Leigui de Oliveira, M. A.;
Lenok, V.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Lo Presti, D.;
Lopes, L.; López, R.; Lorek, R.; Luce, Q.; Lucero, A.; Machado
Payeras, A.; Malacari, M.; Mancarella, G.; Mandat, D.; Manning, B. C.;
Manshanden, J.; Mantsch, P.; Marafico, S.; Mariazzi, A. G.; Mariş,
I. C.; Marsella, G.; Martello, D.; Martinez, H.; Martínez Bravo, O.;
Mastrodicasa, M.; Mathes, H. J.; Matthews, J.; Matthiae, G.; Mayotte,
E.; Mazur, P. O.; Medina-Tanco, G.; Melo, D.; Menshikov, A.; Merenda,
K. -D.; Michal, S.; Micheletti, M. I.; Miramonti, L.; Mockler, D.;
Mollerach, S.; Montanet, F.; Morello, C.; Mostafá, M.; Müller,
A. L.; Muller, M. A.; Mulrey, K.; Mussa, R.; Muzio, M.; Namasaka,
W. M.; Nellen, L.; Niculescu-Oglinzanu, M.; Niechciol, M.; Nitz, D.;
Nosek, D.; Novotny, V.; Nožka, L.; Nucita, A; Núñez, L. A.; Palatka,
M.; Pallotta, J.; Panetta, M. P.; Papenbreer, P.; Parente, G.; Parra,
A.; Pech, M.; Pedreira, F.; Pękala, J.; Pelayo, R.; Peña-Rodriguez,
J.; Perez Armand, J.; Perlin, M.; Perrone, L.; Peters, C.; Petrera,
S.; Pierog, T.; Pimenta, M.; Pirronello, V.; Platino, M.; Pont, B.;
Pothast, M.; Privitera, P.; Prouza, M.; Puyleart, A.; Querchfeld, S.;
Rautenberg, J.; Ravignani, D.; Reininghaus, M.; Ridky, J.; Riehn,
F.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.;
Rodriguez Rojo, J.; Roncoroni, M. J.; Roth, M.; Roulet, E.; Rovero,
A. C.; Ruehl, P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar,
H.; Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Santos, E. M.;
Santos, E.; Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.;
Savina, P.; Schäfer, C.; Scherini, V.; Schieler, H.; Schimassek, M.;
Schimp, M.; Schlüter, F.; Schmidt, D.; Scholten, O.; Schovánek,
P.; Schröder, F. G.; Schröder, S.; Sciutto, S. J.; Scornavacche,
M.; Shellard, R. C.; Sigl, G.; Silli, G.; Sima, O.; Šmída, R.;
Sommers, P.; Soriano, J. F.; Souchard, J.; Squartini, R.; Stadelmaier,
M.; Stanca, D.; Stanič, S.; Stasielak, J.; Stassi, P.; Streich, A.;
Suárez-Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky, A. D.;
Šupík, J.; Szadkowski, Z.; Taboada, A.; Tapia, A.; Timmermans,
C.; Tkachenko, O.; Tobiska, P.; Todero Peixoto, C. J.; Tomé, B.;
Torralba Elipe, G.; Travaini, A.; Travnicek, P.; Trimarelli, C.;
Trini, M.; Tueros, M.; Ulrich, R.; Unger, M.; Urban, M.; Vaclavek,
L.; Vacula, M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.;
van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Vásquez-Ramírez,
A.; Veberič, D.; Ventura, C.; Vergara Quispe, I. D.; Verzi, V.;
Vicha, J.; Villaseñor, L.; Vink, J.; Vorobiov, S.; Wahlberg, H.;
Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński, H.;
Winchen, T.; Wirtz, M.; Wittkowski, D.; Wundheiler, B.; Yushkov, A.;
Zapparrata, O.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zehrer, L.;
Zepeda, A.; Ziolkowski, M.; Zuccarello, F.
2020arXiv200704139T Altcode:
Extensive air showers, originating from ultra-high energy cosmic
rays, have been successfully measured through the use of arrays of
water-Cherenkov detectors (WCDs). Sophisticated analyses exploiting
WCD data have made it possible to demonstrate that shower simulations,
based on different hadronic-interaction models, cannot reproduce the
observed number of muons at the ground. The accurate knowledge of the
WCD response to muons is paramount in establishing the exact level of
this discrepancy. In this work, we report on a study of the response of
a WCD of the Pierre Auger Observatory to atmospheric muons performed
with a hodoscope made of resistive plate chambers (RPCs), enabling us
to select and reconstruct nearly 600 thousand single muon trajectories
with zenith angles ranging from 0$^\circ$ to 55$^\circ$. Comparison
of distributions of key observables between the hodoscope data and
the predictions of dedicated simulations allows us to demonstrate the
accuracy of the latter at a level of 2%. As the WCD calibration is
based on its response to atmospheric muons, the hodoscope data are
also exploited to show the long-term stability of the procedure.
---------------------------------------------------------
Title: On the Magnetic Nature of an Exploding Granule as Revealed
by Sunrise/IMaX
Authors: Guglielmino, Salvo L.; Martínez Pillet, Valentín; Ruiz
Cobo, Basilio; Bellot Rubio, Luis R.; del Toro Iniesta, José Carlos;
Solanki, Sami K.; Riethmüller, Tino L.; Zuccarello, Francesca
2020ApJ...896...62G Altcode: 2020arXiv200503371G
We study the photospheric evolution of an exploding granule
observed in the quiet Sun at high spatial (∼0"3) and temporal
(31.5 s) resolution by the imaging magnetograph Sunrise/IMaX in 2009
June. These observations show that the exploding granule is cospatial
to a magnetic flux emergence event occurring at mesogranular scale
(up to ∼12 Mm<SUP>2</SUP> area). Using a modified version of the
SIR code for inverting the IMaX spectropolarimetric measurements, we
obtain information about the magnetic configuration of this photospheric
feature. In particular, we find evidence of highly inclined emerging
fields in the structure, carrying a magnetic flux content up to ∼4
× 10<SUP>18</SUP> Mx. The balance between gas and magnetic pressure
in the region of flux emergence, compared with a very quiet region of
the Sun, indicates that the additional pressure carried by the emerging
flux increases the total pressure by about 5% and appears to allow the
granulation to be modified, as predicted by numerical simulations. The
overall characteristics suggest that a multipolar structure emerges
into the photosphere, resembling an almost horizontal flux sheet. This
seems to be associated with exploding granules. Finally, we discuss
the origin of such flux emergence events.
---------------------------------------------------------
Title: Search for magnetically-induced signatures in the arrival
directions of ultra-high-energy cosmic rays measured at the Pierre
Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albury, J. M.; Allekotte,
I.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves
Batista, R.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.; Andringa,
S.; Aramo, C.; Araújo Ferreira, P. R.; Asorey, H.; Assis, P.; Avila,
G.; Badescu, A. M.; Bakalova, A.; Balaceanu, A.; Barbato, F.; Barreira
Luz, R. J.; Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.;
Bertou, X.; Biermann, P. L.; Bister, T.; Biteau, J.; Blanco, A.;
Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi, C.;
Bonneau Arbeletche, L.; Borodai, N.; Botti, A. M.; Brack, J.; Bretz,
T.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi,
M.; Caballero-Mora, K. S.; Caccianiga, L.; Calcagni, L.; Cancio, A.;
Canfora, F.; Caracas, I.; Carceller, J. M.; Caruso, R.; Castellina,
A.; Catalani, F.; Cataldi, G.; Cazon, L.; Cerda, M.; Chinellato,
J. A.; Choi, K.; Chudoba, J.; Chytka, L.; Clay, R. W.; Cobos Cerutti,
A. C.; Colalillo, R.; Coleman, A.; Coluccia, M. R.; Conceição, R.;
Condorelli, A.; Consolati, G.; Contreras, F.; Convenga, F.; Covault,
C. E.; Dasso, S.; Daumiller, K.; Dawson, B. R.; Day, J. A.; de Almeida,
R. M.; de Jesús, J.; de Jong, S. J.; De Mauro, G.; de Mello Neto,
J. R. T.; De Mitri, I.; de Oliveira, J.; de Oliveira Franco, D.;
de Souza, V.; Debatin, J.; del Río, M.; Deligny, O.; Dhital, N.;
Di Matteo, A.; Díaz Castro, M. L.; Dobrigkeit, C.; D'Olivo, J. C.;
Dorosti, Q.; dos Anjos, R. C.; Dova, M. T.; Ebr, J.; Engel, R.;
Epicoco, I.; Erdmann, M.; Escobar, C. O.; Etchegoyen, A.; Falcke,
H.; Farmer, J.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Feldbusch,
F.; Fenu, F.; Fick, B.; Figueira, J. M.; Filipčič, A.; Fodran, T.;
Freire, M. M.; Fujii, T.; Fuster, A.; Galea, C.; Galelli, C.; García,
B.; Garcia Vegas, A. L.; Gemmeke, H.; Gesualdi, F.; Gherghel-Lascu,
A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Glombitza,
J.; Gobbi, F.; Golup, G.; Gómez Berisso, M.; Gómez Vitale, P. F.;
Gongora, J. P.; González, N.; Goos, I.; Góra, D.; Gorgi, A.;
Gottowik, M.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Guido, E.;
Hahn, S.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari, D.; Harvey,
V. M.; Haungs, A.; Hebbeker, T.; Heck, D.; Hill, G. C.; Hojvat, C.;
Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman, J.;
Insolia, A.; Isar, P. G.; Johnsen, J. A.; Jurysek, J.; Kääpä, A.;
Kampert, K. H.; Keilhauer, B.; Kemp, J.; Klages, H. O.; Kleifges, M.;
Kleinfeller, J.; Köpke, M.; Kukec Mezek, G.; Lago, B. L.; LaHurd, D.;
Lang, R. G.; Leigui de Oliveira, M. A.; Lenok, V.; Letessier-Selvon,
A.; Lhenry-Yvon, I.; Lo Presti, D.; Lopes, L.; López, R.; Lorek,
R.; Luce, Q.; Lucero, A.; Machado Payeras, A.; Malacari, M.;
Mancarella, G.; Mandat, D.; Manning, B. C.; Manshanden, J.; Mantsch,
P.; Marafico, S.; Mariazzi, A. G.; Mari\c{s}, I. C.; Marsella, G.;
Martello, D.; Martinez, H.; Martínez Bravo, O.; Mastrodicasa, M.;
Mathes, H. J.; Matthews, J.; Matthiae, G.; Mayotte, E.; Mazur, P. O.;
Medina-Tanco, G.; Melo, D.; Menshikov, A.; Merenda, K. -D.; Michal,
S.; Micheletti, M. I.; Miramonti, L.; Mockler, D.; Mollerach, S.;
Montanet, F.; Morello, C.; Mostafá, M.; Müller, A. L.; Muller,
M. A.; Mulrey, K.; Mussa, R.; Muzio, M.; Namasaka, W. M.; Nellen,
L.; Niculescu-Oglinzanu, M.; Niechciol, M.; Nitz, D.; Nosek, D.;
Novotny, V.; Nožka, L.; Nucita, A.; Núñez, L. A.; Palatka, M.;
Pallotta, J.; Panetta, M. P.; Papenbreer, P.; Parente, G.; Parra, A.;
Pech, M.; Pedreira, F.; P\c{e}kala, J.; Pelayo, R.; Peña-Rodriguez,
J.; Perez Armand, J.; Perlin, M.; Perrone, L.; Peters, C.; Petrera,
S.; Pierog, T.; Pimenta, M.; Pirronello, V.; Platino, M.; Pont, B.;
Pothast, M.; Privitera, P.; Prouza, M.; Puyleart, A.; Querchfeld, S.;
Rautenberg, J.; Ravignani, D.; Reininghaus, M.; Ridky, J.; Riehn,
F.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.;
Rodriguez Rojo, J.; Roncoroni, M. J.; Roth, M.; Roulet, E.; Rovero,
A. C.; Ruehl, P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar,
H.; Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Santos, E. M.;
Santos, E.; Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.;
Savina, P.; Schäfer, C.; Scherini, V.; Schieler, H.; Schimassek, M.;
Schimp, M.; Schlüter, F.; Schmidt, D.; Scholten, O.; Schovánek,
P.; Schröder, F. G.; Schröder, S.; Sciutto, S. J.; Scornavacche,
M.; Shellard, R. C.; Sigl, G.; Silli, G.; Sima, O.; \v{S}mída, R.;
Sommers, P.; Soriano, J. F.; Souchard, J.; Squartini, R.; Stadelmaier,
M.; Stanca, D.; Stanič, S.; Stasielak, J.; Stassi, P.; Streich, A.;
Suárez-Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky, A. D.;
\v{S}upík, J.; Szadkowski, Z.; Taboada, A.; Tapia, A.; Timmermans,
C.; Tobiska, P.; Todero Peixoto, C. J.; Tomé, B.; Torralba Elipe, G.;
Travaini, A.; Travnicek, P.; Trimarelli, C.; Trini, M.; Tueros, M.;
Ulrich, R.; Unger, M.; Urban, M.; Vaclavek, L.; Vacula, M.; Valdés
Galicia, J. F.; Valiño, I.; Valore, L.; van Vliet, A.; Varela, E.;
Vargas Cárdenas, B.; Vásquez-Ramírez, A.; Veberič, D.; Ventura,
C.; Vergara Quispe, I. D.; Verzi, V.; Vicha, J.; Villaseñor, L.; Vink,
J.; Vorobiov, S.; Wahlberg, H.; Watson, A. A.; Weber, M.; Weindl, A.;
Wiencke, L.; Wilczyński, H.; Winchen, T.; Wirtz, M.; Wittkowski, D.;
Wundheiler, B.; Yushkov, A.; Zapparrata, O.; Zas, E.; Zavrtanik, D.;
Zavrtanik, M.; Zehrer, L.; Zepeda, A.; Ziolkowski, M.; Zuccarello, F.
2020JCAP...06..017A Altcode: 2020arXiv200410591T
We search for signals of magnetically-induced effects in the arrival
directions of ultra-high-energy cosmic rays detected at the Pierre
Auger Observatory. We apply two different methods. One is a search for
sets of events that show a correlation between their arrival direction
and the inverse of their energy, which would be expected if they come
from the same point-like source, they have the same electric charge and
their deflection is relatively small and coherent. We refer to these
sets of events as "multiplets". The second method, called "thrust",
is a principal axis analysis aimed to detect the elongated patterns in
a region of interest. We study the sensitivity of both methods using
a benchmark simulation and we apply them to data in two different
searches. The first search is done assuming as source candidates a
list of nearby active galactic nuclei and starburst galaxies. The
second is an all-sky blind search. We report the results and we find
no statistically significant features. We discuss the compatibility
of these results with the indications on the mass composition inferred
from data of the Pierre Auger Observatory.
---------------------------------------------------------
Title: The penumbral solar filaments from the photosphere to the
chromosphere
Authors: Murabito, M.; Ermolli, I.; Giorgi, F.; Stangalini, M.;
Guglielmino, S. L.; Jafarzadeh, S.; Socas-Navarro, H.; Romano, P.;
Zuccarello, F.
2020JPhCS1548a2017M Altcode:
The magnetic field structure of sunspots above the photosphere remain
poorly understood due to limitations in observations and the complexity
of these atmospheric layers. In this regard, we studied the large
isolated sunspot (70”× 80”) located in the active region NOAA
12546 with spectro-polarimetric measurements acquired along the Fe I
617.3 nm and Ca II 854.2 nm lines with the IBIS/DST instrument, under
excellent seeing conditions lasting more than three hours. Using the
Non Local Thermodynamic Equilibrium inversion code we inverted both
line measurements simultaneously to retrieve the three-dimensional
magnetic and thermal structure of the penumbral region from the
bottom of the photosphere to the middle chromosphere. The analysis
of data acquired at spectral ranges unexplored allow us to show clear
evidence of the spine and intra-spine structure of the magnetic field at
chromospheric heights. In particular, we found a peak-to-peak variations
of the magnetic field strength and inclination of about 200 G and 10°
chromospheric heights, respectively, and of about 300 G and 20° in the
photosphere. We also investigated the structure of the magnetic field
gradient in the penumbra along the vertical and azimuthal directions,
confirming previous results reported in the literature from data taken
at the spectral region of the He I 1083 nm triplet.
---------------------------------------------------------
Title: A 3-Year Sample of Almost 1,600 Elves Recorded Above South
America by the Pierre Auger Cosmic-Ray Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albuquerque, I. F. M.;
Albury, J. M.; Allekotte, I.; Almela, A.; Alvarez Castillo, J.;
Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.;
Andringa, S.; Aramo, C.; Asorey, H.; Assis, P.; Avila, G.; Badescu,
A. M.; Bakalova, A.; Balaceanu, A.; Barbato, F.; Barreira Luz, R. J.;
Baur, S.; Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.;
Bertou, X.; Biermann, P. L.; Biteau, J.; Blaess, S. G.; Blanco,
A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Botti, A. M.; Brack, J.; Bretz, T.; Bridgeman, A.;
Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.;
Caballero-Mora, K. S.; Caccianiga, L.; Calcagni, L.; Cancio, A.;
Canfora, F.; Carceller, J. M.; Caruso, R.; Castellina, A.; Catalani,
F.; Cataldi, G.; Cazon, L.; Cerda, M.; Chinellato, J. A.; Chudoba, J.;
Chytka, L.; Clay, R. W.; Cobos Cerutti, A. C.; Colalillo, R.; Coleman,
A.; Coluccia, M. R.; Conceição, R.; Condorelli, A.; Consolati,
G.; Contreras, F.; Cooper, M. J.; Coutu, S.; Covault, C. E.; Daniel,
B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; Day, J. A.; de Almeida,
R. M.; de Jong, S. J.; Mauro, G.; de Mello Neto, J. R. T.; Mitri, I.;
de Oliveira, J.; de Oliveira Salles, F. O.; de Souza, V.; Debatin,
J.; del Río, M.; Deligny, O.; Dhital, N.; Díaz Castro, M. L.;
Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.; Dorosti, Q.; dos Anjos,
R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.; Erdmann, M.;
Escobar, C. O.; Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar, G.;
Fauth, A. C.; Fazzini, N.; Feldbusch, F.; Fenu, F.; Ferreyro, L. P.;
Figueira, J. M.; Filipčič, A.; Freire, M. M.; Fujii, T.; Fuster, A.;
García, B.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari,
U.; Giammarchi, M.; Giller, M.; Głas, D.; Glombitza, J.; Gobbi, F.;
Golup, G.; Gómez Berisso, M.; Gómez Vitale, P. F.; Gongora, J. P.;
González, N.; Goos, I.; Góra, D.; Gorgi, A.; Gottowik, M.; Grubb,
T. D.; Guarino, F.; Guedes, G. P.; Guido, E.; Halliday, R.; Hampel,
M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Harvey, V. M.; Haungs,
A.; Hebbeker, T.; Heck, D.; Heimann, P.; Hill, G. C.; Hojvat, C.;
Holt, E. M.; Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.;
Huege, T.; Hulsman, J.; Insolia, A.; Isar, P. G.; Jandt, I.; Johnsen,
J. A.; Josebachuili, M.; Jurysek, J.; Kääpä, A.; Kampert, K. H.;
Keilhauer, B.; Kemmerich, N.; Kemp, J.; Klages, H. O.; Kleifges, M.;
Kleinfeller, J.; Krause, R.; Kuempel, D.; Kukec Mezek, G.; Kuotb Awad,
A.; Lago, B. L.; LaHurd, D.; Lang, R. G.; Legumina, R.; Leigui de
Oliveira, M. A.; Lenok, V.; Letessier-Selvon, A.; Lhenry-Yvon, I.;
Lippmann, O. C.; Lo Presti, D.; Lopes, L.; López, R.; López Casado,
A.; Lorek, R.; Luce, Q.; Lucero, A.; Malacari, M.; Mancarella, G.;
Mandat, D.; Manning, B. C.; Mantsch, P.; Mariazzi, A. G.; Mariş,
I. C.; Marsella, G.; Martello, D.; Martinez, H.; Martínez Bravo, O.;
Mastrodicasa, M.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthiae,
G.; Mayotte, E.; Mazur, P. O.; Medina-Tanco, G.; Melo, D.; Menshikov,
A.; Merenda, K. -D.; Michal, S.; Micheletti, M. I.; Middendorf, L.;
Miramonti, L.; Mitrica, B.; Mockler, D.; Mollerach, S.; Montanet, F.;
Morello, C.; Morlino, G.; Mostafá, M.; Müller, A. L.; Muller, M. A.;
Müller, S.; Mussa, R.; Nellen, L.; Nguyen, P. H.; Niculescu-Oglinzanu,
M.; Niechciol, M.; Nitz, D.; Nosek, D.; Novotny, V.; Noža, L.; Nucita,
A.; Núñez, L. A.; Olinto, A.; Palatka, M.; Pallotta, J.; Panetta,
M. P.; Papenbreer, P.; Parente, G.; Parra, A.; Pech, M.; Pedreira,
F.; Pekala, J.; Pelayo, R.; Peña-Rodriguez, J.; Pereira, L. A. S.;
Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.; Phuntsok, J.; Pierog,
T.; Pimenta, M.; Pirronello, V.; Platino, M.; Poh, J.; Pont, B.;
Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Puyleart, A.;
Querchfeld, S.; Quinn, S.; Ramos-Pollan, R.; Rautenberg, J.; Ravignani,
D.; Reininghaus, M.; Ridky, J.; Riehn, F.; Risse, M.; Ristori, P.;
Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Rojo, J.; Roncoroni,
M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl, P.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Salina, G.; Sanabria Gomez,
J. D.; Sánchez, F.; Santos, E. M.; Santos, E.; Sarazin, F.; Sarmento,
R.; Sarmiento-Cano, C.; Sato, R.; Savina, P.; Schauer, M.; Scherini,
V.; Schieler, H.; Schimassek, M.; Schimp, M.; Schlüter, F.; Schmidt,
D.; Scholten, O.; Schovánek, P.; Schröder, F. G.; Schröder, S.;
Schumacher, J.; Sciutto, S. J.; Scornavacche, M.; Shellard, R. C.;
Sigl, G.; Silli, G.; Sima, O.; Å mída, R.; Snow, G. R.; Sommers, P.;
Soriano, J. F.; Souchard, J.; Squartini, R.; Stanca, D.; Stanič, S.;
Stasielak, J.; Stassi, P.; Stolpovskiy, M.; Streich, A.; Suarez, F.;
Suárez-Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky, A. D.;
Å upík, J.; Szadkowski, Z.; Taboada, A.; Taborda, O. A.; Tapia,
A.; Timmermans, C.; Todero Peixoto, C. J.; Tomé, B.; Torralba Elipe,
G.; Travaini, A.; Travnicek, P.; Trini, M.; Tueros, M.; Ulrich, R.;
Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore,
L.; van Bodegom, P.; van den Berg, A. M.; van Vliet, A.; Varela,
E.; Vargas Cárdenas, B.; Veberič, D.; Ventura, C.; Vergara Quispe,
I. D.; Verzi, V.; Vicha, J.; Villaseñor, L.; Vink, J.; Vorobiov, S.;
Wahlberg, H.; Watson, A. A.; Weber, M.; Weindl, A.; Wiedeński, M.;
Wiencke, L.; Wilczyński, H.; Winchen, T.; Wirtz, M.; Wittkowski,
D.; Wundheiler, B.; Yang, L.; Yushkov, A.; Zas, E.; Zavrtanik, D.;
Zavrtanik, M.; Zehrer, L.; Zepeda, A.; Zimmermann, B.; Ziolkowski,
M.; Zong, Z.; Zuccarello, F.
2020E&SS....700582A Altcode:
Elves are a class of transient luminous events, with a radial extent
typically greater than 250 km, that occur in the lower ionosphere above
strong electrical storms. We report the observation of 1,598 elves,
from 2014 to 2016, recorded with unprecedented time resolution (100 ns)
using the fluorescence detector (FD) of the Pierre Auger Cosmic-Ray
Observatory. The Auger Observatory is located in the Mendoza province
of Argentina with a viewing footprint for elve observations of 3·106
km<SUP>2</SUP>, reaching areas above the Pacific and Atlantic Oceans,
as well as the Córdoba region, which is known for severe convective
thunderstorms. Primarily designed for ultrahigh energy cosmic-ray
observations, the Auger FD turns out to be very sensitive to the
ultraviolet emission in elves. The detector features modified Schmidt
optics with large apertures resulting in a field of view that spans the
horizon, and year-round operation on dark nights with low moonlight
background, when the local weather is favorable. The measured light
profiles of 18% of the elve events have more than one peak, compatible
with intracloud activity. Within the 3-year sample, 72% of the elves
correlate with the far-field radiation measurements of the World Wide
Lightning Location Network. The Auger Observatory plans to continue
operations until at least 2025, including elve observations and
analysis. To the best of our knowledge, this observatory is the only
facility on Earth that measures elves with year-round operation and
full horizon coverage.
---------------------------------------------------------
Title: Cosmic-Ray Anisotropies in Right Ascension Measured by the
Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albuquerque, I. F. M.;
Albury, J. M.; Allekotte, I.; Almela, A.; Alvarez Castillo, J.;
Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.;
Andringa, S.; Aramo, C.; Araújo Ferreira, P. R.; Asorey, H.; Assis,
P.; Avila, G.; Badescu, A. M.; Bakalova, A.; Balaceanu, A.; Barbato,
F.; Barreira Luz, R. J.; Becker, K. H.; Bellido, J. A.; Berat, C.;
Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Bister, T.; Biteau,
J.; Blanco, A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.;
Bonifazi, C.; Bonneau Arbeletche, L.; Borodai, N.; Botti, A. M.; Brack,
J.; Bretz, T.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink,
S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, L.; Calcagni,
L.; Cancio, A.; Canfora, F.; Caracas, I.; Carceller, J. M.; Caruso,
R.; Castellina, A.; Catalani, F.; Cataldi, G.; Cazon, L.; Cerda,
M.; Chinellato, J. A.; Choi, K.; Chudoba, J.; Chytka, L.; Clay,
R. W.; Cobos Cerutti, A. C.; Colalillo, R.; Coleman, A.; Coluccia,
M. R.; Conceição, R.; Condorelli, A.; Consolati, G.; Contreras,
F.; Convenga, F.; Covault, C. E.; Dasso, S.; Daumiller, K.; Dawson,
B. R.; Day, J. A.; de Almeida, R. M.; de Jesús, J.; de Jong, S. J.;
De Mauro, G.; de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira,
J.; de Oliveira Franco, D.; de Souza, V.; Debatin, J.; del Río,
M.; Deligny, O.; Dhital, N.; Di Matteo, A.; Castro, M. L. Díaz;
Dobrigkeit, C.; D'Olivo, J. C.; Dorosti, Q.; dos Anjos, R. C.; Dova,
M. T.; Ebr, J.; Engel, R.; Epicoco, I.; Erdmann, M.; Escobar, C. O.;
Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar, G.; Fauth, A. C.;
Fazzini, N.; Feldbusch, F.; Fenu, F.; Fick, B.; Figueira, J. M.;
Filipčič, A.; Freire, M. M.; Fujii, T.; Fuster, A.; Galea, C.;
Galelli, C.; García, B.; Garcia Vegas, A. L.; Gemmeke, H.; Gesualdi,
F.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.;
Giller, M.; Glombitza, J.; Gobbi, F.; Golup, G.; Gómez Berisso, M.;
Gómez Vitale, P. F.; Gongora, J. P.; González, N.; Goos, I.; Góra,
D.; Gorgi, A.; Gottowik, M.; Grubb, T. D.; Guarino, F.; Guedes, G. P.;
Guido, E.; Hahn, S.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari,
D.; Harvey, V. M.; Haungs, A.; Hebbeker, T.; Heck, D.; Hill, G. C.;
Hojvat, C.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.;
Hulsman, J.; Insolia, A.; Isar, P. G.; Johnsen, J. A.; Jurysek, J.;
Kääpä, A.; Kampert, K. H.; Keilhauer, B.; Kemp, J.; Klages, H. O.;
Kleifges, M.; Kleinfeller, J.; Köpke, M.; Mezek, G. Kukec; Kuotb
Awad, A.; Lago, B. L.; LaHurd, D.; Lang, R. G.; Leigui de Oliveira,
M. A.; Lenok, V.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Lo Presti, D.;
Lopes, L.; López, R.; López Casado, A.; Lorek, R.; Luce, Q.; Lucero,
A.; Machado Payeras, A.; Malacari, M.; Mancarella, G.; Mandat, D.;
Manning, B. C.; Manshanden, J.; Mantsch, P.; Mariazzi, A. G.; Mariş,
I. C.; Marsella, G.; Martello, D.; Martinez, H.; Martínez Bravo, O.;
Mastrodicasa, M.; Mathes, H. J.; Matthews, J.; Matthiae, G.; Mayotte,
E.; Mazur, P. O.; Medina-Tanco, G.; Melo, D.; Menshikov, A.; Merenda,
K. -D.; Michal, S.; Micheletti, M. I.; Miramonti, L.; Mockler, D.;
Mollerach, S.; Montanet, F.; Morello, C.; Morlino, G.; Mostafá, M.;
Müller, A. L.; Muller, M. A.; Müller, S.; Mussa, R.; Muzio, M.;
Namasaka, W. M.; Nellen, L.; Niculescu-Oglinzanu, M.; Niechciol, M.;
Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.; Nucita, A.; Núñez,
L. A.; Palatka, M.; Pallotta, J.; Panetta, M. P.; Papenbreer, P.;
Parente, G.; Parra, A.; Pech, M.; Pedreira, F.; Pȩkala, J.; Pelayo,
R.; Peña-Rodriguez, J.; Pereira, L. A. S.; Perez Armand, J.; Perlin,
M.; Perrone, L.; Peters, C.; Petrera, S.; Pierog, T.; Pimenta, M.;
Pirronello, V.; Platino, M.; Pont, B.; Pothast, M.; Privitera, P.;
Prouza, M.; Puyleart, A.; Querchfeld, S.; Rautenberg, J.; Ravignani,
D.; Reininghaus, M.; Ridky, J.; Riehn, F.; Risse, M.; Ristori, P.;
Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Rojo, J.; Roncoroni,
M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl, P.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Salina, G.; Sanabria Gomez,
J. D.; Sánchez, F.; Santos, E. M.; Santos, E.; Sarazin, F.; Sarmento,
R.; Sarmiento-Cano, C.; Sato, R.; Savina, P.; Schäfer, C.; Scherini,
V.; Schieler, H.; Schimassek, M.; Schimp, M.; Schlüter, F.; Schmidt,
D.; Scholten, O.; Schovánek, P.; Schröder, F. G.; Schröder, S.;
Sciutto, S. J.; Scornavacche, M.; Shellard, R. C.; Sigl, G.; Silli,
G.; Sima, O.; Šmída, R.; Sommers, P.; Soriano, J. F.; Souchard, J.;
Squartini, R.; Stadelmaier, M.; Stanca, D.; Stanič, S.; Stasielak,
J.; Stassi, P.; Streich, A.; Suárez-Durán, M.; Sudholz, T.;
Suomijärvi, T.; Supanitsky, A. D.; Šupík, J.; Szadkowski, Z.;
Taboada, A.; Taborda, O. A.; Tapia, A.; Timmermans, C.; Tobiska, P.;
Todero Peixoto, C. J.; Tomé, B.; Torralba Elipe, G.; Travaini, A.;
Travnicek, P.; Trimarelli, C.; Trini, M.; Tueros, M.; Ulrich, R.;
Unger, M.; Urban, M.; Vaclavek, L.; Valdés Galicia, J. F.; Valiño,
I.; Valore, L.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.;
Vásquez-Ramírez, A.; Veberič, D.; Ventura, C.; Vergara Quispe,
I. D.; Verzi, V.; Vicha, J.; Villaseñor, L.; Vink, J.; Vorobiov,
S.; Wahlberg, H.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.;
Wilczyński, H.; Winchen, T.; Wirtz, M.; Wittkowski, D.; Wundheiler,
B.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zehrer, L.;
Zepeda, A.; Ziolkowski, M.; Zuccarello, F.; Pierre Auger Collaboration
2020ApJ...891..142A Altcode: 2020arXiv200206172T
We present measurements of the large-scale cosmic-ray (CR) anisotropies
in R.A., using data collected by the surface detector array of the
Pierre Auger Observatory over more than 14 yr. We determine the
equatorial dipole component, d<SUB>\perp</SUB>, through a Fourier
analysis in R.A. that includes weights for each event so as to account
for the main detector-induced systematic effects. For the energies at
which the trigger efficiency of the array is small, the "east-west"
method is employed. Besides using the data from the array with
detectors separated by 1500 m, we also include data from the smaller
but denser subarray of detectors with 750 m separation, which allows
us to extend the analysis down to ∼0.03 EeV. The most significant
equatorial dipole amplitude obtained is that in the cumulative bin
above 8 EeV, d<SUB>\perp</SUB>={6.0}<SUB>-0.9</SUB><SUP>+1.0</SUP>
%, which is inconsistent with isotropy at the 6σ level. In the bins
below 8 EeV, we obtain 99% CL upper bounds on d<SUB>⊥</SUB> at the
level of 1%-3%. At energies below 1 EeV, even though the amplitudes
are not significant, the phases determined in most of the bins are not
far from the R.A. of the Galactic center, at α<SUB>GC</SUB> = -94°,
suggesting a predominantly Galactic origin for anisotropies at these
energies. The reconstructed dipole phases in the energy bins above
4 EeV point instead to R.A. that are almost opposite to the Galactic
center one, indicative of an extragalactic CR origin.
---------------------------------------------------------
Title: Impact of small-scale emerging flux from the photosphere to
the corona: a case study from IRIS
Authors: Guglielmino, Salvo L.; Young, Peter R.; Zuccarello, Francesca;
Romano, Paolo; Murabito, Mariarita
2020IAUS..354..439G Altcode:
We report on multi-wavelength ultraviolet (UV) high-resolution
observations taken with the IRIS satellite during the emergence
phase of an emerging flux region embedded in the unipolar plage of
active region NOAA 12529. These data are complemented by measurements
taken with the spectropolarimeter aboard the Hinode satellite and by
observations from SDO.
---------------------------------------------------------
Title: The 3D structure of the penumbra at high resolution from the
bottom of the photosphere to the middle chromosphere
Authors: Murabito, Mariarita; Ermolli, Ilaria; Giorgi, Fabrizio;
Stangalini, Marco; Guglielmino, Salvo L.; Jafarzadeh, Shahin;
Socas-Navarro, Hector; Romano, Paolo; Zuccarello, Francesca
2020IAUS..354..448M Altcode:
Sunspots are the most prominent feature of the solar magnetism in the
photosphere. Although they have been widely investigated in the past,
their structure remains poorly understood. Indeed, due to limitations
in observations and the complexity of the magnetic field estimation
at chromospheric heights, the magnetic field structure of sunspot
above the photosphere is still uncertain. Improving the present
knowledge of sunspot is important in solar and stellar physics,
since spot generation is seen not only on the Sun, but also on other
solar-type stars. In this regard, we studied a large, isolated sunspot
with spectro-polarimeteric measurements that were acquired at the Fe
I 6173 nm and Ca II 8542 nm lines by the spectropolarimeter IBIS/DST
under excellent seeing conditions lasting more than three hours. Using
the Non-LTE inversion code NICOLE, we inverted both line measurements
simultaneously, to retrieve the three-dimensional magnetic and thermal
structure of the penumbral region from the bottom of the photosphere
to the middle chromosphere. Our analysis of data acquired at spectral
ranges unexplored in previous studies shows clear spine and intra-spine
structure of the penumbral magnetic field at chromopheric heights. Our
investigation of the magnetic field gradient in the penumbra along
the vertical and azimuthal directions confirms results reported in
the literature from analysis of data taken at the spectral region of
the He I 1083 nm triplet.
---------------------------------------------------------
Title: Continuum Enhancements, Line Profiles, and Magnetic Field
Evolution during Consecutive Flares
Authors: Zuccarello, Francesca; Guglielmino, Salvo L.; Capparelli,
Vincenzo; Mathioudakis, Mihalis; Keys, Peter H.; Criscuoli, Serena;
Falco, Mariachiara; Murabito, Mariarita
2020ApJ...889...65Z Altcode: 2019arXiv191200859Z
During solar flares, magnetic energy can be converted into
electromagnetic radiation from radio waves to γ-rays. Enhancements in
the continuum at visible wavelengths, as well as continuum enhancements
in the FUV and NUV passbands, give rise to white-light flares. In
addition, the strong energy release in these events can lead to
the rearrangement of the magnetic field at the photospheric level,
causing morphological changes in large and stable magnetic structures
like sunspots. In this context, we describe observations acquired
by satellite instruments (Interface Region Imaging Spectrograph
(IRIS), Solar Dynamics Observatory/Helioseismic and Magnetic Imager,
Hinode/Solar Optical Telescope) and ground-based telescopes (Rapid
Oscillations in the Solar Atmosphere (ROSA)/Dunn Solar Telescope)
during two consecutive C7.0 and X1.6 flares that occurred in active
region NOAA 12205 on 2014 November 7. The flare was accompanied by an
eruption. The results of the analysis show the presence of continuum
enhancements during the evolution of the events, observed both in ROSA
images and in IRIS spectra. In the latter, a prominent blueshifted
component is observed at the onset of the eruption. We investigate
the role played by the evolution of the δ sunspots of the active
region in the flare triggering, and finally we discuss the changes in
the penumbrae surrounding these sunspots as a further consequence of
these flares.
---------------------------------------------------------
Title: Science Requirement Document (SRD) for the European Solar
Telescope (EST) (2nd edition, December 2019)
Authors: Schlichenmaier, R.; Bellot Rubio, L. R.; Collados, M.;
Erdelyi, R.; Feller, A.; Fletcher, L.; Jurcak, J.; Khomenko, E.;
Leenaarts, J.; Matthews, S.; Belluzzi, L.; Carlsson, M.; Dalmasse,
K.; Danilovic, S.; Gömöry, P.; Kuckein, C.; Manso Sainz, R.;
Martinez Gonzalez, M.; Mathioudakis, M.; Ortiz, A.; Riethmüller,
T. L.; Rouppe van der Voort, L.; Simoes, P. J. A.; Trujillo Bueno,
J.; Utz, D.; Zuccarello, F.
2019arXiv191208650S Altcode:
The European Solar Telescope (EST) is a research infrastructure
for solar physics. It is planned to be an on-axis solar telescope
with an aperture of 4 m and equipped with an innovative suite of
spectro-polarimetric and imaging post-focus instrumentation. The EST
project was initiated and is driven by EAST, the European Association
for Solar Telescopes. EAST was founded in 2006 as an association
of 14 European countries. Today, as of December 2019, EAST consists
of 26 European research institutes from 18 European countries. The
Preliminary Design Phase of EST was accomplished between 2008 and
2011. During this phase, in 2010, the first version of the EST Science
Requirement Document (SRD) was published. After EST became a project
on the ESFRI roadmap 2016, the preparatory phase started. The goal
of the preparatory phase is to accomplish a final design for the
telescope and the legal governance structure of EST. A major milestone
on this path is to revisit and update the Science Requirement Document
(SRD). The EST Science Advisory Group (SAG) has been constituted by
EAST and the Board of the PRE-EST EU project in November 2017 and has
been charged with the task of providing with a final statement on the
science requirements for EST. Based on the conceptual design, the SRD
update takes into account recent technical and scientific developments,
to ensure that EST provides significant advancement beyond the current
state-of-the-art. The present update of the EST SRD has been developed
and discussed during a series of EST SAG meetings. The SRD develops
the top-level science objectives of EST into individual science
cases. Identifying critical science requirements is one of its main
goals. Those requirements will define the capabilities of EST and the
post-focus instrument suite. The technical requirements for the final
design of EST will be derived from the SRD.
---------------------------------------------------------
Title: Limits on point-like sources of ultra-high-energy neutrinos
with the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albuquerque, I. F. M.;
Albury, J. M.; Allekotte, I.; Almela, A.; Alvarez Castillo, J.;
Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.;
Andringa, S.; Aramo, C.; Asorey, H.; Assis, P.; Avila, G.; Badescu,
A. M.; Bakalova, A.; Balaceanu, A.; Barbato, F.; Barreira Luz, R. J.;
Baur, S.; Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.;
Bertou, X.; Biermann, P. L.; Biteau, J.; Blanco, A.; Blazek, J.;
Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi, C.; Borodai, N.;
Botti, A. M.; Brack, J.; Bretz, T.; Bridgeman, A.; Briechle, F. L.;
Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora,
K. S.; Caccianiga, L.; Calcagni, L.; Cancio, A.; Canfora, F.;
Caracas, I.; Carceller, J. M.; Caruso, R.; Castellina, A.; Catalani,
F.; Cataldi, G.; Cazon, L.; Cerda, M.; Chinellato, J. A.; Choi, K.;
Chudoba, J.; Chytka, L.; Clay, R. W.; Cobos Cerutti, A. C.; Colalillo,
R.; Coleman, A.; Coluccia, M. R.; Conceição, R.; Condorelli, A.;
Consolati, G.; Contreras, F.; Convenga, F.; Cooper, M. J.; Coutu,
S.; Covault, C. E.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson,
B. R.; Day, J. A.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza, V.;
Debatin, J.; del Río, M.; Deligny, O.; Dhital, N.; Di Matteo, A.;
Díaz Castro, M. L.; Dobrigkeit, C.; D'Olivo, J. C.; Dorosti, Q.; dos
Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.; Erdmann,
M.; Escobar, C. O.; Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar,
G.; Fauth, A. C.; Fazzini, N.; Feldbusch, F.; Fenu, F.; Ferreyro,
L. P.; Figueira, J. M.; Filipčič, A.; Freire, M. M.; Fujii, T.;
Fuster, A.; García, B.; Gemmeke, H.; Gesualdi, F.; Gherghel-Lascu,
A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Głas,
D.; Glombitza, J.; Gobbi, F.; Golup, G.; Gómez Berisso, M.; Gómez
Vitale, P. F.; Gongora, J. P.; González, N.; Goos, I.; Góra, D.;
Gorgi, A.; Gottowik, M.; Grubb, T. D.; Guarino, F.; Guedes, G. P.;
Guido, E.; Hahn, S.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari,
D.; Harrison, T. A.; Harvey, V. M.; Haungs, A.; Hebbeker, T.; Heck,
D.; Heimann, P.; Hill, G. C.; Hojvat, C.; Holt, E. M.; Homola, P.;
Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman,
J.; Insolia, A.; Isar, P. G.; Johnsen, J. A.; Jurysek, J.; Kääpä,
A.; Kampert, K. H.; Keilhauer, B.; Kemmerich, N.; Kemp, J.; Klages,
H. O.; Kleifges, M.; Kleinfeller, J.; Kuempel, D.; Kukec Mezek, G.;
Kuotb Awad, A.; Lago, B. L.; LaHurd, D.; Lang, R. G.; Legumina,
R.; Leigui de Oliveira, M. A.; Lenok, V.; Letessier-Selvon, A.;
Lhenry-Yvon, I.; Lippmann, O. C.; Lo Presti, D.; Lopes, L.; López,
R.; López Casado, A.; Lorek, R.; Luce, Q.; Lucero, A.; Malacari, M.;
Mancarella, G.; Mandat, D.; Manning, B. C.; Manshanden, J.; Mantsch,
P.; Mariazzi, A. G.; Mariş, I. C.; Marsella, G.; Martello, D.;
Martinez, H.; Martínez Bravo, O.; Mastrodicasa, M.; Mathes, H. J.;
Mathys, S.; Matthews, J.; Matthiae, G.; Mayotte, E.; Mazur, P. O.;
Medina-Tanco, G.; Melo, D.; Menshikov, A.; Merenda, K. -D.; Michal,
S.; Micheletti, M. I.; Miramonti, L.; Mockler, D.; Mollerach, S.;
Montanet, F.; Morello, C.; Morlino, G.; Mostafá, M.; Müller, A. L.;
Muller, M. A.; Müller, S.; Mussa, R.; Namasaka, W. M.; Nellen, L.;
Niculescu-Oglinzanu, M.; Niechciol, M.; Nitz, D.; Nosek, D.; Novotny,
V.; Nožka, L.; Nucita, A.; Núñez, L. A.; Olinto, A.; Palatka, M.;
Pallotta, J.; Panetta, M. P.; Papenbreer, P.; Parente, G.; Parra, A.;
Pech, M.; Pedreira, F.; Pȩkala, J.; Pelayo, R.; Peña-Rodriguez, J.;
Pereira, L. A. S.; Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.;
Phuntsok, J.; Pierog, T.; Pimenta, M.; Pirronello, V.; Platino, M.;
Poh, J.; Pont, B.; Porowski, C.; Pothast, M.; Prado, R. R.; Privitera,
P.; Prouza, M.; Puyleart, A.; Querchfeld, S.; Quinn, S.; Ramos-Pollan,
R.; Rautenberg, J.; Ravignani, D.; Reininghaus, M.; Ridky, J.; Riehn,
F.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.;
Rodriguez Rojo, J.; Roncoroni, M. J.; Roth, M.; Roulet, E.; Rovero,
A. C.; Ruehl, P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar,
H.; Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Santos, E. M.;
Santos, E.; Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.;
Savina, P.; Schauer, M.; Scherini, V.; Schieler, H.; Schimassek, M.;
Schimp, M.; Schlüter, F.; Schmidt, D.; Scholten, O.; Schovánek,
P.; Schröder, F. G.; Schröder, S.; Schumacher, J.; Sciutto, S. J.;
Scornavacche, M.; Shellard, R. C.; Sigl, G.; Silli, G.; Sima, O.;
Šmída, R.; Snow, G. R.; Sommers, P.; Soriano, J. F.; Souchard, J.;
Squartini, R.; Stadelmaier, M.; Stanca, D.; Stanič, S.; Stasielak, J.;
Stassi, P.; Stolpovskiy, M.; Streich, A.; Suárez-Durán, M.; Sudholz,
T.; Suomijärvi, T.; Supanitsky, A. D.; Šupík, J.; Szadkowski, Z.;
Taboada, A.; Taborda, O. A.; Tapia, A.; Timmermans, C.; Tobiska, P.;
Todero Peixoto, C. J.; Tomé, B.; Torralba Elipe, G.; Travaini, A.;
Travnicek, P.; Trini, M.; Tueros, M.; Ulrich, R.; Unger, M.; Urban,
M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.; van Bodegom,
P.; van den Berg, A. M.; van Vliet, A.; Varela, E.; Vargas Cárdenas,
B.; Vásquez-Ramírez, A.; Veberič, D.; Ventura, C.; Vergara Quispe,
I. D.; Verzi, V.; Vicha, J.; Villaseñor, L.; Vink, J.; Vorobiov, S.;
Wahlberg, H.; Watson, A. A.; Weber, M.; Weindl, A.; Wiedeński, M.;
Wiencke, L.; Wilczyński, H.; Winchen, T.; Wirtz, M.; Wittkowski,
D.; Wundheiler, B.; Yang, L.; Yushkov, A.; Zas, E.; Zavrtanik, D.;
Zavrtanik, M.; Zehrer, L.; Zepeda, A.; Zimmermann, B.; Ziolkowski,
M.; Zuccarello, F.
2019JCAP...11..004A Altcode: 2019arXiv190607419T
With the Surface Detector array (SD) of the Pierre Auger Observatory
we can detect neutrinos with energy between 10<SUP>17</SUP> eV and
10<SUP>20</SUP> eV from point-like sources across the sky, from close
to the Southern Celestial Pole up to 60<SUP>o</SUP> in declination,
with peak sensitivities at declinations around ~ -53<SUP>o</SUP> and
~+55<SUP>o</SUP>, and an unmatched sensitivity for arrival directions in
the Northern hemisphere. A search has been performed for highly-inclined
air showers induced by neutrinos of all flavours with no candidate
events found in data taken between 1 Jan 2004 and 31 Aug 2018. Upper
limits on the neutrino flux from point-like steady sources have been
derived as a function of source declination. An unrivaled sensitivity is
achieved in searches for transient sources with emission lasting over an
hour or less, if they occur within the field of view corresponding to
the zenith angle range between 60<SUP>o</SUP> and 95<SUP>o</SUP> where
the SD of the Pierre Auger Observatory is most sensitive to neutrinos.
---------------------------------------------------------
Title: Data-driven estimation of the invisible energy of cosmic ray
showers with the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albuquerque, I. F. M.;
Albury, J. M.; Allekotte, I.; Almela, A.; Alvarez Castillo, J.;
Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.;
Andringa, S.; Aramo, C.; Asorey, H.; Assis, P.; Avila, G.; Badescu,
A. M.; Bakalova, A.; Balaceanu, A.; Barbato, F.; Barreira Luz, R. J.;
Baur, S.; Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.;
Bertou, X.; Biermann, P. L.; Biteau, J.; Blaess, S. G.; Blanco,
A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Botti, A. M.; Brack, J.; Bretz, T.; Bridgeman, A.;
Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.;
Caballero-Mora, K. S.; Caccianiga, L.; Calcagni, L.; Cancio, A.;
Canfora, F.; Carceller, J. M.; Caruso, R.; Castellina, A.; Catalani,
F.; Cataldi, G.; Cazon, L.; Cerda, M.; Chinellato, J. A.; Chudoba,
J.; Chytka, L.; Clay, R. W.; Cobos Cerutti, A. C.; Colalillo, R.;
Coleman, A.; Coluccia, M. R.; Conceição, R.; Condorelli, A.;
Consolati, G.; Contreras, F.; Convenga, F.; Cooper, M. J.; Coutu,
S.; Covault, C. E.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson,
B. R.; Day, J. A.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Oliveira
Salles, F. O.; de Souza, V.; Debatin, J.; del Río, M.; Deligny, O.;
Dhital, N.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo,
J. C.; Dorosti, Q.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr,
J.; Engel, R.; Erdmann, M.; Escobar, C. O.; Etchegoyen, A.; Falcke,
H.; Farmer, J.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Feldbusch, F.;
Fenu, F.; Ferreyro, L. P.; Figueira, J. M.; Filipčič, A.; Freire,
M. M.; Fujii, T.; Fuster, A.; García, B.; Gemmeke, H.; Gherghel-Lascu,
A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Głas, D.;
Glombitza, J.; Gobbi, F.; Golup, G.; Gómez Berisso, M.; Gómez Vitale,
P. F.; Gongora, J. P.; González, N.; Goos, I.; Góra, D.; Gorgi,
A.; Gottowik, M.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Guido,
E.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison,
T. A.; Harvey, V. M.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.;
Hill, G. C.; Hojvat, C.; Holt, E. M.; Homola, P.; Hörandel, J. R.;
Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman, J.; Insolia, A.;
Isar, P. G.; Jandt, I.; Johnsen, J. A.; Josebachuili, M.; Jurysek,
J.; Kääpä, A.; Kampert, K. H.; Keilhauer, B.; Kemmerich, N.;
Kemp, J.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.;
Kuempel, D.; Kukec Mezek, G.; Kuotb Awad, A.; Lago, B. L.; LaHurd,
D.; Lang, R. G.; Legumina, R.; Leigui de Oliveira, M. A.; Lenok, V.;
Letessier-Selvon, A.; Lhenry-Yvon, I.; Lippmann, O. C.; Lo Presti,
D.; Lopes, L.; López, R.; López Casado, A.; Lorek, R.; Luce,
Q.; Lucero, A.; Malacari, M.; Mancarella, G.; Mandat, D.; Manning,
B. C.; Mantsch, P.; Mariazzi, A. G.; Mariş, I. C.; Marsella, G.;
Martello, D.; Martinez, H.; Martínez Bravo, O.; Mastrodicasa, M.;
Mathes, H. J.; Mathys, S.; Matthews, J.; Matthiae, G.; Mayotte, E.;
Mazur, P. O.; Medina-Tanco, G.; Melo, D.; Menshikov, A.; Merenda,
K. -D.; Michal, S.; Micheletti, M. I.; Middendorf, L.; Miramonti, L.;
Mitrica, B.; Mockler, D.; Mollerach, S.; Montanet, F.; Morello, C.;
Morlino, G.; Mostafá, M.; Müller, A. L.; Muller, M. A.; Müller,
S.; Mussa, R.; Nellen, L.; Nguyen, P. H.; Niculescu-Oglinzanu, M.;
Niechciol, M.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.; Nucita,
A.; Núñez, L. A.; Olinto, A.; Palatka, M.; Pallotta, J.; Panetta,
M. P.; Papenbreer, P.; Parente, G.; Parra, A.; Pech, M.; Pedreira,
F.; Pękala, J.; Pelayo, R.; Peña-Rodriguez, J.; Pereira, L. A. S.;
Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.; Phuntsok, J.; Pierog,
T.; Pimenta, M.; Pirronello, V.; Platino, M.; Poh, J.; Pont, B.;
Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Puyleart, A.;
Querchfeld, S.; Quinn, S.; Ramos-Pollan, R.; Rautenberg, J.; Ravignani,
D.; Reininghaus, M.; Ridky, J.; Riehn, F.; Risse, M.; Ristori, P.;
Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Rojo, J.; Roncoroni,
M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl, P.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Salina, G.; Sanabria Gomez,
J. D.; Sánchez, F.; Santos, E. M.; Santos, E.; Sarazin, F.; Sarmento,
R.; Sarmiento-Cano, C.; Sato, R.; Savina, P.; Schauer, M.; Scherini,
V.; Schieler, H.; Schimassek, M.; Schimp, M.; Schlüter, F.; Schmidt,
D.; Scholten, O.; Schovánek, P.; Schröder, F. G.; Schröder, S.;
Schumacher, J.; Sciutto, S. J.; Scornavacche, M.; Shellard, R. C.;
Sigl, G.; Silli, G.; Sima, O.; Šmída, R.; Snow, G. R.; Sommers, P.;
Soriano, J. F.; Souchard, J.; Squartini, R.; Stanca, D.; Stanič, S.;
Stasielak, J.; Stassi, P.; Stolpovskiy, M.; Streich, A.; Suarez, F.;
Suárez-Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky, A. D.;
Šupík, J.; Szadkowski, Z.; Taboada, A.; Taborda, O. A.; Tapia, A.;
Timmermans, C.; Todero Peixoto, C. J.; Tomé, B.; Torralba Elipe,
G.; Travaini, A.; Travnicek, P.; Trini, M.; Tueros, M.; Ulrich, R.;
Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore,
L.; van Bodegom, P.; van den Berg, A. M.; van Vliet, A.; Varela,
E.; Vargas Cárdenas, B.; Veberič, D.; Ventura, C.; Vergara Quispe,
I. D.; Verzi, V.; Vicha, J.; Villaseñor, L.; Vink, J.; Vorobiov, S.;
Wahlberg, H.; Watson, A. A.; Weber, M.; Weindl, A.; Wiedeński, M.;
Wiencke, L.; Wilczyński, H.; Winchen, T.; Wirtz, M.; Wittkowski,
D.; Wundheiler, B.; Yang, L.; Yushkov, A.; Zas, E.; Zavrtanik, D.;
Zavrtanik, M.; Zehrer, L.; Zepeda, A.; Zimmermann, B.; Ziolkowski,
M.; Zong, Z.; Zuccarello, F.; Pierre Auger Collaboration
2019PhRvD.100h2003A Altcode: 2019arXiv190108040T
The determination of the primary energy of extensive air showers using
the fluorescence detection technique requires an estimation of the
energy carried away by particles that do not deposit all their energy
in the atmosphere. This estimation is typically made using Monte Carlo
simulations and thus depends on the assumed primary particle mass and
on model predictions for neutrino and muon production. In this work we
present a new method to obtain the invisible energy from events detected
by the Pierre Auger Observatory. The method uses measurements of the
muon number at ground level, and it allows us to significantly reduce
the systematic uncertainties related to the mass composition and the
high energy hadronic interaction models, and consequently to improve
the estimation of the energy scale of the Pierre Auger Observatory.
---------------------------------------------------------
Title: IBIS-A: The IBIS Solar Spectro-polarimetric Data Archive
Authors: Ermolli, Ilaria; Giordano, Silvio; Giorgi, Fabrizio; Guido,
Vincenzo; Marassi, Alessandro; Volpicelli, Antonio; Di Marcantonio,
Paolo; Zuccarello, Francesca; Cauzzi, Gianna
2019ASPC..521..431E Altcode:
We review the efforts undertaken to set up the archive of the IBIS
ground-based solar spectro-polarimetric observations into the VO
framework, according to the SOLARNET standards, by using SOAP/XML and
RESTful Web Services.
---------------------------------------------------------
Title: Probing the origin of ultra-high-energy cosmic rays with
neutrinos in the EeV energy range using the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albuquerque, I. F. M.;
Albury, J. M.; Allekotte, I.; Almela, A.; Alvarez Castillo, J.;
Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.;
Andringa, S.; Aramo, C.; Asorey, H.; Assis, P.; Avila, G.; Badescu,
A. M.; Bakalova, A.; Balaceanu, A.; Barbato, F.; Barreira Luz, R. J.;
Baur, S.; Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.;
Bertou, X.; Biermann, P. L.; Biteau, J.; Blanco, A.; Blazek, J.;
Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi, C.; Borodai, N.;
Botti, A. M.; Brack, J.; Bretz, T.; Bridgeman, A.; Briechle, F. L.;
Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora,
K. S.; Caccianiga, L.; Calcagni, L.; Cancio, A.; Canfora, F.;
Caracas, I.; Carceller, J. M.; Caruso, R.; Castellina, A.; Catalani,
F.; Cataldi, G.; Cazon, L.; Cerda, M.; Chinellato, J. A.; Choi, K.;
Chudoba, J.; Chytka, L.; Clay, R. W.; Cobos Cerutti, A. C.; Colalillo,
R.; Coleman, A.; Coluccia, M. R.; Conceição, R.; Condorelli, A.;
Consolati, G.; Contreras, F.; Convenga, F.; Cooper, M. J.; Coutu,
S.; Covault, C. E.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson,
B. R.; Day, J. A.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza, V.;
Debatin, J.; del Río, M.; Deligny, O.; Dhital, N.; Di Matteo, A.;
Díaz Castro, M. L.; Dobrigkeit, C.; D'Olivo, J. C.; Dorosti, Q.; dos
Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.; Erdmann,
M.; Escobar, C. O.; Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar,
G.; Fauth, A. C.; Fazzini, N.; Feldbusch, F.; Fenu, F.; Ferreyro,
L. P.; Figueira, J. M.; Filipčič, A.; Freire, M. M.; Fujii, T.;
Fuster, A.; García, B.; Gemmeke, H.; Gesualdi, F.; Gherghel-Lascu,
A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Głas,
D.; Glombitza, J.; Gobbi, F.; Golup, G.; Gómez Berisso, M.; Gómez
Vitale, P. F.; Gongora, J. P.; González, N.; Goos, I.; Góra, D.;
Gorgi, A.; Gottowik, M.; Grubb, T. D.; Guarino, F.; Guedes, G. P.;
Guido, E.; Hahn, S.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari,
D.; Harrison, T. A.; Harvey, V. M.; Haungs, A.; Hebbeker, T.; Heck,
D.; Heimann, P.; Hill, G. C.; Hojvat, C.; Holt, E. M.; Homola, P.;
Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman,
J.; Insolia, A.; Isar, P. G.; Johnsen, J. A.; Jurysek, J.; Kääpä,
A.; Kampert, K. H.; Keilhauer, B.; Kemmerich, N.; Kemp, J.; Klages,
H. O.; Kleifges, M.; Kleinfeller, J.; Kuempel, D.; Kukec Mezek, G.;
Kuotb Awad, A.; Lago, B. L.; LaHurd, D.; Lang, R. G.; Legumina,
R.; Leigui de Oliveira, M. A.; Lenok, V.; Letessier-Selvon, A.;
Lhenry-Yvon, I.; Lippmann, O. C.; Lo Presti, D.; Lopes, L.; López,
R.; López Casado, A.; Lorek, R.; Luce, Q.; Lucero, A.; Malacari, M.;
Mancarella, G.; Mandat, D.; Manning, B. C.; Manshanden, J.; Mantsch,
P.; Mariazzi, A. G.; Mariş, I. C.; Marsella, G.; Martello, D.;
Martinez, H.; Martínez Bravo, O.; Mastrodicasa, M.; Mathes, H. J.;
Mathys, S.; Matthews, J.; Matthiae, G.; Mayotte, E.; Mazur, P. O.;
Medina-Tanco, G.; Melo, D.; Menshikov, A.; Merenda, K. -D.; Michal,
S.; Micheletti, M. I.; Miramonti, L.; Mockler, D.; Mollerach, S.;
Montanet, F.; Morello, C.; Morlino, G.; Mostafá, M.; Müller, A. L.;
Muller, M. A.; Müller, S.; Mussa, R.; Namasaka, W. M.; Nellen, L.;
Niculescu-Oglinzanu, M.; Niechciol, M.; Nitz, D.; Nosek, D.; Novotny,
V.; Nožka, L.; Nucita, A.; Núñez, L. A.; Olinto, A.; Palatka, M.;
Pallotta, J.; Panetta, M. P.; Papenbreer, P.; Parente, G.; Parra, A.;
Pech, M.; Pedreira, F.; Pȩkala, J.; Pelayo, R.; Peña-Rodriguez, J.;
Pereira, L. A. S.; Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.;
Phuntsok, J.; Pierog, T.; Pimenta, M.; Pirronello, V.; Platino, M.;
Poh, J.; Pont, B.; Porowski, C.; Pothast, M.; Prado, R. R.; Privitera,
P.; Prouza, M.; Puyleart, A.; Querchfeld, S.; Quinn, S.; Ramos-Pollan,
R.; Rautenberg, J.; Ravignani, D.; Reininghaus, M.; Ridky, J.; Riehn,
F.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.;
Rodriguez Rojo, J.; Roncoroni, M. J.; Roth, M.; Roulet, E.; Rovero,
A. C.; Ruehl, P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar,
H.; Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Santos, E. M.;
Santos, E.; Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.;
Savina, P.; Schauer, M.; Scherini, V.; Schieler, H.; Schimassek, M.;
Schimp, M.; Schlüter, F.; Schmidt, D.; Scholten, O.; Schovánek,
P.; Schröder, F. G.; Schröder, S.; Schumacher, J.; Sciutto, S. J.;
Scornavacche, M.; Shellard, R. C.; Sigl, G.; Silli, G.; Sima, O.;
Šmída, R.; Snow, G. R.; Sommers, P.; Soriano, J. F.; Souchard, J.;
Squartini, R.; Stadelmaier, M.; Stanca, D.; Stanič, S.; Stasielak, J.;
Stassi, P.; Stolpovskiy, M.; Streich, A.; Suárez-Durán, M.; Sudholz,
T.; Suomijärvi, T.; Supanitsky, A. D.; Šupík, J.; Szadkowski, Z.;
Taboada, A.; Taborda, O. A.; Tapia, A.; Timmermans, C.; Tobiska, P.;
Todero Peixoto, C. J.; Tomé, B.; Torralba Elipe, G.; Travaini, A.;
Travnicek, P.; Trini, M.; Tueros, M.; Ulrich, R.; Unger, M.; Urban,
M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.; van Bodegom,
P.; van den Berg, A. M.; van Vliet, A.; Varela, E.; Vargas Cárdenas,
B.; Vásquez-Ramírez, A.; Veberič, D.; Ventura, C.; Vergara Quispe,
I. D.; Verzi, V.; Vicha, J.; Villaseñor, L.; Vink, J.; Vorobiov, S.;
Wahlberg, H.; Watson, A. A.; Weber, M.; Weindl, A.; Wiedeński, M.;
Wiencke, L.; Wilczyński, H.; Winchen, T.; Wirtz, M.; Wittkowski,
D.; Wundheiler, B.; Yang, L.; Yushkov, A.; Zas, E.; Zavrtanik, D.;
Zavrtanik, M.; Zehrer, L.; Zepeda, A.; Zimmermann, B.; Ziolkowski,
M.; Zuccarello, F.
2019JCAP...10..022A Altcode: 2019arXiv190607422T
Neutrinos with energies above 10<SUP>17</SUP> eV are detectable
with the Surface Detector Array of the Pierre Auger Observatory. The
identification is efficiently performed for neutrinos of all flavors
interacting in the atmosphere at large zenith angles, as well as for
Earth-skimming τ neutrinos with nearly tangential trajectories relative
to the Earth. No neutrino candidates were found in ~ 14.7 years of data
taken up to 31 August 2018. This leads to restrictive upper bounds on
their flux. The 90% C.L. single-flavor limit to the diffuse flux of
ultra-high-energy neutrinos with an E<SUB>ν</SUB><SUP>-2</SUP> spectrum
in the energy range 1.0 × 10<SUP>17</SUP> eV -2.5 × 10<SUP>19</SUP>
eV is E<SUP>2</SUP> dN<SUB>ν</SUB>/dE<SUB>ν</SUB> < 4.4 ×
10<SUP>-9</SUP> GeV cm<SUP>-2</SUP> s<SUP>-1</SUP> sr<SUP>-1</SUP>,
placing strong constraints on several models of neutrino production at
EeV energies and on the properties of the sources of ultra-high-energy
cosmic rays.
---------------------------------------------------------
Title: The Pierre Auger Observatory: Contributions to the 36th
International Cosmic Ray Conference (ICRC 2019)
Authors: The Pierre Auger Collaboration; Aab, A.; Abreu, P.; Aglietta,
M.; Albuquerque, I. F. M.; Albury, J. M.; Allekotte, I.; Almela, A.;
Alvarez Castillo, J.; Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui,
L.; Andrada, B.; Andringa, S.; Aramo, C.; Asorey, H.; Assis, P.;
Avila, G.; Badescu, A. M.; Bakalova, A.; Balaceanu, A.; Barbato, F.;
Barreira Luz, R. J.; Baur, S.; Becker, K. H.; Bellido, J. A.; Berat,
C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Bister, T.; Biteau,
J.; Blanco, A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli,
D.; Bonifazi, C.; Borodai, N.; Botti, A. M.; Brack, J.; Bretz, T.;
Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.;
Caballero-Mora, K. S.; Caccianiga, L.; Calcagni, L.; Cancio, A.;
Canfora, F.; Caracas, I.; Carceller, J. M.; Caruso, R.; Castellina,
A.; Catalani, F.; Cataldi, G.; Cazon, L.; Cerda, M.; Chinellato,
J. A.; Choi, K.; Chudoba, J.; Chytka, L.; Clay, R. W.; Cobos Cerutti,
A. C.; Colalillo, R.; Coleman, A.; Coluccia, M. R.; Conceição, R.;
Condorelli, A.; Consolati, G.; Contreras, F.; Convenga, F.; Cooper,
M. J.; Coutu, S.; Covault, C. E.; Daniel, B.; Dasso, S.; Daumiller,
K.; Dawson, B. R.; Day, J. A.; de Almeida, R. M.; de Jong, S. J.;
De Mauro, G.; de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira,
J.; de Souza, V.; Debatin, J.; del Río, M.; Deligny, O.; Dhital, N.;
Di Matteo, A.; Díaz Castro, M. L.; Dobrigkeit, C.; D'Olivo, J. C.;
Dorosti, Q.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.;
Engel, R.; Erdmann, M.; Escobar, C. O.; Etchegoyen, A.; Falcke, H.;
Farmer, J.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Feldbusch, F.;
Fenu, F.; Ferreyro, L. P.; Figueira, J. M.; Filipčič, A.; Freire,
M. M.; Fujii, T.; Fuster, A.; García, B.; Gemmeke, H.; Gesualdi, F.;
Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller,
M.; Głas, D.; Glombitza, J.; Gobbi, F.; Golup, G.; Gómez Berisso,
M.; Gómez Vitale, P. F.; Gongora, J. P.; González, N.; Goos, I.;
Góra, D.; Gorgi, A.; Gottowik, M.; Grubb, T. D.; Guarino, F.; Guedes,
G. P.; Guido, E.; Hahn, S.; Halliday, R.; Hampel, M. R.; Hansen, P.;
Harari, D.; Harrison, T. A.; Harvey, V. M.; Haungs, A.; Hebbeker,
T.; Heck, D.; Hill, G. C.; Hojvat, C.; Holt, E. M.; Hörandel, J. R.;
Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman, J.; Insolia, A.; Isar,
P. G.; Johnsen, J. A.; Jurysek, J.; Kääpä, A.; Kampert, K. H.;
Keilhauer, B.; Kemmerich, N.; Kemp, J.; Klages, H. O.; Kleifges,
M.; Kleinfeller, J.; Kukec Mezek, G.; Kuotb Awad, A.; Lago, B. L.;
LaHurd, D.; Lang, R. G.; Legumina, R.; Leigui de Oliveira, M. A.;
Lenok, V.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Lippmann, O. C.;
Lo Presti, D.; Lopes, L.; López, R.; López Casado, A.; Lorek,
R.; Luce, Q.; Lucero, A.; Malacari, M.; Mancarella, G.; Mandat,
D.; Manning, B. C.; Manshanden, J.; Mantsch, P.; Mariazzi, A. G.;
Mariş, I. C.; Marsella, G.; Martello, D.; Martinez, H.; Martínez
Bravo, O.; Mastrodicasa, M.; Mathes, H. J.; Mathys, S.; Matthews,
J.; Matthiae, G.; Mayotte, E.; Mazur, P. O.; Medina-Tanco, G.; Melo,
D.; Menshikov, A.; Merenda, K. -D.; Michal, S.; Micheletti, M. I.;
Miramonti, L.; Mockler, D.; Mollerach, S.; Montanet, F.; Morello, C.;
Morlino, G.; Mostafá, M.; Müller, A. L.; Muller, M. A.; Müller,
S.; Mussa, R.; Namasaka, W. M.; Nellen, L.; Niculescu-Oglinzanu, M.;
Niechciol, M.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.; Nucita,
A; Núñez, L. A.; Olinto, A.; Palatka, M.; Pallotta, J.; Panetta,
M. P.; Papenbreer, P.; Parente, G.; Parra, A.; Pech, M.; Pedreira,
F.; Pękala, J.; Pelayo, R.; Peña-Rodriguez, J.; Pereira, L. A. S.;
Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.; Phuntsok, J.;
Pierog, T.; Pimenta, M.; Pirronello, V.; Platino, M.; Poh, J.; Pont,
B.; Pothast, M.; Prado, R. R.; Privitera, P.; Prouza, M.; Puyleart,
A.; Querchfeld, S.; Ramos-Pollan, R.; Rautenberg, J.; Ravignani,
D.; Reininghaus, M.; Ridky, J.; Riehn, F.; Risse, M.; Ristori, P.;
Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Rojo, J.; Roncoroni,
M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl, P.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Salina, G.; Sanabria Gomez,
J. D.; Sánchez, F.; Santos, E. M.; Santos, E.; Sarazin, F.; Sarmento,
R.; Sarmiento-Cano, C.; Sato, R.; Savina, P.; Schauer, M.; Scherini,
V.; Schieler, H.; Schimassek, M.; Schimp, M.; Schlüter, F.; Schmidt,
D.; Scholten, O.; Schovánek, P.; Schröder, F. G.; Schröder, S.;
Schumacher, J.; Sciutto, S. J.; Scornavacche, M.; Shellard, R. C.;
Sigl, G.; Silli, G.; Sima, O.; Šmída, R.; Snow, G. R.; Sommers,
P.; Soriano, J. F.; Souchard, J.; Squartini, R.; Stadelmaier, M.;
Stanca, D.; Stanič, S.; Stasielak, J.; Stassi, P.; Stolpovskiy,
M.; Streich, A.; Suárez-Durán, M.; Sudholz, T.; Suomijärvi, T.;
Supanitsky, A. D.; Šupík, J.; Szadkowski, Z.; Taboada, A.; Taborda,
O. A.; Tapia, A.; Timmermans, C.; Tobiska, P.; Todero Peixoto, C. J.;
Tomé, B.; Torralba Elipe, G.; Travaini, A.; Travnicek, P.; Trini,
M.; Tueros, M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia,
J. F.; Valiño, I.; Valore, L.; van den Berg, A. M.; van Vliet, A.;
Varela, E.; Vargas Cárdenas, B.; Vásquez-Ramírez, A.; Veberič, D.;
Ventura, C.; Vergara Quispe, I. D.; Verzi, V.; Vicha, J.; Villaseñor,
L.; Vink, J.; Vorobiov, S.; Wahlberg, H.; Watson, A. A.; Weber, M.;
Weindl, A.; Wiedeński, M.; Wiencke, L.; Wilczyński, H.; Winchen,
T.; Wirtz, M.; Wittkowski, D.; Wundheiler, B.; Yang, L.; Yushkov,
A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zehrer, L.; Zepeda, A.;
Zimmermann, B.; Ziolkowski, M.; Zuccarello, F.
2019arXiv190909073T Altcode:
Contributions of the Pierre Auger Collaboration to the 36th
International Cosmic Ray Conference (ICRC 2019), 24 July - 1 August
2019, Madison, Wisconsin, USA.
---------------------------------------------------------
Title: SpectroPolarimetric Analysis of an Umbral Filament
Authors: Guglielmino, S.; Romano, P.; Cobo, B. R.; Zuccarello,
F. . Murabito, M.
2019spw..confE..12G Altcode: 2020arXiv200108509G
High-resolution observations of the solar photosphere have recently
revealed the presence of elongated filamentary bright structures inside
sunspot umbrae. These features, which have been called umbral filaments
(UFs), differ in morphology, evolution, and magnetic configuration from
light bridges that are usually observed to intrude in sunspots. To
study an UF observed in the leading sunspot of active region NOAA
12529, we have analyzed spectro-polarimetric observations taken in
the photosphere with the spectropolarimeter (SP) aboard the Hinode
satellite. High-resolution observations in the upper chromosphere
and transition region taken with the IRIS telescope and observations
acquired by SDO/HMI and SDO/AIA have been used to complement the
spectro-polarimetric analysis. The results obtained from the inversion
of the Hinode/SP measurements allow us to discard the hypothesis that
UFs are a kind of light bridge. In fact, we find no field-free or
low-field strength region cospatial to the observed UF. In contrast,
we detect in the structure Stokes profiles that indicate the presence of
strong horizontal fields, larger than 2500 G. Furthermore, a significant
portion of the UF has opposite polarity with respect to the hosting
umbra. In the upper atmospheric layers, we observe filaments being
cospatial to the UF in the photosphere. We interpret these findings
as suggesting that the UF could be the photospheric manifestation of
a flux rope hanging above the sunspot, which triggers the formation
of penumbral-like filaments within the umbra via magneto-convection.
---------------------------------------------------------
Title: Properties of the Umbral Filament Observed in Active Region
NOAA 12529
Authors: Guglielmino, Salvo L.; Romano, Paolo; Ruiz Cobo, Basilio;
Zuccarello, Francesca; Murabito, Mariarita
2019ApJ...880...34G Altcode: 2019arXiv190600065G
Recent observations of the solar photosphere revealed the presence
of elongated filamentary bright structures inside sunspot umbrae,
called umbral filaments (UFs). These features differ in morphology,
magnetic configuration, and evolution from light bridges (LBs) that are
usually observed to intrude in sunspots. To characterize a UF observed
in the umbra of the giant leading sunspot of active region NOAA 12529,
we analyze high-resolution observations taken in the photosphere with
the spectropolarimeter on board the Hinode satellite and in the upper
chromosphere and transition region with the IRIS telescope. The results
of this analysis definitely rule out the hypothesis that the UF might
be a kind of LB. In fact, we find no field-free or low-field strength
region cospatial to the UF. Conversely, we recognize the presence of
a strong horizontal field larger than 2500 G, a significant portion
of the UF with opposite polarity with respect to the surroundings,
and filaments in the upper atmospheric layers corresponding to the
UF in the photosphere. These findings suggest that this structure
is the photospheric manifestation of a flux rope hanging above the
sunspot and forming penumbral-like filaments within the umbra via
magneto-convection. This reinforces a previously proposed scenario.
---------------------------------------------------------
Title: On the Magnetic Nature of Solar Exploding Granules
Authors: Guglielmino, S. L.; Martínez Pillet, V.; Ruiz Cobo,
B.; Bellot Rubio, L. R.; del Toro Iniesta, J. C.; Solanki, S. K.;
Zuccarello, F.
2019ASPC..526..299G Altcode:
We report on spectropolarimetric observations acquired by the imaging
magnetograph SUNRISE/IMaX at high spatial 0.”3 and temporal (31.5 s)
resolution during the first science flight of this balloon-borne solar
observatory. We describe the photospheric evolution of an exploding
granule observed in the quiet Sun. This granule is cospatial with
a magnetic flux emergence event occurring at mesogranular scales
(up to ∼12 Mm<SUP>2</SUP> area). Using a modified version of the
SIR code, we show that we can estimate the longitudinal field also
in the presence of a residual cross-talk in these IMaX longitudinal
measurements. We determine the magnetic flux content of the structure
(∼3 ×10<SUP>18</SUP> Mx), which appears to have a multipolar
configuration, and discuss the origin of such flux emergence events.
---------------------------------------------------------
Title: Formation of the Penumbra and Start of the Evershed Flow
Authors: Murabito, M.; Romano, P.; Guglielmino, S. L.; Zuccarello,
F.; Solanki, S. K.
2019ASPC..526..243M Altcode:
We analyze high-resolution observations of Active Region NOAA 11490,
acquired on 2012 May 28 and 29. Spectropolarimetric measurements of
the photospheric lines of Fe I at 617.3 nm and 630.25 nm were taken
with the Interferometric BIdimensional Spectrometer (IBIS), mounted on
NSO/DST, during about 30 minutes for each day. To study the evolution
of continuum intensity, LOS velocity, inclination and strength of the
magnetic field during the entire time interval, we also used data taken
by SDO/HMI. We used the SIR code to invert the Stokes profiles observed
with IBIS, using different initial models to take into account the
physical conditions of the plasma in the region of umbra, penumbra,
and quiet Sun. From the analysis of the SIR results, we found that,
before the formation of the penumbra, the annular zone is characterized
by downflows in the inner part. Furthermore, we observed that the onset
of the classical Evershed flow occurs on a short time scale, 1-3 hours,
while the penumbra is forming. In order to investigate the conditions
that lead to the establishment of the classical Evershed flow, we
analyzed the evolution of the continuum intensity, LOS velocity,
inclination and strength of the magnetic field in a segment in the
north-western part of the leading spot. In about 1 hour, we noted a
clear evolution from redshift to blueshift in the penumbral filaments
along the selected segment. We propose a scenario in which the penumbra
is formed by magnetic flux dragged down from the canopy surrounding
the initial pore: the Evershed flow starts when the sinking magnetic
field dips below the solar surface and magnetoconvection sets in.
---------------------------------------------------------
Title: Multi-Messenger Physics with the Pierre Auger Observatory
Authors: The Pierre Auger Collaboration; Aab, A.; Abreu, P.; Aglietta,
M.; Albuquerque, I. F. M.; Albury, J. M.; Allekotte, I.; Almela, A.;
Alvarez Castillo, J.; Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui,
L.; Andrada, B.; Andringa, S.; Aramo, C.; Asorey, H.; Assis, P.;
Avila, G.; Badescu, A. M.; Bakalova, A.; Balaceanu, A.; Barbato, F.;
Barreira Luz, R. J.; Baur, S.; Becker, K. H.; Bellido, J. A.; Berat,
C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Biteau, J.; Blaess,
S. G.; Blanco, A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli,
D.; Bonifazi, C.; Borodai, N.; Botti, A. M.; Brack, J.; Bretz, T.;
Bridgeman, A.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink,
S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, L.; Calcagni, L.;
Cancio, A.; Canfora, F.; Carceller, J. M.; Caruso, R.; Castellina, A.;
Catalani, F.; Cataldi, G.; Cazon, L.; Cerda, M.; Chinellato, J. A.;
Chudoba, J.; Chytka, L.; Clay, R. W.; Cobos Cerutti, A. C.; Colalillo,
R.; Coleman, A.; Coluccia, M. R.; Conceição, R.; Condorelli, A.;
Consolati, G.; Contreras, F.; Convenga, F.; Cooper, M. J.; Coutu,
S.; Covault, C. E.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson,
B. R.; Day, J. A.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Oliveira
Salles, F. O.; de Souza, V.; Debatin, J.; del Río, M.; Deligny, O.;
Dhital, N.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo,
J. C.; Dorosti, Q.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr,
J.; Engel, R.; Erdmann, M.; Escobar, C. O.; Etchegoyen, A.; Falcke,
H.; Farmer, J.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Feldbusch, F.;
Fenu, F.; Ferreyro, L. P.; Figueira, J. M.; Filipčič, A.; Freire,
M. M.; Fujii, T.; Fuster, A.; García, B.; Gemmeke, H.; Gherghel-Lascu,
A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Głas, D.;
Glombitza, J.; Gobbi, F.; Golup, G.; Gómez Berisso, M.; Gómez Vitale,
P. F.; Gongora, J. P.; González, N.; Goos, I.; Góra, D.; Gorgi,
A.; Gottowik, M.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Guido,
E.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison,
T. A.; Harvey, V. M.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.;
Hill, G. C.; Hojvat, C.; Holt, E. M.; Homola, P.; Hörandel, J. R.;
Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman, J.; Insolia, A.;
Isar, P. G.; Jandt, I.; Johnsen, J. A.; Josebachuili, M.; Jurysek,
J.; Kääpä, A.; Kampert, K. H.; Keilhauer, B.; Kemmerich, N.;
Kemp, J.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.;
Kuempel, D.; Kukec Mezek, G.; Kuotb Awad, A.; Lago, B. L.; LaHurd,
D.; Lang, R. G.; Legumina, R.; Leigui de Oliveira, M. A.; Lenok, V.;
Letessier-Selvon, A.; Lhenry-Yvon, I.; Lippmann, O. C.; Lo Presti,
D.; Lopes, L.; López, R.; López Casado, A.; Lorek, R.; Luce, Q.;
Lucero, A.; Malacari, M.; Mancarella, G.; Mandat, D.; Manning, B. C.;
Mantsch, P.; Mariazzi, A. G.; Mariş, I. C.; Marsella, G.; Martello,
D.; Martinez, H.; Martínez Bravo, O.; Mastrodicasa, M.; Mathes,
H. J.; Mathys, S.; Matthews, J.; Matthiae, G.; Mayotte, E.; Mazur,
P. O.; Medina-Tanco, G.; Melo, D.; Menshikov, A.; Merenda, K. -D.;
Michal, S.; Micheletti, M. I.; Middendorf, L.; Miramonti, L.; Mitrica,
B.; Mockler, D.; Mollerach, S.; Montanet, F.; Morello, C.; Morlino,
G.; Mostafá, M.; Müller, A. L.; Muller, M. A.; Müller, S.; Mussa,
R.; Nellen, L.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol,
M.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.; Nucita, A; Núñez,
L. A.; Oikonomou, F.; Olinto, A.; Palatka, M.; Pallotta, J.; Panetta,
M. P.; Papenbreer, P.; Parente, G.; Parra, A.; Pech, M.; Pedreira,
F.; Pękala, J.; Pelayo, R.; Peña-Rodriguez, J.; Pereira, L. A. S.;
Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.; Phuntsok, J.; Pierog,
T.; Pimenta, M.; Pirronello, V.; Platino, M.; Poh, J.; Pont, B.;
Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Puyleart, A.;
Querchfeld, S.; Quinn, S.; Ramos-Pollan, R.; Rautenberg, J.; Ravignani,
D.; Reininghaus, M.; Ridky, J.; Riehn, F.; Risse, M.; Ristori, P.;
Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Rojo, J.; Roncoroni,
M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl, P.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Salina, G.; Sanabria Gomez,
J. D.; Sánchez, F.; Santos, E. M.; Santos, E.; Sarazin, F.; Sarmento,
R.; Sarmiento-Cano, C.; Sato, R.; Savina, P.; Schauer, M.; Scherini,
V.; Schieler, H.; Schimassek, M.; Schimp, M.; Schlüter, F.; Schmidt,
D.; Scholten, O.; Schovánek, P.; Schröder, F. G.; Schröder, S.;
Schumacher, J.; Sciutto, S. J.; Scornavacche, M.; Shellard, R. C.;
Sigl, G.; Silli, G.; Sima, O.; Šmída, R.; Snow, G. R.; Sommers, P.;
Soriano, J. F.; Souchard, J.; Squartini, R.; Stanca, D.; Stanič, S.;
Stasielak, J.; Stassi, P.; Stolpovskiy, M.; Streich, A.; Suarez, F.;
Suárez-Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky, A. D.;
Šupík, J.; Szadkowski, Z.; Taboada, A.; Taborda, O. A.; Tapia, A.;
Timmermans, C.; Todero Peixoto, C. J.; Tomé, B.; Torralba Elipe,
G.; Travaini, A.; Travnicek, P.; Trini, M.; Tueros, M.; Ulrich, R.;
Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore,
L.; van Bodegom, P.; van den Berg, A. M.; van Vliet, A.; Varela,
E.; Vargas Cárdenas, B.; Veberič, D.; Ventura, C.; Vergara Quispe,
I. D.; Verzi, V.; Vicha, J.; Villaseñor, L.; Vink, J.; Vorobiov, S.;
Wahlberg, H.; Watson, A. A.; Weber, M.; Weindl, A.; Wiedeński, M.;
Wiencke, L.; Wilczyński, H.; Winchen, T.; Wirtz, M.; Wittkowski,
D.; Wundheiler, B.; Yang, L.; Yushkov, A.; Zas, E.; Zavrtanik, D.;
Zavrtanik, M.; Zehrer, L.; Zepeda, A.; Zimmermann, B.; Ziolkowski,
M.; Zong, Z.; Zuccarello, F.
2019arXiv190411918T Altcode:
An overview of the multi-messenger capabilities of the Pierre
Auger Observatory is presented. The techniques and performance of
searching for Ultra-High Energy neutrinos, photons and neutrons
are described. Some of the most relevant results are reviewed,
such as stringent upper bounds that were placed to a flux of diffuse
cosmogenic neutrinos and photons, bounds placed on neutrinos emitted
from compact binary mergers that were detected by LIGO and Virgo
during their first and second observing runs, as well as searches
for high energy photons and neutrons from the Galactic center that
constrain the properties of the putative Galactic PeVatron, observed
by the H.E.S.S.\ collaboration. The observation of directional
correlations between ultra-high energy cosmic rays and either high
energy astrophysical neutrinos or specific source populations, weighted
by their electromagnetic radiation, are also discussed. They constitute
additional multi-messenger approaches aimed at identifying the sources
of high energy cosmic rays.
---------------------------------------------------------
Title: Measurement of the average shape of longitudinal profiles of
cosmic-ray air showers at the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albuquerque, I. F. M.;
Albury, J. M.; Allekotte, I.; Almela, A.; Alvarez Castillo, J.;
Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.;
Andringa, S.; Aramo, C.; Asorey, H.; Assis, P.; Avila, G.; Badescu,
A. M.; Bakalova, A.; Balaceanu, A.; Barbato, F.; Barreira Luz, R. J.;
Baur, S.; Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.;
Bertou, X.; Biermann, P. L.; Biteau, J.; Blaess, S. G.; Blanco,
A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Botti, A. M.; Brack, J.; Bretz, T.; Bridgeman, A.;
Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.;
Caballero-Mora, K. S.; Caccianiga, L.; Calcagni, L.; Cancio, A.;
Canfora, F.; Carceller, J. M.; Caruso, R.; Castellina, A.; Catalani,
F.; Cataldi, G.; Cazon, L.; Chinellato, J. A.; Chudoba, J.; Chytka,
L.; Clay, R. W.; Cobos Cerutti, A. C.; Colalillo, R.; Coleman, A.;
Coluccia, M. R.; Conceição, R.; Condorelli, A.; Consolati, G.;
Contreras, F.; Cooper, M. J.; Coutu, S.; Covault, C. E.; Daniel, B.;
Dasso, S.; Daumiller, K.; Dawson, B. R.; Day, J. A.; de Almeida,
R. M.; de Jong, S. J.; De Mauro, G.; de Mello Neto, J. R. T.; De
Mitri, I.; de Oliveira, J.; de Oliveira Salles, F. O.; de Souza,
V.; Debatin, J.; Deligny, O.; Dhital, N.; Díaz Castro, M. L.;
Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.; Dorosti, Q.; dos Anjos,
R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.; Erdmann, M.;
Escobar, C. O.; Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar, G.;
Fauth, A. C.; Fazzini, N.; Feldbusch, F.; Fenu, F.; Ferreyro, L. P.;
Figueira, J. M.; Filipčič, A.; Freire, M. M.; Fujii, T.; Fuster, A.;
García, B.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari,
U.; Giammarchi, M.; Giller, M.; Głas, D.; Glombitza, J.; Golup,
G.; Gómez Berisso, M.; Gómez Vitale, P. F.; González, N.; Goos,
I.; Góra, D.; Gorgi, A.; Gottowik, M.; Grubb, T. D.; Guarino, F.;
Guedes, G. P.; Guido, E.; Halliday, R.; Hampel, M. R.; Hansen, P.;
Harari, D.; Harrison, T. A.; Harvey, V. M.; Haungs, A.; Hebbeker,
T.; Heck, D.; Heimann, P.; Hill, G. C.; Hojvat, C.; Holt, E. M.;
Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege,
T.; Hulsman, J.; Insolia, A.; Isar, P. G.; Jandt, I.; Johnsen, J. A.;
Josebachuili, M.; Jurysek, J.; Kääpä, A.; Kampert, K. H.; Keilhauer,
B.; Kemmerich, N.; Kemp, J.; Klages, H. O.; Kleifges, M.; Kleinfeller,
J.; Krause, R.; Kuempel, D.; Kukec Mezek, G.; Kuotb Awad, A.; Lago,
B. L.; LaHurd, D.; Lang, R. G.; Legumina, R.; Leigui de Oliveira,
M. A.; Lenok, V.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Lippmann,
O. C.; Lo Presti, D.; Lopes, L.; López, R.; López Casado, A.; Lorek,
R.; Luce, Q.; Lucero, A.; Malacari, M.; Mancarella, G.; Mandat, D.;
Manning, B. C.; Mantsch, P.; Mariazzi, A. G.; Mariş, I. C.; Marsella,
G.; Martello, D.; Martinez, H.; Martínez Bravo, O.; Mastrodicasa,
M.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthiae, G.; Mayotte,
E.; Mazur, P. O.; Medina-Tanco, G.; Melo, D.; Menshikov, A.; Merenda,
K. -D.; Michal, S.; Micheletti, M. I.; Middendorf, L.; Miramonti, L.;
Mitrica, B.; Mockler, D.; Mollerach, S.; Montanet, F.; Morello, C.;
Morlino, G.; Mostafá, M.; Müller, A. L.; Muller, M. A.; Müller,
S.; Mussa, R.; Nellen, L.; Nguyen, P. H.; Niculescu-Oglinzanu, M.;
Niechciol, M.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.; Nucita,
A.; Núñez, L. A.; Olinto, A.; Palatka, M.; Pallotta, J.; Panetta,
M. P.; Papenbreer, P.; Parente, G.; Parra, A.; Pech, M.; Pedreira,
F.; Pçkala, J.; Pelayo, R.; Peña-Rodriguez, J.; Pereira, L. A. S.;
Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.; Phuntsok, J.;
Pierog, T.; Pimenta, M.; Pirronello, V.; Platino, M.; Poh, J.; Pont,
B.; Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Puyleart,
A.; Querchfeld, S.; Quinn, S.; Ramos-Pollan, R.; Rautenberg, J.;
Ravignani, D.; Reininghaus, M.; Ridky, J.; Riehn, F.; Risse, M.;
Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Rojo,
J.; Roncoroni, M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl,
P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh,
A.; Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Santos, E. M.;
Santos, E.; Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.;
Savina, P.; Schauer, M.; Scherini, V.; Schieler, H.; Schimassek, M.;
Schimp, M.; Schlüter, F.; Schmidt, D.; Scholten, O.; Schovánek,
P.; Schröder, F. G.; Schröder, S.; Schumacher, J.; Sciutto, S. J.;
Scornavacche, M.; Shellard, R. C.; Sigl, G.; Silli, G.; Sima, O.;
Šmída, R.; Snow, G. R.; Sommers, P.; Soriano, J. F.; Souchard, J.;
Squartini, R.; Stanca, D.; Stanič, S.; Stasielak, J.; Stassi, P.;
Stolpovskiy, M.; Streich, A.; Suarez, F.; Suárez-Durán, M.; Sudholz,
T.; Suomijärvi, T.; Supanitsky, A. D.; Šupík, J.; Szadkowski, Z.;
Taboada, A.; Taborda, O. A.; Tapia, A.; Timmermans, C.; Todero Peixoto,
C. J.; Tomé, B.; Torralba Elipe, G.; Travnicek, P.; Trini, M.; Tueros,
M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño,
I.; Valore, L.; van Bodegom, P.; van den Berg, A. M.; van Vliet,
A.; Varela, E.; Vargas Cárdenas, B.; Vázquez, R. A.; Veberič, D.;
Ventura, C.; Vergara Quispe, I. D.; Verzi, V.; Vicha, J.; Villaseñor,
L.; Vink, J.; Vorobiov, S.; Wahlberg, H.; Watson, A. A.; Weber, M.;
Weindl, A.; Wiedeński, M.; Wiencke, L.; Wilczyński, H.; Winchen,
T.; Wirtz, M.; Wittkowski, D.; Wundheiler, B.; Yang, L.; Yushkov,
A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zehrer, L.; Zepeda, A.;
Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello, F.
2019JCAP...03..018A Altcode: 2018arXiv181104660T
The profile of the longitudinal development of showers produced by
ultra-high energy cosmic rays carries information related to the
interaction properties of the primary particles with atmospheric
nuclei. In this work, we present the first measurement of the
average shower profile in traversed atmospheric depth at the Pierre
Auger Observatory. The shapes of profiles are well reproduced by
the Gaisser-Hillas parametrization within the range studied, for
E>10<SUP>17.8</SUP> eV . A detailed analysis of the systematic
uncertainties is performed using ten years of data and a full detector
simulation. The average shape is quantified using two variables related
to the width and asymmetry of the profile, and the results are compared
with predictions of hadronic interaction models for different primary
particles.
---------------------------------------------------------
Title: Height Dependence of the Penumbral Fine-scale Structure in
the Inner Solar Atmosphere
Authors: Murabito, Mariarita; Ermolli, I.; Giorgi, F.; Stangalini,
M.; Guglielmino, S. L.; Jafarzadeh, S.; Socas-Navarro, H.; Romano,
P.; Zuccarello, F.
2019ApJ...873..126M Altcode: 2018arXiv181209029M
We studied the physical parameters of the penumbra in a large and fully
developed sunspot, one of the largest over the last two solar cycles,
by using full-Stokes measurements taken at the photospheric Fe I 617.3
nm and chromospheric Ca II 854.2 nm lines with the Interferometric
Bidimensional Spectrometer. Inverting measurements with the Non-LTE
inversion COde (NICOLE) code, we obtained the three-dimensional
structure of the magnetic field in the penumbra from the bottom
of the photosphere up to the middle chromosphere. We analyzed the
azimuthal and vertical gradient of the magnetic field strength and
inclination. Our results provide new insights on the properties of the
penumbral magnetic fields in the chromosphere at atmospheric heights
unexplored in previous studies. We found signatures of the small-scale
spine and intraspine structure of both the magnetic field strength and
inclination at all investigated atmospheric heights. In particular,
we report typical peak-to-peak variations of the field strength and
inclination of ≈300 G and ≈20°, respectively, in the photosphere,
and of ≈200 G and ≈10° in the chromosphere. In addition, we
estimated the vertical gradient of the magnetic field strength in
the studied penumbra: we find a value of ≈0.3 G km<SUP>-1</SUP>
between the photosphere and the middle chromosphere. Interestingly,
the photospheric magnetic field gradient changes sign from negative
in the inner to positive in the outer penumbra.
---------------------------------------------------------
Title: Continuum emission enhancements and penumbral changes observed
during flares by IRIS, ROSA, and Hinode
Authors: Zuccarello, F.; Guglielmino, S. L.; Capparelli, V.;
Mathioudakis, M.; Keys, P.; Fletcher, L.; Criscuoli, S.; Falco, M.;
Murabito, M.
2019NCimC..42...13Z Altcode: 2019arXiv190101732Z
In this paper we describe observations acquired by satellite instruments
( Hinode/SOT and IRIS) and ground-based telescopes (ROSA@DST) during
two consecutive C7.0 and X1.6 flares occurred in active region NOAA
12205 on 2014 November 7. The analysis of these data show the presence
of continuum enhancements during the evolution of the events, observed
both in ROSA images and in IRIS spectra. Moreover, we analyze the role
played by the evolution of the δ sunspots of the active region in the
flare triggering, indicating the disappearance of a large portion of
penumbra around these sunspots.
---------------------------------------------------------
Title: Satellite observations of reconnection between emerging and
pre-existing small-scale magnetic fields
Authors: Guglielmino, S. L.; Zuccarello, F.; Young, P. R.; Romano,
P.; Murabito, M.
2019NCimC..42...33G Altcode: 2019arXiv190101056G
We report multi-wavelength ultraviolet observations taken with the IRIS
satellite, concerning the emergence phase in the upper chromosphere
and transition region of an emerging flux region (EFR) embedded in
the unipolar plage of active region NOAA 12529. The photospheric
configuration of the EFR is analyzed in detail benefitting from
measurements taken with the spectropolarimeter aboard the Hinode
satellite, when the EFR was fully developed. In addition, these data
are complemented by full-disk, simultaneous observations of the
SDO satellite, relevant to the photosphere and the corona. In the
photosphere, magnetic flux emergence signatures are recognized in the
fuzzy granulation, with dark alignments between the emerging polarities,
cospatial with highly inclined fields. In the upper atmospheric
layers, we identify recurrent brightenings that resemble UV bursts,
with counterparts in all coronal passbands. These occur at the edges of
the EFR and in the region of the arch filament system (AFS) cospatial to
the EFR. Jet activity is also found at chromospheric and coronal levels,
near the AFS and the observed brightness enhancement sites. The analysis
of the IRIS line profiles reveals the heating of dense plasma in the
low solar atmosphere and the driving of bi-directional high-velocity
flows with speeds up to 100 km/s at the same locations. Furthermore,
we detect a correlation between the Doppler velocity and line width of
the Si IV 1394 and 1402 Å line profiles in the UV burst pixels and
their skewness. Comparing these findings with previous observations
and numerical models, we suggest evidence of several long-lasting,
small-scale magnetic reconnection episodes between the emerging bipole
and the ambient field. This process leads to the cancellation of a
pre-existing photospheric flux concentration of the plage with the
opposite polarity flux patch of the EFR. The reconnection appears to
occur higher in the atmosphere than usually observed.
---------------------------------------------------------
Title: IRIS Observations of Magnetic Interactions in the Solar
Atmosphere between Preexisting and Emerging Magnetic Fields. II. UV
Emission Properties
Authors: Guglielmino, Salvo L.; Young, Peter R.; Zuccarello, Francesca
2019ApJ...871...82G Altcode: 2018arXiv181207285G
Multiwavelength ultraviolet (UV) observations by the Interface
Region Imaging Spectrograph satellite in active region NOAA 12529
have recently pointed out the presence of long-lasting brightenings,
akin to UV bursts, and simultaneous plasma ejections occurring in
the upper chromosphere and transition region during secondary flux
emergence. These signatures have been interpreted as evidence of
small-scale, recurrent magnetic reconnection episodes between the
emerging flux region (EFR) and the preexisting plage field. Here we
characterize the UV emission of these strong, intermittent brightenings
and study the surge activity above the chromospheric arch filament
system (AFS) overlying the EFR. We analyze the surges and the cospatial
brightenings observed at different wavelengths. We find an asymmetry
in the emission between the blue and red wings of the Si IV λ1402
Å and Mg II k λ2796.3 lines, which clearly outlines the dynamics of
the structures above the AFS that form during the small-scale eruptive
phenomena. We also detect a correlation between the Doppler velocity
and skewness of the Si IV λλ1394 and 1402 line profiles in the UV
burst pixels. Finally, we show that genuine emission in the Fe XII
λ1349.4 line is cospatial to the Si IV brightenings. This definitely
reveals a pure coronal counterpart to the reconnection event.
---------------------------------------------------------
Title: Recent insights on the penumbra formation process
Authors: Murabito, M.; Romano, P.; Zuccarello, F.; Guglielmino, S. L.
2019NCimC..42...11M Altcode: 2019arXiv190105207M
Using high-resolution spectropolarimetric data acquired by IBIS,
as well as SDO/HMI observations, we studied the penumbra formation
in AR NOAA 11490 and in a sample of twelve ARs appeared on the solar
disk on 2011 and 2012, which were characterized by β -type magnetic
field configuration. The results show that the onset of the classical
Evershed flow occurs in a very short time scale, 1-3 hours. Studying
the formation of the first penumbral sector around the following
proto-spot, we found that a stable penumbra forms in the area facing
the opposite polarity, which appears to be co-spatial with an AFS,
i.e. in a flux emergence region, in contrast with the results of the
paper SCHLICHENMAIER R., REZAEI R. ET AL., Astron. Astrophys., 512
(2010) L1 concerning the leading polarity of AR NOAA 11490. Conversely,
analyzing the sample of twelve ARs, we noticed that there is not a
preferred location for the formation of the first penumbral sector. We
also observed before the penumbra formation an inverse Evershed flow,
which changes its sign when the penumbra appears. This confirms the
observational evidence that the appearance of the penumbral filaments
is correlated with the transition from the inverse Evershed to the
classical Evershed flow. Furthermore, the analysis suggests that the
time needed to form the penumbra may be related to the location where
the penumbra first appears. New high-resolution observations, like those
that will be provided by the European Solar Telescope, are expected
to increase our understanding of the penumbra formation process.
---------------------------------------------------------
Title: Spectro-polarimetric analysis of a short lived solar active
region
Authors: Viavattene, G.; Zuccarello, F.; Collados Vera, , M.; Ruiz
Cobo, B.
2019NCimC..42...10V Altcode:
The physical processes related to the formation, evolution
and disappearance of solar active regions are not completely
clear. High-resolution solar spectro-polarimetric data are needed
to investigate these processes with unprecedented details. Here we
present the analysis of the short-lived NOAA 12549 active region using
high-resolution spectro-polarimetric data acquired with the GREGOR
solar telescope and the GRIS instrument, inverted using the SIR code.
---------------------------------------------------------
Title: Large-scale Cosmic-Ray Anisotropies above 4 EeV Measured by
the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albuquerque, I. F. M.;
Albury, J. M.; Allekotte, I.; Almela, A.; Alvarez Castillo, J.;
Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.;
Andringa, S.; Aramo, C.; Asorey, H.; Assis, P.; Avila, G.; Badescu,
A. M.; Balaceanu, A.; Barbato, F.; Barreira Luz, R. J.; Baur, S.;
Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.;
Biermann, P. L.; Biteau, J.; Blaess, S. G.; Blanco, A.; Blazek, J.;
Bleve, C.; Boháčová, M.; Bonifazi, C.; Borodai, N.; Botti, A. M.;
Brack, J.; Bretz, T.; Bridgeman, A.; Briechle, F. L.; Buchholz,
P.; Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.;
Caccianiga, L.; Calcagni, L.; Cancio, A.; Canfora, F.; Carceller,
J. M.; Caruso, R.; Castellina, A.; Catalani, F.; Cataldi, G.;
Cazon, L.; Chinellato, J. A.; Chudoba, J.; Chytka, L.; Clay, R. W.;
Cobos Cerutti, A. C.; Colalillo, R.; Coleman, A.; Coluccia, M. R.;
Conceição, R.; Consolati, G.; Contreras, F.; Cooper, M. J.; Coutu,
S.; Covault, C. E.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson,
B. R.; Day, J. A.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza,
V.; Debatin, J.; Deligny, O.; Dhital, N.; Díaz Castro, M. L.;
Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.; Dorosti, Q.; dos Anjos,
R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.; Erdmann, M.;
Escobar, C. O.; Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar, G.;
Fauth, A. C.; Fazzini, N.; Feldbusch, F.; Fenu, F.; Ferreyro, L. P.;
Figueira, J. M.; Filipčič, A.; Freire, M. M.; Fujii, T.; Fuster, A.;
García, B.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari,
U.; Giammarchi, M.; Giller, M.; Głas, D.; Glombitza, J.; Golup, G.;
Gómez Berisso, M.; Gómez Vitale, P. F.; González, N.; Goos, I.;
Góra, D.; Gorgi, A.; Gottowik, M.; Grubb, T. D.; Guarino, F.; Guedes,
G. P.; Guido, E.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari,
D.; Harrison, T. A.; Harvey, V. M.; Haungs, A.; Hebbeker, T.; Heck,
D.; Heimann, P.; Hill, G. C.; Hojvat, C.; Holt, E. M.; Homola, P.;
Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman, J.;
Insolia, A.; Isar, P. G.; Jandt, I.; Johnsen, J. A.; Josebachuili, M.;
Jurysek, J.; Kääpä, A.; Kampert, K. H.; Keilhauer, B.; Kemmerich,
N.; Kemp, J.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause,
R.; Kuempel, D.; Kukec Mezek, G.; Kuotb Awad, A.; Lago, B. L.; LaHurd,
D.; Lang, R. G.; Legumina, R.; Leigui de Oliveira, M. A.; Lenok,
V.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Lo Presti, D.; Lopes,
L.; López, R.; López Casado, A.; Lorek, R.; Luce, Q.; Lucero, A.;
Malacari, M.; Mallamaci, M.; Mancarella, G.; Mandat, D.; Mantsch, P.;
Mariazzi, A. G.; Mariş, I. C.; Marsella, G.; Martello, D.; Martinez,
H.; Martínez Bravo, O.; Mathes, H. J.; Mathys, S.; Matthews, J.;
Matthiae, G.; Mayotte, E.; Mazur, P. O.; Medina-Tanco, G.; Melo,
D.; Menshikov, A.; Merenda, K. -D.; Michal, S.; Micheletti, M. I.;
Middendorf, L.; Miramonti, L.; Mitrica, B.; Mockler, D.; Mollerach,
S.; Montanet, F.; Morello, C.; Morlino, G.; Mostafá, M.; Müller,
A. L.; Muller, M. A.; Müller, S.; Mussa, R.; Nellen, L.; Nguyen,
P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.; Nitz, D.; Nosek, D.;
Novotny, V.; Nožka, L.; Nucita, A.; Núñez, L. A.; Olinto, A.;
Palatka, M.; Pallotta, J.; Papenbreer, P.; Parente, G.; Parra, A.;
Pech, M.; Pedreira, F.; Pȩkala, J.; Pelayo, R.; Peña-Rodriguez,
J.; Pereira, L. A. S.; Perlin, M.; Perrone, L.; Peters, C.; Petrera,
S.; Phuntsok, J.; Pierog, T.; Pimenta, M.; Pirronello, V.; Platino,
M.; Poh, J.; Pont, B.; Porowski, C.; Prado, R. R.; Privitera, P.;
Prouza, M.; Puyleart, A.; Querchfeld, S.; Quinn, S.; Ramos-Pollan,
R.; Rautenberg, J.; Ravignani, D.; Reininghaus, M.; Ridky, J.; Riehn,
F.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.;
Rodriguez Rojo, J.; Roncoroni, M. J.; Roth, M.; Roulet, E.; Rovero,
A. C.; Ruehl, P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar,
H.; Saleh, A.; Salina, G.; Sánchez, F.; Santos, E. M.; Santos, E.;
Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.; Savina, P.;
Schauer, M.; Scherini, V.; Schieler, H.; Schimassek, M.; Schimp,
M.; Schmidt, D.; Scholten, O.; Schovánek, P.; Schröder, F. G.;
Schröder, S.; Schumacher, J.; Sciutto, S. J.; Shellard, R. C.;
Sigl, G.; Silli, G.; Sima, O.; Šmída, R.; Snow, G. R.; Sommers, P.;
Soriano, J. F.; Souchard, J.; Squartini, R.; Stanca, D.; Stanič, S.;
Stasielak, J.; Stassi, P.; Stolpovskiy, M.; Streich, A.; Suarez, F.;
Suárez-Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky, A. D.;
Šupík, J.; Szadkowski, Z.; Taboada, A.; Taborda, O. A.; Tapia, A.;
Timmermans, C.; Todero Peixoto, C. J.; Tomé, B.; Torralba Elipe, G.;
Travnicek, P.; Trini, M.; Tueros, M.; Ulrich, R.; Unger, M.; Urban,
M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.; van Bodegom, P.;
van den Berg, A. M.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.;
Vázquez, R. A.; Veberič, D.; Ventura, C.; Vergara Quispe, I. D.;
Verzi, V.; Vicha, J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.;
Wainberg, O.; Watson, A. A.; Weber, M.; Weindl, A.; Wiedeński, M.;
Wiencke, L.; Wilczyński, H.; Wirtz, M.; Wittkowski, D.; Wundheiler,
B.; Yang, L.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zehrer, L.; Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.;
Zuccarello, F.; Pierre Auger Collaboration
2018ApJ...868....4A Altcode: 2018arXiv180803579T
We present a detailed study of the large-scale anisotropies of
cosmic rays with energies above 4 EeV measured using the Pierre Auger
Observatory. For the energy bins [4, 8] EeV and E ≥ 8 EeV, the most
significant signal is a dipolar modulation in R.A. at energies above 8
EeV, as previously reported. In this paper we further scrutinize the
highest-energy bin by splitting it into three energy ranges. We find
that the amplitude of the dipole increases with energy above 4 EeV. The
growth can be fitted with a power law with index β = 0.79 ± 0.19. The
directions of the dipoles are consistent with an extragalactic origin
of these anisotropies at all the energies considered. Additionally,
we have estimated the quadrupolar components of the anisotropy:
they are not statistically significant. We discuss the results in the
context of the predictions from different models for the distribution
of ultrahigh-energy sources and cosmic magnetic fields.
---------------------------------------------------------
Title: Observation of inclined EeV air showers with the radio detector
of the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albuquerque, I. F. M.;
Albury, J. M.; Allekotte, I.; Almela, A.; Alvarez Castillo, J.;
Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.;
Andringa, S.; Aramo, C.; Arsene, N.; Asorey, H.; Assis, P.; Avila, G.;
Badescu, A. M.; Balaceanu, A.; Barbato, F.; Barreira Luz, R. J.; Baur,
S.; Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou,
X.; Biermann, P. L.; Biteau, J.; Blaess, S. G.; Blanco, A.; Blazek, J.;
Bleve, C.; Boháčová, M.; Bonifazi, C.; Borodai, N.; Botti, A. M.;
Brack, J.; Bretz, T.; Bridgeman, A.; Briechle, F. L.; Buchholz, P.;
Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga,
L.; Calcagni, L.; Cancio, A.; Canfora, F.; Carceller, J. M.; Caruso,
R.; Castellina, A.; Catalani, F.; Cataldi, G.; Cazon, L.; Chinellato,
J. A.; Chudoba, J.; Chytka, L.; Clay, R. W.; Cobos Cerutti, A. C.;
Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição,
R.; Consolati, G.; Contreras, F.; Cooper, M. J.; Coutu, S.; Covault,
C. E.; D'Amico, S.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson,
B. R.; Day, J. A.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza, V.;
Debatin, J.; Deligny, O.; Dhital, N.; Díaz Castro, M. L.; Diogo, F.;
Dobrigkeit, C.; D'Olivo, J. C.; Dorosti, Q.; dos Anjos, R. C.; Dova,
M. T.; Dundovic, A.; Ebr, J.; Engel, R.; Erdmann, M.; Escobar, C. O.;
Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar, G.; Fauth, A. C.;
Fazzini, N.; Feldbusch, F.; Fenu, F.; Ferreyro, L. P.; Fick, B.;
Figueira, J. M.; Filipčič, A.; Freire, M. M.; Fujii, T.; Fuster,
A.; Gaïor, R.; García, B.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia,
P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Głas, D.; Glaser,
C.; Glombitza, J.; Golup, G.; Gómez Berisso, M.; Gómez Vitale,
P. F.; González, N.; Goos, I.; Góra, D.; Gorgi, A.; Gottowik,
M.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Guido, E.; Halliday,
R.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Harvey,
V. M.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Hill, G. C.;
Hojvat, C.; Holt, E. M.; Homola, P.; Hörandel, J. R.; Horvath, P.;
Hrabovský, M.; Huege, T.; Hulsman, J.; Insolia, A.; Isar, P. G.;
Jandt, I.; Johnsen, J. A.; Josebachuili, M.; Jurysek, J.; Kääpä,
A.; Kambeitz, O.; Kampert, K. H.; Keilhauer, B.; Kemmerich, N.; Kemp,
J.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Kuempel,
D.; Kukec Mezek, G.; Kunka, N.; Kuotb Awad, A.; Lago, B. L.; LaHurd,
D.; Lang, R. G.; Legumina, R.; Leigui de Oliveira, M. A.; Lenok,
V.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Lo Presti, D.; Lopes,
L.; López, R.; López Casado, A.; Lorek, R.; Luce, Q.; Lucero, A.;
Malacari, M.; Mallamaci, M.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.;
Mariş, I. C.; Marsella, G.; Martello, D.; Martinez, H.; Martínez
Bravo, O.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthiae, G.;
Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Melo,
D.; Menshikov, A.; Merenda, K. -D.; Michal, S.; Micheletti, M. I.;
Middendorf, L.; Miramonti, L.; Mitrica, B.; Mockler, D.; Mollerach,
S.; Montanet, F.; Morello, C.; Morlino, G.; Mostafá, M.; Müller,
A. L.; Muller, M. A.; Müller, S.; Mussa, R.; Nellen, L.; Nguyen,
P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.; Niemietz, L.; Nitz,
D.; Nosek, D.; Novotny, V.; Nožka, L.; Nucita, A.; Núñez, L. A.;
Oikonomou, F.; Olinto, A.; Palatka, M.; Pallotta, J.; Papenbreer, P.;
Parente, G.; Parra, A.; Paul, T.; Pech, M.; Pedreira, F.; Pȩkala,
J.; Pelayo, R.; Peña-Rodriguez, J.; Pereira, L. A. S.; Perlin,
M.; Perrone, L.; Peters, C.; Petrera, S.; Phuntsok, J.; Pierog,
T.; Pimenta, M.; Pirronello, V.; Platino, M.; Poh, J.; Pont, B.;
Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Puyleart, A.;
Quel, E. J.; Querchfeld, S.; Quinn, S.; Ramos-Pollan, R.; Rautenberg,
J.; Ravignani, D.; Reininghaus, M.; Ridky, J.; Riehn, F.; Risse, M.;
Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Fernandez,
G.; Rodriguez Rojo, J.; Roncoroni, M. J.; Roth, M.; Roulet, E.;
Rovero, A. C.; Ruehl, P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.;
Salazar, H.; Saleh, A.; Salina, G.; Sánchez, F.; Sanchez-Lucas, P.;
Santos, E. M.; Santos, E.; Sarazin, F.; Sarmento, R.; Sarmiento-Cano,
C.; Sato, R.; Savina, P.; Schauer, M.; Scherini, V.; Schieler, H.;
Schimassek, M.; Schimp, M.; Schmidt, D.; Scholten, O.; Schovánek,
P.; Schröder, F. G.; Schröder, S.; Schulz, A.; Schumacher, J.;
Sciutto, S. J.; Segreto, A.; Shellard, R. C.; Sigl, G.; Silli, G.;
Sima, O.; Šmída, R.; Snow, G. R.; Sommers, P.; Soriano, J. F.;
Souchard, J.; Squartini, R.; Stanca, D.; Stanič, S.; Stasielak, J.;
Stassi, P.; Stolpovskiy, M.; Strafella, F.; Streich, A.; Suarez, F.;
Suárez-Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky, A. D.;
Šupík, J.; Swain, J.; Szadkowski, Z.; Taboada, A.; Taborda, O. A.;
Timmermans, C.; Todero Peixoto, C. J.; Tomé, B.; Torralba Elipe, G.;
Travnicek, P.; Trini, M.; Tueros, M.; Ulrich, R.; Unger, M.; Urban,
M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.; van Bodegom, P.;
van den Berg, A. M.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.;
Vázquez, R. A.; Veberič, D.; Ventura, C.; Vergara Quispe, I. D.;
Verzi, V.; Vicha, J.; Villaseñor, L.; Vorobiov, S.; Wahlberg,
H.; Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weindl, A.;
Wiedeński, M.; Wiencke, L.; Wilczyński, H.; Wirtz, M.; Wittkowski,
D.; Wundheiler, B.; Yang, L.; Yushkov, A.; Zas, E.; Zavrtanik, D.;
Zavrtanik, M.; Zehrer, L.; Zepeda, A.; Zimmermann, B.; Ziolkowski,
M.; Zong, Z.; Zuccarello, F.
2018JCAP...10..026A Altcode: 2018arXiv180605386T
With the Auger Engineering Radio Array (AERA) of the Pierre Auger
Observatory, we have observed the radio emission from 561 extensive air
showers with zenith angles between 60<SUP>o</SUP> and 84<SUP>o</SUP>. In
contrast to air showers with more vertical incidence, these inclined
air showers illuminate large ground areas of several km<SUP>2</SUP>
with radio signals detectable in the 30 to 80 MHz band. A comparison
of the measured radio-signal amplitudes with Monte Carlo simulations
of a subset of 50 events for which we reconstruct the energy using
the Auger surface detector shows agreement within the uncertainties
of the current analysis. As expected for forward-beamed radio emission
undergoing no significant absorption or scattering in the atmosphere,
the area illuminated by radio signals grows with the zenith angle
of the air shower. Inclined air showers with EeV energies are thus
measurable with sparse radio-antenna arrays with grid sizes of a km
or more. This is particularly attractive as radio detection provides
direct access to the energy in the electromagnetic cascade of an air
shower, which in case of inclined air showers is not accessible by
arrays of particle detectors on the ground.
---------------------------------------------------------
Title: Threshold of Non-potential Magnetic Helicity Ratios at the
Onset of Solar Eruptions
Authors: Zuccarello, F. P.; Pariat, E.; Valori, G.; Linan, L.
2018ApJ...863...41Z Altcode: 2018arXiv180700532Z
The relative magnetic helicity is a quantity that is often used to
describe the level of entanglement of non-isolated magnetic fields,
such as the magnetic field of solar active regions. The aim of this
paper is to investigate how different kinds of photospheric boundary
flows accumulate relative magnetic helicity in the corona and if and
how well magnetic-helicity-related quantities identify the onset
of an eruption. We use a series of three-dimensional, parametric
magnetohydrodynamic simulations of the formation and eruption of
magnetic flux ropes. All the simulations are performed on the same
grid, using the same parameters, but they are characterized by different
driving photospheric flows, i.e., shearing, convergence, stretching, and
peripheral- and central- dispersion flows. For each of the simulations,
the instant of the onset of the eruption is carefully identified
by using a series of relaxation runs. We find that magnetic energy
and total relative helicity are mostly injected when shearing flows
are applied at the boundary, while the magnetic energy and helicity
associated with the coronal electric currents increase regardless of
the kind of photospheric flows. We also find that, at the onset of
the eruptions, the ratio between the non-potential magnetic helicity
and the total relative magnetic helicity has the same value for all
the simulations, suggesting the existence of a threshold in this
quantity. Such a threshold is not observed for other quantities as,
for example, those related to the magnetic energy.
---------------------------------------------------------
Title: IRIS Observations of Magnetic Interactions in the
Solar Atmosphere between Preexisting and Emerging Magnetic
Fields. I. Overall Evolution
Authors: Guglielmino, Salvo L.; Zuccarello, Francesca; Young, Peter
R.; Murabito, Mariarita; Romano, Paolo
2018ApJ...856..127G Altcode: 2018arXiv180205657G
We report multiwavelength ultraviolet observations taken with the IRIS
satellite, concerning the emergence phase in the upper chromosphere
and transition region of an emerging flux region (EFR) embedded in the
preexisting field of active region NOAA 12529 in the Sun. IRIS data are
complemented by full-disk observations of the Solar Dynamics Observatory
satellite, relevant to the photosphere and the corona. The photospheric
configuration of the EFR is also analyzed by measurements taken with
the spectropolarimeter on board the Hinode satellite, when the EFR was
fully developed. Recurrent intense brightenings that resemble UV bursts,
with counterparts in all coronal passbands, are identified at the edges
of the EFR. Jet activity is also observed at chromospheric and coronal
levels, near the observed brightenings. The analysis of the IRIS line
profiles reveals the heating of dense plasma in the low solar atmosphere
and the driving of bidirectional high-velocity flows with speed up to
100 km s<SUP>-1</SUP> at the same locations. Compared with previous
observations and numerical models, these signatures suggest evidence
of several long-lasting, small-scale magnetic reconnection episodes
between the emerging bipole and the ambient field. This process leads
to the cancellation of a preexisting photospheric flux concentration
and appears to occur higher in the atmosphere than usually found in
UV bursts, explaining the observed coronal counterparts.
---------------------------------------------------------
Title: Formation of Penumbra in a Sample of Active Regions Observed
by the SDO Satellite
Authors: Murabito, Mariarita; Zuccarello, Francesca; Guglielmino,
Salvo L.; Romano, Paolo
2018ApJ...855...58M Altcode:
Recently, high-resolution observations improved our understanding of
the penumbra formation process around sunspots. In particular, two
aspects have been carefully investigated: whether the settlement of
the penumbra can occur between the main opposite magnetic polarities
where new magnetic flux is still emerging, and the establishment
of the Evershed flow. In this paper, we present the analysis of
twelve active regions (ARs) where both the penumbra formation and
the onset of the Evershed flow were observed. We used data acquired
by the Helioseismic and Magnetic Imager (HMI) instrument on board
the Solar Dynamic Observatory (SDO) satellite analyzing continuum
images, magnetograms, and Dopplergrams of the selected ARs. The
results obtained in our sample provided the following information
about the stable settlement of the penumbra: eight spots formed the
first stable penumbral sector in the region between the two opposite
polarities, and nine spots formed on the opposite side. Moreover,
eleven sunpots showed an inverse Evershed flow (i.e., a plasma motion
directed toward the protospot border) before the penumbra formation,
which changes within 1-6 hr into the classical Evershed flow as soon
as the penumbra forms. Comparing our results with recent observations,
we are able to discriminate between the different ways of penumbra
formation. Moreover, we suggest that the change from inverse Evershed
flow, visible before the penumbra appears, into the classical Evershed
flow may be a signature of the formation of penumbral filaments.
---------------------------------------------------------
Title: Long-term optical monitoring of the solar atmosphere in Italy
Authors: Guglielmino, S. L.; Ermolli, I.; Romano, P.; Zuccarello,
F.; Giorgi, F.; Falco, M.; Piazzesi, R.; Stangalini, M.; Murabito,
M.; Ferrucci, M.; Mangano, A.
2018IAUS..340..251G Altcode: 2019arXiv190101050G
Probably, the long-term monitoring of the solar atmosphere started
in Italy with the first telescopic observations of the Sun made by
Galileo Galilei in the early 17<SUP>th</SUP> century. His recorded
observations and science results, as well as the work carried out by
other following outstanding Italian astronomers inspired the start of
institutional programs of regular solar observations at the Arcetri,
Catania, and Rome Observatories. <P />These programs have accumulated
daily images of the solar photosphere and chromosphere taken at various
spectral bands over a time span larger than 80 years. In the last
two decades, regular solar observations were continued with digital
cameras only at the Catania and Rome Observatories, which are now part
of the INAF National Institute for Astrophysics. At the two sites,
daily solar images are taken at the photospheric G-band, Blue (λ =
409.4 nm), and Red (λ = 606.9 nm) continua spectral ranges and at the
chromospheric Ca II K and Hα lines, with a 2” spatial resolution. <P
/>Solar observation in Italy, which benefits from over 2500 hours
of yearly sunshine, currently aims at the operational monitoring of
solar activity and long-term variability and at the continuation of the
historical series as well. Existing instruments will be soon enriched
by the SAMM double channel telescope equipped with magneto-optical
filters that will enable the tomography of the solar atmosphere with
simultaneous observations at the K I 769.9 nm and Na I D 589.0 nm
lines. In this contribution, we present the available observations
and outline their scientific relevance.
---------------------------------------------------------
Title: An Indication of Anisotropy in Arrival Directions of
Ultra-high-energy Cosmic Rays through Comparison to the Flux Pattern
of Extragalactic Gamma-Ray Sources
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Albuquerque, I. F. M.;
Allekotte, I.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muñiz,
J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.; Andringa, S.;
Aramo, C.; Arsene, N.; Asorey, H.; Assis, P.; Avila, G.; Badescu,
A. M.; Balaceanu, A.; Barbato, F.; Barreira Luz, R. J.; Beatty, J. J.;
Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.;
Biermann, P. L.; Biteau, J.; Blaess, S. G.; Blanco, A.; Blazek, J.;
Bleve, C.; Boháčová, M.; Bonifazi, C.; Borodai, N.; Botti, A. M.;
Brack, J.; Brancus, I.; Bretz, T.; Bridgeman, A.; Briechle, F. L.;
Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora,
K. S.; Caccianiga, L.; Cancio, A.; Canfora, F.; Caruso, R.; Castellina,
A.; Catalani, F.; Cataldi, G.; Cazon, L.; Chavez, A. G.; Chinellato,
J. A.; Chudoba, J.; Clay, R. W.; Cobos Cerutti, A. C.; Colalillo, R.;
Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição, R.; Consolati,
G.; Contreras, F.; Cooper, M. J.; Coutu, S.; Covault, C. E.; Cronin,
J.; D'Amico, S.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.;
de Almeida, R. M.; de Jong, S. J.; De Mauro, G.; de Mello Neto,
J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza, V.; Debatin, J.;
Deligny, O.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo,
J. C.; Dorosti, Q.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr,
J.; Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal,
J.; Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar, G.; Fauth,
A. C.; Fazzini, N.; Fenu, F.; Fick, B.; Figueira, J. M.; Filipčič,
A.; Freire, M. M.; Fujii, T.; Fuster, A.; Gaïor, R.; García, B.;
Gaté, F.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.;
Giammarchi, M.; Giller, M.; Głas, D.; Glaser, C.; Golup, G.; Gómez
Berisso, M.; Gómez Vitale, P. F.; González, N.; Gorgi, A.; Grillo,
A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Halliday, R.; Hampel,
M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Haungs, A.; Hebbeker,
T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Holt,
E.; Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege,
T.; Hulsman, J.; Insolia, A.; Isar, P. G.; Jandt, I.; Johnsen, J. A.;
Josebachuili, M.; Jurysek, J.; Kääpä, A.; Kambeitz, O.; Kampert,
K. H.; Keilhauer, B.; Kemmerich, N.; Kemp, E.; Kemp, J.; Kieckhafer,
R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.;
Krohm, N.; Kuempel, D.; Kukec Mezek, G.; Kunka, N.; Kuotb Awad,
A.; Lago, B. L.; LaHurd, D.; Lang, R. G.; Lauscher, M.; Legumina,
R.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon,
I.; Link, K.; Lo Presti, D.; Lopes, L.; López, R.; López Casado,
A.; Lorek, R.; Luce, Q.; Lucero, A.; Malacari, M.; Mallamaci, M.;
Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Mariş, I. C.; Marsella,
G.; Martello, D.; Martinez, H.; Martínez Bravo, O.; Masías Meza,
J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthiae, G.; Mayotte,
E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Melo, D.; Menshikov,
A.; Merenda, K. -D.; Michal, S.; Micheletti, M. I.; Middendorf, L.;
Miramonti, L.; Mitrica, B.; Mockler, D.; Mollerach, S.; Montanet,
F.; Morello, C.; Morlino, G.; Mostafá, M.; Müller, A. L.; Müller,
G.; Muller, M. A.; Müller, S.; Mussa, R.; Naranjo, I.; Nellen, L.;
Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.; Niemietz,
L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.;
Núñez, L. A.; Oikonomou, F.; Olinto, A.; Palatka, M.; Pallotta,
J.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.; Pech, M.;
Pedreira, F.; Pȩkala, J.; Pelayo, R.; Peña-Rodriguez, J.; Pereira,
L. A. S.; Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.; Phuntsok,
J.; Pierog, T.; Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.;
Poh, J.; Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Quel,
E. J.; Querchfeld, S.; Quinn, S.; Ramos-Pollan, R.; Rautenberg, J.;
Ravignani, D.; Ridky, J.; Riehn, F.; Risse, M.; Ristori, P.; Rizi, V.;
Rodrigues de Carvalho, W.; Rodriguez Fernandez, G.; Rodriguez Rojo,
J.; Roncoroni, M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl,
P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.;
Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santos, E. M.; Santos,
E.; Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.; Schauer,
M.; Scherini, V.; Schieler, H.; Schimp, M.; Schmidt, D.; Scholten,
O.; Schovánek, P.; Schröder, F. G.; Schröder, S.; Schulz, A.;
Schumacher, J.; Sciutto, S. J.; Segreto, A.; Shadkam, A.; Shellard,
R. C.; Sigl, G.; Silli, G.; Šmída, R.; Snow, G. R.; Sommers, P.;
Sonntag, S.; Soriano, J. F.; Squartini, R.; Stanca, D.; Stanič, S.;
Stasielak, J.; Stassi, P.; Stolpovskiy, M.; Strafella, F.; Streich,
A.; Suarez, F.; Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.;
Supanitsky, A. D.; Šupík, J.; Swain, J.; Szadkowski, Z.; Taboada,
A.; Taborda, O. A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Tomankova, L.; Tomé, B.; Torralba Elipe, G.; Travnicek, P.;
Trini, M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.;
Valiño, I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg,
A. M.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Vázquez,
R. A.; Veberič, D.; Ventura, C.; Vergara Quispe, I. D.; Verzi, V.;
Vicha, J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.; Wainberg,
O.; Walz, D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiedeński, M.;
Wiencke, L.; Wilczyński, H.; Wirtz, M.; Wittkowski, D.; Wundheiler,
B.; Yang, L.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello,
F.; Pierre Auger Collaboration
2018ApJ...853L..29A Altcode: 2018arXiv180106160T
A new analysis of the data set from the Pierre Auger Observatory
provides evidence for anisotropy in the arrival directions of
ultra-high-energy cosmic rays on an intermediate angular scale, which
is indicative of excess arrivals from strong, nearby sources. The
data consist of 5514 events above 20 {EeV} with zenith angles up to
80° recorded before 2017 April 30. Sky models have been created for
two distinct populations of extragalactic gamma-ray emitters: active
galactic nuclei from the second catalog of hard Fermi-LAT sources
(2FHL) and starburst galaxies from a sample that was examined with
Fermi-LAT. Flux-limited samples, which include all types of galaxies
from the Swift-BAT and 2MASS surveys, have been investigated for
comparison. The sky model of cosmic-ray density constructed using each
catalog has two free parameters, the fraction of events correlating
with astrophysical objects, and an angular scale characterizing
the clustering of cosmic rays around extragalactic sources. A
maximum-likelihood ratio test is used to evaluate the best values of
these parameters and to quantify the strength of each model by contrast
with isotropy. It is found that the starburst model fits the data better
than the hypothesis of isotropy with a statistical significance of
4.0σ, the highest value of the test statistic being for energies above
39 {EeV}. The three alternative models are favored against isotropy
with 2.7σ-3.2σ significance. The origin of the indicated deviation
from isotropy is examined and prospects for more sensitive future
studies are discussed. <P />Any correspondence should be addressed to .
---------------------------------------------------------
Title: Hα and Hβ emission in a C3.3 solar flare: comparison between
observations and simulations
Authors: Zuccarello, F.; Simoes, P. J. D. A.; Capparelli, V.; Fletcher,
L.; Romano, P.; Mathioudakis, M.; Cauzzi, G.; Carlsson, M.; Kuridze,
D.; Keys, P.
2017AGUFMSH41A2742Z Altcode:
This work is based on the analysis of an extremely rare set of
simultaneous observations of a C3.3 solar flare in the Hα and Hβ lines
at high spatial and temporal resolution, which were acquired at the
Dunn Solar Telescope. Images of the C3.3 flare (SOL2014-04-22T15:22)
made at various wavelengths along the Hα line profile by the
Interferometric Bidimensional Spectrometer (IBIS) and in the Hβ
with the Rapid Oscillations in the Solar Atmosphere (ROSA) broadband
imager are analyzed to obtain the intensity evolution. The analysis
shows that Hα and Hβ intensity excesses in three identified flare
footpoints are well correlated in time. In the stronger footpoints,
the typical value of the the Hα/Hβ intensity ratio observed is ∼
0.4 - 0.5, in broad agreement with values obtained from a RADYN non-LTE
simulation driven by an electron beam with parameters constrained by
observations. The weaker footpoint has a larger Hα/Hβ ratio, again
consistent with a RADYN simulation but with a smaller energy flux.
---------------------------------------------------------
Title: Search for High-energy Neutrinos from Binary Neutron
Star Merger GW170817 with ANTARES, IceCube, and the Pierre Auger
Observatory
Authors: Albert, A.; André, M.; Anghinolfi, M.; Ardid, M.; Aubert,
J. -J.; Aublin, J.; Avgitas, T.; Baret, B.; Barrios-Martí, J.; Basa,
S.; Belhorma, B.; Bertin, V.; Biagi, S.; Bormuth, R.; Bourret, S.;
Bouwhuis, M. C.; Brânzaş, H.; Bruijn, R.; Brunner, J.; Busto, J.;
Capone, A.; Caramete, L.; Carr, J.; Celli, S.; Cherkaoui El Moursli,
R.; Chiarusi, T.; Circella, M.; Coelho, J. A. B.; Coleiro, A.;
Coniglione, R.; Costantini, H.; Coyle, P.; Creusot, A.; Díaz, A. F.;
Deschamps, A.; De Bonis, G.; Distefano, C.; Di Palma, I.; Domi, A.;
Donzaud, C.; Dornic, D.; Drouhin, D.; Eberl, T.; El Bojaddaini, I.; El
Khayati, N.; Elsässer, D.; Enzenhöfer, A.; Ettahiri, A.; Fassi, F.;
Felis, I.; Fusco, L. A.; Gay, P.; Giordano, V.; Glotin, H.; Grégoire,
T.; Ruiz, R. Gracia; Graf, K.; Hallmann, S.; van Haren, H.; Heijboer,
A. J.; Hello, Y.; Hernández-Rey, J. J.; Hößl, J.; Hofestädt,
J.; Illuminati, G.; James, C. W.; de Jong, M.; Jongen, M.; Kadler,
M.; Kalekin, O.; Katz, U.; Kießling, D.; Kouchner, A.; Kreter, M.;
Kreykenbohm, I.; Kulikovskiy, V.; Lachaud, C.; Lahmann, R.; Lefèvre,
D.; Leonora, E.; Lotze, M.; Loucatos, S.; Marcelin, M.; Margiotta, A.;
Marinelli, A.; Martínez-Mora, J. A.; Mele, R.; Melis, K.; Michael,
T.; Migliozzi, P.; Moussa, A.; Navas, S.; Nezri, E.; Organokov, M.;
Păvălaş, G. E.; Pellegrino, C.; Perrina, C.; Piattelli, P.; Popa,
V.; Pradier, T.; Quinn, L.; Racca, C.; Riccobene, G.; Sánchez-Losa,
A.; Saldaña, M.; Salvadori, I.; Samtleben, D. F. E.; Sanguineti, M.;
Sapienza, P.; Schüssler, F.; Sieger, C.; Spurio, M.; Stolarczyk,
Th.; Taiuti, M.; Tayalati, Y.; Trovato, A.; Turpin, D.; Tönnis,
C.; Vallage, B.; Van Elewyck, V.; Versari, F.; Vivolo, D.; Vizzoca,
A.; Wilms, J.; Zornoza, J. D.; Zúñiga, J.; ANTARES Collaboration;
Aartsen, M. G.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.;
Ahrens, M.; Samarai, I. Al; Altmann, D.; Andeen, K.; Anderson, T.;
Ansseau, I.; Anton, G.; Argüelles, C.; Auffenberg, J.; Axani, S.;
Bagherpour, H.; Bai, X.; Barron, J. P.; Barwick, S. W.; Baum, V.; Bay,
R.; Beatty, J. J.; Becker Tjus, J.; Becker, K. -H.; BenZvi, S.; Berley,
D.; Bernardini, E.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss,
E.; Blot, S.; Bohm, C.; Börner, M.; Bos, F.; Bose, D.; Böser, S.;
Botner, O.; Bourbeau, E.; Bourbeau, J.; Bradascio, F.; Braun, J.;
Brayeur, L.; Brenzke, M.; Bretz, H. -P.; Bron, S.; Brostean-Kaiser,
J.; Burgman, A.; Carver, T.; Casey, J.; Casier, M.; Cheung, E.;
Chirkin, D.; Christov, A.; Clark, K.; Classen, L.; Coenders, S.;
Collin, G. H.; Conrad, J. M.; Cowen, D. F.; Cross, R.; Day, M.;
de André, J. P. A. M.; De Clercq, C.; DeLaunay, J. J.; Dembinski,
H.; De Ridder, S.; Desiati, P.; de Vries, K. D.; de Wasseige, G.;
de With, M.; DeYoung, T.; Díaz-Vélez, J. C.; di Lorenzo, V.;
Dujmovic, H.; Dumm, J. P.; Dunkman, M.; Dvorak, E.; Eberhardt,
B.; Ehrhardt, T.; Eichmann, B.; Eller, P.; Evenson, P. A.; Fahey,
S.; Fazely, A. R.; Felde, J.; Filimonov, K.; Finley, C.; Flis, S.;
Franckowiak, A.; Friedman, E.; Fuchs, T.; Gaisser, T. K.; Gallagher,
J.; Gerhardt, L.; Ghorbani, K.; Giang, W.; Glauch, T.; Glüsenkamp,
T.; Goldschmidt, A.; Gonzalez, J. G.; Grant, D.; Griffith, Z.; Haack,
C.; Hallgren, A.; Halzen, F.; Hanson, K.; Hebecker, D.; Heereman, D.;
Helbing, K.; Hellauer, R.; Hickford, S.; Hignight, J.; Hill, G. C.;
Hoffman, K. D.; Hoffmann, R.; Hokanson-Fasig, B.; Hoshina, K.; Huang,
F.; Huber, M.; Hultqvist, K.; Hünnefeld, M.; In, S.; Ishihara, A.;
Jacobi, E.; Japaridze, G. S.; Jeong, M.; Jero, K.; Jones, B. J. P.;
Kalaczynski, P.; Kang, W.; Kappes, A.; Karg, T.; Karle, A.; Katz, U.;
Kauer, M.; Keivani, A.; Kelley, J. L.; Kheirandish, A.; Kim, J.; Kim,
M.; Kintscher, T.; Kiryluk, J.; Kittler, T.; Klein, S. R.; Kohnen,
G.; Koirala, R.; Kolanoski, H.; Köpke, L.; Kopper, C.; Kopper, S.;
Koschinsky, J. P.; Koskinen, D. J.; Kowalski, M.; Krings, K.; Kroll,
M.; Krückl, G.; Kunnen, J.; Kunwar, S.; Kurahashi, N.; Kuwabara, T.;
Kyriacou, A.; Labare, M.; Lanfranchi, J. L.; Larson, M. J.; Lauber,
F.; Lesiak-Bzdak, M.; Leuermann, M.; Liu, Q. R.; Lu, L.; Lünemann,
J.; Luszczak, W.; Madsen, J.; Maggi, G.; Mahn, K. B. M.; Mancina,
S.; Maruyama, R.; Mase, K.; Maunu, R.; McNally, F.; Meagher, K.;
Medici, M.; Meier, M.; Menne, T.; Merino, G.; Meures, T.; Miarecki,
S.; Micallef, J.; Momenté, G.; Montaruli, T.; Moore, R. W.; Moulai,
M.; Nahnhauer, R.; Nakarmi, P.; Naumann, U.; Neer, G.; Niederhausen,
H.; Nowicki, S. C.; Nygren, D. R.; Obertacke Pollmann, A.; Olivas,
A.; O'Murchadha, A.; Palczewski, T.; Pandya, H.; Pankova, D. V.;
Peiffer, P.; Pepper, J. A.; Pérez de los Heros, C.; Pieloth, D.;
Pinat, E.; Plum, M.; Pranav, D.; Price, P. B.; Przybylski, G. T.;
Raab, C.; Rädel, L.; Rameez, M.; Rawlins, K.; Rea, I. C.; Reimann,
R.; Relethford, B.; Relich, M.; Resconi, E.; Rhode, W.; Richman, M.;
Robertson, S.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk,
D.; Sälzer, T.; Sanchez Herrera, S. E.; Sandrock, A.; Sandroos, J.;
Santander, M.; Sarkar, S.; Sarkar, S.; Satalecka, K.; Schlunder, P.;
Schmidt, T.; Schneider, A.; Schoenen, S.; Schöneberg, S.; Schumacher,
L.; Seckel, D.; Seunarine, S.; Soedingrekso, J.; Soldin, D.; Song,
M.; Spiczak, G. M.; Spiering, C.; Stachurska, J.; Stamatikos, M.;
Stanev, T.; Stasik, A.; Stettner, J.; Steuer, A.; Stezelberger,
T.; Stokstad, R. G.; Stößl, A.; Strotjohann, N. L.; Stuttard, T.;
Sullivan, G. W.; Sutherland, M.; Taboada, I.; Tatar, J.; Tenholt,
F.; Ter-Antonyan, S.; Terliuk, A.; Tešić, G.; Tilav, S.; Toale,
P. A.; Tobin, M. N.; Toscano, S.; Tosi, D.; Tselengidou, M.; Tung,
C. F.; Turcati, A.; Turley, C. F.; Ty, B.; Unger, E.; Usner, M.;
Vandenbroucke, J.; Van Driessche, W.; van Eijndhoven, N.; Vanheule,
S.; van Santen, J.; Vehring, M.; Vogel, E.; Vraeghe, M.; Walck, C.;
Wallace, A.; Wallraff, M.; Wandler, F. D.; Wandkowsky, N.; Waza, A.;
Weaver, C.; Weiss, M. J.; Wendt, C.; Werthebach, J.; Westerhoff, S.;
Whelan, B. J.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams, D. R.;
Wills, L.; Wolf, M.; Wood, J.; Wood, T. R.; Woolsey, E.; Woschnagg,
K.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yanez, J. P.; Yodh, G.; Yoshida,
S.; Yuan, T.; Zoll, M.; IceCube Collaboration; Aab, A.; Abreu, P.;
Aglietta, M.; Albuquerque, I. F. M.; Albury, J. M.; Allekotte, I.;
Almela, A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Anastasi, G. A.;
Anchordoqui, L.; Andrada, B.; Andringa, S.; Aramo, C.; Arsene, N.;
Asorey, H.; Assis, P.; Avila, G.; Badescu, A. M.; Balaceanu, A.;
Barbato, F.; Barreira Luz, R. J.; Beatty, J. J.; Becker, K. H.;
Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann,
P. L.; Biteau, J.; Blaess, S. G.; Blanco, A.; Blazek, J.; Bleve, C.;
Boháčová, M.; Bonifazi, C.; Borodai, N.; Botti, A. M.; Brack, J.;
Brancus, I.; Bretz, T.; Bridgeman, A.; Briechle, F. L.; Buchholz, P.;
Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga,
L.; Cancio, A.; Canfora, F.; Caruso, R.; Castellina, A.; Catalani, F.;
Cataldi, G.; Cazon, L.; Chavez, A. G.; Chinellato, J. A.; Chudoba, J.;
Clay, R. W.; Cobos Cerutti, A. C.; Colalillo, R.; Coleman, A.; Collica,
L.; Coluccia, M. R.; Conceição, R.; Consolati, G.; Contreras, F.;
Cooper, M. J.; Coutu, S.; Covault, C. E.; Cronin, J.; D'Amico, S.;
Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; Day, J. A.; de
Almeida, R. M.; de Jong, S. J.; De Mauro, G.; de Mello Neto, J. R. T.;
De Mitri, I.; de Oliveira, J.; de Souza, V.; Debatin, J.; Deligny,
O.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.;
Dorosti, Q.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.;
Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.;
Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar, G.; Fauth, A. C.;
Fazzini, N.; Feldbusch, F.; Fenu, F.; Fick, B.; Figueira, J. M.;
Filipčič, A.; Freire, M. M.; Fujii, T.; Fuster, A.; Gaïor, R.;
García, B.; Gaté, F.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.;
Giaccari, U.; Giammarchi, M.; Giller, M.; Głas, D.; Glaser, C.; Golup,
G.; Gómez Berisso, M.; Gómez Vitale, P. F.; González, N.; Gorgi,
A.; Gottowik, M.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes,
G. P.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison,
T. A.; Harvey, V. M.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.;
Herve, A. E.; Hill, G. C.; Hojvat, C.; Holt, E.; Homola, P.; Hörandel,
J. R.; Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman, J.; Insolia,
A.; Isar, P. G.; Jandt, I.; Johnsen, J. A.; Josebachuili, M.; Jurysek,
J.; Kääpä, A.; Kampert, K. H.; Keilhauer, B.; Kemmerich, N.; Kemp,
J.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.;
Krause, R.; Krohm, N.; Kuempel, D.; Kukec Mezek, G.; Kunka, N.; Kuotb
Awad, A.; Lago, B. L.; LaHurd, D.; Lang, R. G.; Lauscher, M.; Legumina,
R.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon,
I.; Link, K.; Lo Presti, D.; Lopes, L.; López, R.; López Casado,
A.; Lorek, R.; Luce, Q.; Lucero, A.; Malacari, M.; Mallamaci, M.;
Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Mariş, I. C.; Marsella,
G.; Martello, D.; Martinez, H.; Martínez Bravo, O.; Masías Meza,
J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthiae, G.; Mayotte,
E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Melo, D.; Menshikov,
A.; Merenda, K. -D.; Michal, S.; Micheletti, M. I.; Middendorf, L.;
Miramonti, L.; Mitrica, B.; Mockler, D.; Mollerach, S.; Montanet,
F.; Morello, C.; Morlino, G.; Mostafá, M.; Müller, A. L.; Müller,
G.; Muller, M. A.; Müller, S.; Mussa, R.; Naranjo, I.; Nellen, L.;
Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.; Niemietz,
L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.;
Núñez, L. A.; Oikonomou, F.; Olinto, A.; Palatka, M.; Pallotta,
J.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.; Pech, M.;
Pedreira, F.; Pȩkala, J.; Pelayo, R.; Peña-Rodriguez, J.; Pereira,
L. A. S.; Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.; Phuntsok,
J.; Pierog, T.; Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.;
Poh, J.; Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Quel,
E. J.; Querchfeld, S.; Quinn, S.; Ramos-Pollan, R.; Rautenberg, J.;
Ravignani, D.; Ridky, J.; Riehn, F.; Risse, M.; Ristori, P.; Rizi, V.;
Rodrigues de Carvalho, W.; Rodriguez Fernandez, G.; Rodriguez Rojo,
J.; Roncoroni, M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl,
P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.;
Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santos, E. M.; Santos,
E.; Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.; Schauer,
M.; Scherini, V.; Schieler, H.; Schimp, M.; Schmidt, D.; Scholten,
O.; Schovánek, P.; Schröder, F. G.; Schröder, S.; Schulz, A.;
Schumacher, J.; Sciutto, S. J.; Segreto, A.; Shadkam, A.; Shellard,
R. C.; Sigl, G.; Silli, G.; Šmída, R.; Snow, G. R.; Sommers, P.;
Sonntag, S.; Soriano, J. F.; Squartini, R.; Stanca, D.; Stanič, S.;
Stasielak, J.; Stassi, P.; Stolpovskiy, M.; Strafella, F.; Streich,
A.; Suarez, F.; Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.;
Supanitsky, A. D.; Šupík, J.; Swain, J.; Szadkowski, Z.; Taboada,
A.; Taborda, O. A.; Timmermans, C.; Todero Peixoto, C. J.; Tomankova,
L.; Tomé, B.; Torralba Elipe, G.; Travnicek, P.; Trini, M.; Tueros,
M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño,
I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.;
van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Vázquez, R. A.;
Veberič, D.; Ventura, C.; Vergara Quispe, I. D.; Verzi, V.; Vicha,
J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz,
D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiedeński, M.; Wiencke,
L.; Wilczyński, H.; Wirtz, M.; Wittkowski, D.; Wundheiler, B.; Yang,
L.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zepeda, A.;
Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello, F.; Pierre Auger
Collaboration; Abbott, B. P.; Abbott, R.; Abbott, T. D.; Acernese,
F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.;
Adya, V. B.; Affeldt, C.; Afrough, M.; Agarwal, B.; Agathos, M.;
Agatsuma, K.; Aggarwal, N.; Aguiar, O. D.; Aiello, L.; Ain, A.;
Ajith, P.; Allen, B.; Allen, G.; Allocca, A.; Altin, P. A.; Amato,
A.; Ananyeva, A.; Anderson, S. B.; Anderson, W. G.; Angelova, S. V.;
Antier, S.; Appert, S.; Arai, K.; Araya, M. C.; Areeda, J. S.; Arnaud,
N.; Arun, K. G.; Ascenzi, S.; Ashton, G.; Ast, M.; Aston, S. M.;
Astone, P.; Atallah, D. V.; Aufmuth, P.; Aulbert, C.; AultONeal, K.;
Austin, C.; Avila-Alvarez, A.; Babak, S.; Bacon, P.; Bader, M. K. M.;
Bae, S.; Baker, P. T.; Baldaccini, F.; Ballardin, G.; Ballmer, S. W.;
Banagiri, S.; Barayoga, J. C.; Barclay, S. E.; Barish, B. C.; Barker,
D.; Barkett, K.; Barone, F.; Barr, B.; Barsotti, L.; Barsuglia, M.;
Barta, D.; Bartlett, J.; Bartos, I.; Bassiri, R.; Basti, A.; Batch,
J. C.; Bawaj, M.; Bayley, J. C.; Bazzan, M.; Bécsy, B.; Beer, C.;
Bejger, M.; Belahcene, I.; Bell, A. S.; Berger, B. K.; Bergmann,
G.; Bero, J. J.; Berry, C. P. L.; Bersanetti, D.; Bertolini, A.;
Betzwieser, J.; Bhagwat, S.; Bhandare, R.; Bilenko, I. A.; Billingsley,
G.; Billman, C. R.; Birch, J.; Birney, R.; Birnholtz, O.; Biscans, S.;
Biscoveanu, S.; Bisht, A.; Bitossi, M.; Biwer, C.; Bizouard, M. A.;
Blackburn, J. K.; Blackman, J.; Blair, C. D.; Blair, D. G.; Blair,
R. M.; Bloemen, S.; Bock, O.; Bode, N.; Boer, M.; Bogaert, G.; Bohe,
A.; Bondu, F.; Bonilla, E.; Bonnand, R.; Boom, B. A.; Bork, R.; Boschi,
V.; Bose, S.; Bossie, K.; Bouffanais, Y.; Bozzi, A.; Bradaschia, C.;
Brady, P. R.; Branchesi, M.; Brau, J. E.; Briant, T.; Brillet, A.;
Brinkmann, M.; Brisson, V.; Brockill, P.; Broida, J. E.; Brooks,
A. F.; Brown, D. A.; Brown, D. D.; Brunett, S.; Buchanan, C. C.;
Buikema, A.; Bulik, T.; Bulten, H. J.; Buonanno, A.; Buskulic,
D.; Buy, C.; Byer, R. L.; Cabero, M.; Cadonati, L.; Cagnoli, G.;
Cahillane, C.; Calderón Bustillo, J.; Callister, T. A.; Calloni, E.;
Camp, J. B.; Canepa, M.; Canizares, P.; Cannon, K. C.; Cao, H.; Cao,
J.; Capano, C. D.; Capocasa, E.; Carbognani, F.; Caride, S.; Carney,
M. F.; Casanueva Diaz, J.; Casentini, C.; Caudill, S.; Cavaglià, M.;
Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C. B.; Cerdá-Durán,
P.; Cerretani, G.; Cesarini, E.; Chamberlin, S. J.; Chan, M.; Chao,
S.; Charlton, P.; Chase, E.; Chassande-Mottin, E.; Chatterjee, D.;
Cheeseboro, B. D.; Chen, H. Y.; Chen, X.; Chen, Y.; Cheng, H. -P.;
Chia, H.; Chincarini, A.; Chiummo, A.; Chmiel, T.; Cho, H. S.; Cho, M.;
Chow, J. H.; Christensen, N.; Chu, Q.; Chua, A. J. K.; Chua, S.; Chung,
A. K. W.; Chung, S.; Ciani, G.; Ciolfi, R.; Cirelli, C. E.; Cirone,
A.; Clara, F.; Clark, J. A.; Clearwater, P.; Cleva, F.; Cocchieri,
C.; Coccia, E.; Cohadon, P. -F.; Cohen, D.; Colla, A.; Collette,
C. G.; Cominsky, L. R.; Constancio, M., Jr.; Conti, L.; Cooper,
S. J.; Corban, P.; Corbitt, T. R.; Cordero-Carrión, I.; Corley,
K. R.; Cornish, N.; Corsi, A.; Cortese, S.; Costa, C. A.; Coughlin,
M. W.; Coughlin, S. B.; Coulon, J. -P.; Countryman, S. T.; Couvares,
P.; Covas, P. B.; Cowan, E. E.; Coward, D. M.; Cowart, M. J.; Coyne,
D. C.; Coyne, R.; Creighton, J. D. E.; Creighton, T. D.; Cripe, J.;
Crowder, S. G.; Cullen, T. J.; Cumming, A.; Cunningham, L.; Cuoco, E.;
Dal Canton, T.; Dálya, G.; Danilishin, S. L.; D'Antonio, S.; Danzmann,
K.; Dasgupta, A.; Da Silva Costa, C. F.; Dattilo, V.; Dave, I.; Davier,
M.; Davis, D.; Daw, E. J.; Day, B.; De, S.; DeBra, D.; Degallaix, J.;
De Laurentis, M.; Deléglise, S.; Del Pozzo, W.; Demos, N.; Denker, T.;
Dent, T.; De Pietri, R.; Dergachev, V.; De Rosa, R.; DeRosa, R. T.;
De Rossi, C.; DeSalvo, R.; de Varona, O.; Devenson, J.; Dhurandhar,
S.; Díaz, M. C.; Di Fiore, L.; Di Giovanni, M.; Di Girolamo, T.;
Di Lieto, A.; Di Pace, S.; Di Palma, I.; Di Renzo, F.; Doctor, Z.;
Dolique, V.; Donovan, F.; Dooley, K. L.; Doravari, S.; Dorrington,
I.; Douglas, R.; Dovale Álvarez, M.; Downes, T. P.; Drago, M.;
Dreissigacker, C.; Driggers, J. C.; Du, Z.; Ducrot, M.; Dupej, P.;
Dwyer, S. E.; Edo, T. B.; Edwards, M. C.; Effler, A.; Eggenstein,
H. -B.; Ehrens, P.; Eichholz, J.; Eikenberry, S. S.; Eisenstein,
R. A.; Essick, R. C.; Estevez, D.; Etienne, Z. B.; Etzel, T.; Evans,
M.; Evans, T. M.; Factourovich, M.; Fafone, V.; Fair, H.; Fairhurst,
S.; Fan, X.; Farinon, S.; Farr, B.; Farr, W. M.; Fauchon-Jones, E. J.;
Favata, M.; Fays, M.; Fee, C.; Fehrmann, H.; Feicht, J.; Fejer, M. M.;
Fernandez-Galiana, A.; Ferrante, I.; Ferreira, E. C.; Ferrini, F.;
Fidecaro, F.; Finstad, D.; Fiori, I.; Fiorucci, D.; Fishbach, M.;
Fisher, R. P.; Fitz-Axen, M.; Flaminio, R.; Fletcher, M.; Fong, H.;
Font, J. A.; Forsyth, P. W. F.; Forsyth, S. S.; Fournier, J. -D.;
Frasca, S.; Frasconi, F.; Frei, Z.; Freise, A.; Frey, R.; Frey, V.;
Fries, E. M.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.;
Gabbard, H.; Gadre, B. U.; Gaebel, S. M.; Gair, J. R.; Gammaitoni, L.;
Ganija, M. R.; Gaonkar, S. G.; Garcia-Quiros, C.; Garufi, F.; Gateley,
B.; Gaudio, S.; Gaur, G.; Gayathri, V.; Gehrels, N.; Gemme, G.;
Genin, E.; Gennai, A.; George, D.; George, J.; Gergely, L.; Germain,
V.; Ghonge, S.; Ghosh, Abhirup; Ghosh, Archisman; Ghosh, S.; Giaime,
J. A.; Giardina, K. D.; Giazotto, A.; Gill, K.; Glover, L.; Goetz, E.;
Goetz, R.; Gomes, S.; Goncharov, B.; González, G.; Gonzalez Castro,
J. M.; Gopakumar, A.; Gorodetsky, M. L.; Gossan, S. E.; Gosselin,
M.; Gouaty, R.; Grado, A.; Graef, C.; Granata, M.; Grant, A.; Gras,
S.; Gray, C.; Greco, G.; Green, A. C.; Gretarsson, E. M.; Groot, P.;
Grote, H.; Grunewald, S.; Gruning, P.; Guidi, G. M.; Guo, X.; Gupta,
A.; Gupta, M. K.; Gushwa, K. E.; Gustafson, E. K.; Gustafson, R.;
Halim, O.; Hall, B. R.; Hall, E. D.; Hamilton, E. Z.; Hammond, G.;
Haney, M.; Hanke, M. M.; Hanks, J.; Hanna, C.; Hannam, M. D.;
Hannuksela, O. A.; Hanson, J.; Hardwick, T.; Harms, J.; Harry, G. M.;
Harry, I. W.; Hart, M. J.; Haster, C. -J.; Haughian, K.; Healy, J.;
Heidmann, A.; Heintze, M. C.; Heitmann, H.; Hello, P.; Hemming, G.;
Hendry, M.; Heng, I. S.; Hennig, J.; Heptonstall, A. W.; Heurs, M.;
Hild, S.; Hinderer, T.; Hoak, D.; Hofman, D.; Holt, K.; Holz, D. E.;
Hopkins, P.; Horst, C.; Hough, J.; Houston, E. A.; Howell, E. J.;
Hreibi, A.; Hu, Y. M.; Huerta, E. A.; Huet, D.; Hughey, B.; Husa,
S.; Huttner, S. H.; Huynh-Dinh, T.; Indik, N.; Inta, R.; Intini, G.;
Isa, H. N.; Isac, J. -M.; Isi, M.; Iyer, B. R.; Izumi, K.; Jacqmin,
T.; Jani, K.; Jaranowski, P.; Jawahar, S.; Jiménez-Forteza, F.;
Johnson, W. W.; Jones, D. I.; Jones, R.; Jonker, R. J. G.; Ju, L.;
Junker, J.; Kalaghatgi, C. V.; Kalogera, V.; Kamai, B.; Kandhasamy,
S.; Kang, G.; Kanner, J. B.; Kapadia, S. J.; Karki, S.; Karvinen,
K. S.; Kasprzack, M.; Katolik, M.; Katsavounidis, E.; Katzman, W.;
Kaufer, S.; Kawabe, K.; Kéfélian, F.; Keitel, D.; Kemball, A. J.;
Kennedy, R.; Kent, C.; Key, J. S.; Khalili, F. Y.; Khan, I.; Khan, S.;
Khan, Z.; Khazanov, E. A.; Kijbunchoo, N.; Kim, Chunglee; Kim, J. C.;
Kim, K.; Kim, W.; Kim, W. S.; Kim, Y. -M.; Kimbrell, S. J.; King,
E. J.; King, P. J.; Kinley-Hanlon, M.; Kirchhoff, R.; Kissel, J. S.;
Kleybolte, L.; Klimenko, S.; Knowles, T. D.; Koch, P.; Koehlenbeck,
S. M.; Koley, S.; Kondrashov, V.; Kontos, A.; Korobko, M.; Korth,
W. Z.; Kowalska, I.; Kozak, D. B.; Krämer, C.; Kringel, V.; Krishnan,
B.; Królak, A.; Kuehn, G.; Kumar, P.; Kumar, R.; Kumar, S.; Kuo,
L.; Kutynia, A.; Kwang, S.; Lackey, B. D.; Lai, K. H.; Landry, M.;
Lang, R. N.; Lange, J.; Lantz, B.; Lanza, R. K.; Lartaux-Vollard,
A.; Lasky, P. D.; Laxen, M.; Lazzarini, A.; Lazzaro, C.; Leaci, P.;
Leavey, S.; Lee, C. H.; Lee, H. K.; Lee, H. M.; Lee, H. W.; Lee,
K.; Lehmann, J.; Lenon, A.; Leonardi, M.; Leroy, N.; Letendre, N.;
Levin, Y.; Li, T. G. F.; Linker, S. D.; Littenberg, T. B.; Liu, J.; Lo,
R. K. L.; Lockerbie, N. A.; London, L. T.; Lord, J. E.; Lorenzini, M.;
Loriette, V.; Lormand, M.; Losurdo, G.; Lough, J. D.; Lousto, C. O.;
Lovelace, G.; Lück, H.; Lumaca, D.; Lundgren, A. P.; Lynch, R.; Ma,
Y.; Macas, R.; Macfoy, S.; Machenschalk, B.; MacInnis, M.; Macleod,
D. M.; Magaña Hernandez, I.; Magaña-Sandoval, F.; Magaña Zertuche,
L.; Magee, R. M.; Majorana, E.; Maksimovic, I.; Man, N.; Mandic, V.;
Mangano, V.; Mansell, G. L.; Manske, M.; Mantovani, M.; Marchesoni,
F.; Marion, F.; Márka, S.; Márka, Z.; Markakis, C.; Markosyan, A. S.;
Markowitz, A.; Maros, E.; Marquina, A.; Martelli, F.; Martellini, L.;
Martin, I. W.; Martin, R. M.; Martynov, D. V.; Mason, K.; Massera,
E.; Masserot, A.; Massinger, T. J.; Masso-Reid, M.; Mastrogiovanni,
S.; Matas, A.; Matichard, F.; Matone, L.; Mavalvala, N.; Mazumder,
N.; McCarthy, R.; McClelland, D. E.; McCormick, S.; McCuller, L.;
McGuire, S. C.; McIntyre, G.; McIver, J.; McManus, D. J.; McNeill, L.;
McRae, T.; McWilliams, S. T.; Meacher, D.; Meadors, G. D.; Mehmet, M.;
Meidam, J.; Mejuto-Villa, E.; Melatos, A.; Mendell, G.; Mercer, R. A.;
Merilh, E. L.; Merzougui, M.; Meshkov, S.; Messenger, C.; Messick, C.;
Metzdorff, R.; Meyers, P. M.; Miao, H.; Michel, C.; Middleton, H.;
Mikhailov, E. E.; Milano, L.; Miller, A. L.; Miller, B. B.; Miller,
J.; Millhouse, M.; Milovich-Goff, M. C.; Minazzoli, O.; Minenkov, Y.;
Ming, J.; Mishra, C.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher,
G.; Mittleman, R.; Moffa, D.; Moggi, A.; Mogushi, K.; Mohan, M.;
Mohapatra, S. R. P.; Montani, M.; Moore, C. J.; Moraru, D.; Moreno,
G.; Morriss, S. R.; Mours, B.; Mow-Lowry, C. M.; Mueller, G.; Muir,
A. W.; Mukherjee, Arunava; Mukherjee, D.; Mukherjee, S.; Mukund, N.;
Mullavey, A.; Munch, J.; Muñiz, E. A.; Muratore, M.; Murray, P. G.;
Napier, K.; Nardecchia, I.; Naticchioni, L.; Nayak, R. K.; Neilson,
J.; Nelemans, G.; Nelson, T. J. N.; Nery, M.; Neunzert, A.; Nevin,
L.; Newport, J. M.; Newton, G.; Ng, K. K. Y.; Nguyen, T. T.; Nichols,
D.; Nielsen, A. B.; Nissanke, S.; Nitz, A.; Noack, A.; Nocera, F.;
Nolting, D.; North, C.; Nuttall, L. K.; Oberling, J.; O'Dea, G. D.;
Ogin, G. H.; Oh, J. J.; Oh, S. H.; Ohme, F.; Okada, M. A.; Oliver, M.;
Oppermann, P.; Oram, Richard J.; O'Reilly, B.; Ormiston, R.; Ortega,
L. F.; O'Shaughnessy, R.; Ossokine, S.; Ottaway, D. J.; Overmier, H.;
Owen, B. J.; Pace, A. E.; Page, J.; Page, M. A.; Pai, A.; Pai, S. A.;
Palamos, J. R.; Palashov, O.; Palomba, C.; Pal-Singh, A.; Pan, Howard;
Pan, Huang-Wei; Pang, B.; Pang, P. T. H.; Pankow, C.; Pannarale, F.;
Pant, B. C.; Paoletti, F.; Paoli, A.; Papa, M. A.; Parida, A.; Parker,
W.; Pascucci, D.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.;
Patil, M.; Patricelli, B.; Pearlstone, B. L.; Pedraza, M.; Pedurand,
R.; Pekowsky, L.; Pele, A.; Penn, S.; Perez, C. J.; Perreca, A.;
Perri, L. M.; Pfeiffer, H. P.; Phelps, M.; Piccinni, O. J.; Pichot,
M.; Piergiovanni, F.; Pierro, V.; Pillant, G.; Pinard, L.; Pinto,
I. M.; Pirello, M.; Pitkin, M.; Poe, M.; Poggiani, R.; Popolizio,
P.; Porter, E. K.; Post, A.; Powell, J.; Prasad, J.; Pratt, J. W. W.;
Pratten, G.; Predoi, V.; Prestegard, T.; Prijatelj, M.; Principe, M.;
Privitera, S.; Prodi, G. A.; Prokhorov, L. G.; Puncken, O.; Punturo,
M.; Puppo, P.; Pürrer, M.; Qi, H.; Quetschke, V.; Quintero, E. A.;
Quitzow-James, R.; Raab, F. J.; Rabeling, D. S.; Radkins, H.; Raffai,
P.; Raja, S.; Rajan, C.; Rajbhandari, B.; Rakhmanov, M.; Ramirez,
K. E.; Ramos-Buades, A.; Rapagnani, P.; Raymond, V.; Razzano, M.;
Read, J.; Regimbau, T.; Rei, L.; Reid, S.; Reitze, D. H.; Ren, W.;
Reyes, S. D.; Ricci, F.; Ricker, P. M.; Rieger, S.; Riles, K.; Rizzo,
M.; Robertson, N. A.; Robie, R.; Robinet, F.; Rocchi, A.; Rolland,
L.; Rollins, J. G.; Roma, V. J.; Romano, R.; Romel, C. L.; Romie,
J. H.; Rosińska, D.; Ross, M. P.; Rowan, S.; Rüdiger, A.; Ruggi,
P.; Rutins, G.; Ryan, K.; Sachdev, S.; Sadecki, T.; Sadeghian, L.;
Sakellariadou, M.; Salconi, L.; Saleem, M.; Salemi, F.; Samajdar,
A.; Sammut, L.; Sampson, L. M.; Sanchez, E. J.; Sanchez, L. E.;
Sanchis-Gual, N.; Sandberg, V.; Sanders, J. R.; Sassolas, B.; Saulson,
P. R.; Sauter, O.; Savage, R. L.; Sawadsky, A.; Schale, P.; Scheel,
M.; Scheuer, J.; Schmidt, J.; Schmidt, P.; Schnabel, R.; Schofield,
R. M. S.; Schönbeck, A.; Schreiber, E.; Schuette, D.; Schulte, B. W.;
Schutz, B. F.; Schwalbe, S. G.; Scott, J.; Scott, S. M.; Seidel, E.;
Sellers, D.; Sengupta, A. S.; Sentenac, D.; Sequino, V.; Sergeev, A.;
Shaddock, D. A.; Shaffer, T. J.; Shah, A. A.; Shahriar, M. S.; Shaner,
M. B.; Shao, L.; Shapiro, B.; Shawhan, P.; Sheperd, A.; Shoemaker,
D. H.; Shoemaker, D. M.; Siellez, K.; Siemens, X.; Sieniawska,
M.; Sigg, D.; Silva, A. D.; Singer, L. P.; Singh, A.; Singhal, A.;
Sintes, A. M.; Slagmolen, B. J. J.; Smith, B.; Smith, J. R.; Smith,
R. J. E.; Somala, S.; Son, E. J.; Sonnenberg, J. A.; Sorazu, B.;
Sorrentino, F.; Souradeep, T.; Spencer, A. P.; Srivastava, A. K.;
Staats, K.; Staley, A.; Steinke, M.; Steinlechner, J.; Steinlechner,
S.; Steinmeyer, D.; Stevenson, S. P.; Stone, R.; Stops, D. J.; Strain,
K. A.; Stratta, G.; Strigin, S. E.; Strunk, A.; Sturani, R.; Stuver,
A. L.; Summerscales, T. Z.; Sun, L.; Sunil, S.; Suresh, J.; Sutton,
P. J.; Swinkels, B. L.; Szczepańczyk, M. J.; Tacca, M.; Tait, S. C.;
Talbot, C.; Talukder, D.; Tanner, D. B.; Tápai, M.; Taracchini, A.;
Tasson, J. D.; Taylor, J. A.; Taylor, R.; Tewari, S. V.; Theeg, T.;
Thies, F.; Thomas, E. G.; Thomas, M.; Thomas, P.; Thorne, K. A.;
Thrane, E.; Tiwari, S.; Tiwari, V.; Tokmakov, K. V.; Toland, K.;
Tonelli, M.; Tornasi, Z.; Torres-Forné, A.; Torrie, C. I.; Töyrä,
D.; Travasso, F.; Traylor, G.; Trinastic, J.; Tringali, M. C.; Trozzo,
L.; Tsang, K. W.; Tse, M.; Tso, R.; Tsukada, L.; Tsuna, D.; Tuyenbayev,
D.; Ueno, K.; Ugolini, D.; Unnikrishnan, C. S.; Urban, A. L.; Usman,
S. A.; Vahlbruch, H.; Vajente, G.; Valdes, G.; van Bakel, N.; van
Beuzekom, M.; van den Brand, J. F. J.; Van Den Broeck, C.; Vander-Hyde,
D. C.; van der Schaaf, L.; van Heijningen, J. V.; van Veggel, A. A.;
Vardaro, M.; Varma, V.; Vass, S.; Vasúth, M.; Vecchio, A.; Vedovato,
G.; Veitch, J.; Veitch, P. J.; Venkateswara, K.; Venugopalan, G.;
Verkindt, D.; Vetrano, F.; Viceré, A.; Viets, A. D.; Vinciguerra, S.;
Vine, D. J.; Vinet, J. -Y.; Vitale, S.; Vo, T.; Vocca, H.; Vorvick,
C.; Vyatchanin, S. P.; Wade, A. R.; Wade, L. E.; Wade, M.; Walet, R.;
Walker, M.; Wallace, L.; Walsh, S.; Wang, G.; Wang, H.; Wang, J. Z.;
Wang, W. H.; Wang, Y. F.; Ward, R. L.; Warner, J.; Was, M.; Watchi,
J.; Weaver, B.; Wei, L. -W.; Weinert, M.; Weinstein, A. J.; Weiss,
R.; Wen, L.; Wessel, E. K.; Weßels, P.; Westerweck, J.; Westphal,
T.; Wette, K.; Whelan, J. T.; Whiting, B. F.; Whittle, C.; Wilken,
D.; Williams, D.; Williams, R. D.; Williamson, A. R.; Willis, J. L.;
Willke, B.; Wimmer, M. H.; Winkler, W.; Wipf, C. C.; Wittel, H.; Woan,
G.; Woehler, J.; Wofford, J.; Wong, K. W. K.; Worden, J.; Wright,
J. L.; Wu, D. S.; Wysocki, D. M.; Xiao, S.; Yamamoto, H.; Yancey,
C. C.; Yang, L.; Yap, M. J.; Yazback, M.; Yu, Hang; Yu, Haocun; Yvert,
M.; Zadrożny, A.; Zanolin, M.; Zelenova, T.; Zendri, J. -P.; Zevin,
M.; Zhang, L.; Zhang, M.; Zhang, T.; Zhang, Y. -H.; Zhao, C.; Zhou,
M.; Zhou, Z.; Zhu, S. J.; Zhu, X. J.; Zucker, M. E.; Zweizig, J.;
LIGO Scientific Collaboration; Virgo Collaboration
2017ApJ...850L..35A Altcode: 2017arXiv171005839A
The Advanced LIGO and Advanced Virgo observatories recently discovered
gravitational waves from a binary neutron star inspiral. A short
gamma-ray burst (GRB) that followed the merger of this binary was also
recorded by the Fermi Gamma-ray Burst Monitor (Fermi-GBM), and the
Anti-Coincidence Shield for the Spectrometer for the International
Gamma-Ray Astrophysics Laboratory (INTEGRAL), indicating particle
acceleration by the source. The precise location of the event was
determined by optical detections of emission following the merger. We
searched for high-energy neutrinos from the merger in the GeV-EeV energy
range using the ANTARES, IceCube, and Pierre Auger Observatories. No
neutrinos directionally coincident with the source were detected within
±500 s around the merger time. Additionally, no MeV neutrino burst
signal was detected coincident with the merger. We further carried
out an extended search in the direction of the source for high-energy
neutrinos within the 14 day period following the merger, but found
no evidence of emission. We used these results to probe dissipation
mechanisms in relativistic outflows driven by the binary neutron star
merger. The non-detection is consistent with model predictions of
short GRBs observed at a large off-axis angle.
---------------------------------------------------------
Title: Comprehensive Analysis of the Geoeffective Solar Event
of 21 June 2015: Effects on the Magnetosphere, Plasmasphere, and
Ionosphere Systems
Authors: Piersanti, Mirko; Alberti, Tommaso; Bemporad, Alessandro;
Berrilli, Francesco; Bruno, Roberto; Capparelli, Vincenzo; Carbone,
Vincenzo; Cesaroni, Claudio; Consolini, Giuseppe; Cristaldi, Alice;
Del Corpo, Alfredo; Del Moro, Dario; Di Matteo, Simone; Ermolli,
Ilaria; Fineschi, Silvano; Giannattasio, Fabio; Giorgi, Fabrizio;
Giovannelli, Luca; Guglielmino, Salvatore Luigi; Laurenza, Monica;
Lepreti, Fabio; Marcucci, Maria Federica; Martucci, Matteo; Mergè,
Matteo; Pezzopane, Michael; Pietropaolo, Ermanno; Romano, Paolo;
Sparvoli, Roberta; Spogli, Luca; Stangalini, Marco; Vecchio, Antonio;
Vellante, Massimo; Villante, Umberto; Zuccarello, Francesca; Heilig,
Balázs; Reda, Jan; Lichtenberger, János
2017SoPh..292..169P Altcode:
A full-halo coronal mass ejection (CME) left the Sun on 21 June 2015
from active region (AR) NOAA 12371. It encountered Earth on 22 June
2015 and generated a strong geomagnetic storm whose minimum Dst value
was −204 nT. The CME was associated with an M2-class flare observed
at 01:42 UT, located near disk center (N12 E16). Using satellite data
from solar, heliospheric, and magnetospheric missions and ground-based
instruments, we performed a comprehensive Sun-to-Earth analysis. In
particular, we analyzed the active region evolution using ground-based
and satellite instruments (Big Bear Solar Observatory (BBSO), Interface
Region Imaging Spectrograph (IRIS), Hinode, Atmospheric Imaging Assembly
(AIA) onboard the Solar Dynamics Observatory (SDO), Reuven Ramaty High
Energy Solar Spectroscopic Imager (RHESSI), covering Hα , EUV, UV, and
X-ray data); the AR magnetograms, using data from SDO/Helioseismic and
Magnetic Imager (HMI); the high-energy particle data, using the Payload
for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA)
instrument; and the Rome neutron monitor measurements to assess the
effects of the interplanetary perturbation on cosmic-ray intensity. We
also evaluated the 1 - 8 Å soft X-ray data and the ∼1 MHz type III
radio burst time-integrated intensity (or fluence) of the flare in order
to predict the associated solar energetic particle (SEP) event using
the model developed by Laurenza et al. (Space Weather7(4), 2009). In
addition, using ground-based observations from lower to higher latitudes
(International Real-time Magnetic Observatory Network (INTERMAGNET) and
European Quasi-Meridional Magnetometer Array (EMMA)), we reconstructed
the ionospheric current system associated with the geomagnetic
sudden impulse (SI). Furthermore, Super Dual Auroral Radar Network
(SuperDARN) measurements were used to image the global ionospheric
polar convection during the SI and during the principal phases of
the geomagnetic storm. In addition, to investigate the influence of
the disturbed electric field on the low-latitude ionosphere induced
by geomagnetic storms, we focused on the morphology of the crests
of the equatorial ionospheric anomaly by the simultaneous use of the
Global Navigation Satellite System (GNSS) receivers, ionosondes, and
Langmuir probes onboard the Swarm constellation satellites. Moreover,
we investigated the dynamics of the plasmasphere during the different
phases of the geomagnetic storm by examining the time evolution of
the radial profiles of the equatorial plasma mass density derived from
field line resonances detected at the EMMA network (1.5 <L <6.5
). Finally, we present the general features of the geomagnetic response
to the CME by applying innovative data analysis tools that allow us
to investigate the time variation of ground-based observations of the
Earth's magnetic field during the associated geomagnetic storm.
---------------------------------------------------------
Title: The 2013 February 17 Sunquake in the Context of the Active
Region's Magnetic Field Configuration
Authors: Green, L. M.; Valori, G.; Zuccarello, F. P.; Zharkov, S.;
Matthews, S. A.; Guglielmino, S. L.
2017ApJ...849...40G Altcode: 2017arXiv170904874G
Sunquakes are created by the hydrodynamic response of the lower
atmosphere to a sudden deposition of energy and momentum. In this study,
we investigate a sunquake that occurred in NOAA active region 11675
on 2013 February 17. Observations of the corona, chromosphere, and
photosphere are brought together for the first time with a nonlinear
force-free model of the active region’s magnetic field in order to
probe the magnetic environment in which the sunquake was initiated. We
find that the sunquake was associated with the destabilization of a
flux rope and an associated M-class GOES flare. Active region 11675
was in its emergence phase at the time of the sunquake and photospheric
motions caused by the emergence heavily modified the flux rope and its
associated quasi-separatrix layers, eventually triggering the flux
rope’s instability. The flux rope was surrounded by an extended
envelope of field lines rooted in a small area at the approximate
position of the sunquake. We argue that the configuration of the
envelope, by interacting with the expanding flux rope, created a
“magnetic lens” that may have focussed energy on one particular
location of the photosphere, creating the necessary conditions for
the initiation of the sunquake.
---------------------------------------------------------
Title: Hα and Hβ Emission in a C3.3 Solar Flare: Comparison between
Observations and Simulations
Authors: Capparelli, Vincenzo; Zuccarello, Francesca; Romano, Paolo;
Simões, Paulo J. A.; Fletcher, Lyndsay; Kuridze, David; Mathioudakis,
Mihalis; Keys, Peter H.; Cauzzi, Gianna; Carlsson, Mats
2017ApJ...850...36C Altcode: 2017arXiv171004067C
The hydrogen Balmer series is a basic radiative loss channel from
the flaring solar chromosphere. We report here on the analysis of an
extremely rare set of simultaneous observations of a solar flare in the
{{H}}α and {{H}}β lines, at high spatial and temporal resolutions,
that were acquired at the Dunn Solar Telescope. Images of the C3.3 flare
(SOL2014-04-22T15:22) made at various wavelengths along the {{H}}α line
profile by the Interferometric Bidimensional Spectrometer (IBIS) and in
the {{H}}β with the Rapid Oscillations in the Solar Atmosphere (ROSA)
broadband imager are analyzed to obtain the intensity evolution. The
{{H}}α and {{H}}β intensity excesses in three identified flare
footpoints are well-correlated in time. We examine the ratio of {{H}}α
to {{H}}β flare excess, which was proposed by previous authors as
a possible diagnostic of the level of electron-beam energy input. In
the stronger footpoints, the typical value of the the {{H}}α /H β
intensity ratio observed is ∼0.4-0.5, in broad agreement with values
obtained from a RADYN non-LTE simulation driven by an electron beam
with parameters constrained (as far as possible) by observation. The
weaker footpoint has a larger {{H}}α /H β ratio, again consistent
with a RADYN simulation, but with a smaller energy flux. The {{H}}α
line profiles observed have a less prominent central reversal than is
predicted by the RADYN results, but can be brought into agreement if
the {{H}}α -emitting material has a filling factor of around 0.2-0.3.
---------------------------------------------------------
Title: Inferences on Mass Composition and Tests of Hadronic
Interactions from 0.3 to 100 EeV using the water-Cherenkov Detectors
of the Pierre Auger Observatory
Authors: The Pierre Auger Collaboration; Aab, A.; Abreu, P.; Aglietta,
M.; Samarai, I. Al; Albuquerque, I. F. M.; Allekotte, I.; Almela,
A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Anastasi, G. A.;
Anchordoqui, L.; Andrada, B.; Andringa, S.; Aramo, C.; Arqueros, F.;
Arsene, N.; Asorey, H.; Assis, P.; Aublin, J.; Avila, G.; Badescu,
A. M.; Balaceanu, A.; Barbato, F.; Barreira Luz, R. J.; Beatty,
J. J.; Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.;
Bertou, X.; Biermann, P. L.; Biteau, J.; Blaess, S. G.; Blanco,
A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Botti, A. M.; Brack, J.; Brancus, I.; Bretz, T.;
Bridgeman, A.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink,
S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, L.; Cancio, A.;
Canfora, F.; Caramete, L.; Caruso, R.; Castellina, A.; Catalani, F.;
Cataldi, G.; Cazon, L.; Chavez, A. G.; Chinellato, J. A.; Chudoba,
J.; Clay, R. W.; Cobos, A.; Colalillo, R.; Coleman, A.; Collica,
L.; Coluccia, M. R.; Conceição, R.; Consolati, G.; Contreras, F.;
Cooper, M. J.; Coutu, S.; Covault, C. E.; Cronin, J.; D'Amico, S.;
Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; de Almeida,
R. M.; de Jong, S. J.; De Mauro, G.; de Mello Neto, J. R. T.; De
Mitri, I.; de Oliveira, J.; de Souza, V.; Debatin, J.; Deligny,
O.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.;
Dorosti, Q.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.;
Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.;
Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar, G.; Fauth, A. C.;
Fazzini, N.; Fenu, F.; Fick, B.; Figueira, J. M.; Filipčič, A.;
Fratu, O.; Freire, M. M.; Fujii, T.; Fuster, A.; Gaior, R.; García,
B.; Garcia-Pinto, D.; Gaté, F.; Gemmeke, H.; Gherghel-Lascu, A.;
Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Głas, D.;
Glaser, C.; Golup, G.; Gómez Berisso, M.; Gómez Vitale, P. F.;
González, N.; Gorgi, A.; Gorham, P.; Grillo, A. F.; Grubb, T. D.;
Guarino, F.; Guedes, G. P.; Halliday, R.; Hampel, M. R.; Hansen, P.;
Harari, D.; Harrison, T. A.; Harton, J. L.; Haungs, A.; Hebbeker, T.;
Heck, D.; Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Holt,
E.; Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege,
T.; Hulsman, J.; Insolia, A.; Isar, P. G.; Jandt, I.; Johnsen, J. A.;
Josebachuili, M.; Jurysek, J.; Kääpä, A.; Kambeitz, O.; Kampert,
K. H.; Keilhauer, B.; Kemmerich, N.; Kemp, E.; Kemp, J.; Kieckhafer,
R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.;
Krohm, N.; Kuempel, D.; Kukec Mezek, G.; Kunka, N.; Kuotb Awad,
A.; Lago, B. L.; LaHurd, D.; Lang, R. G.; Lauscher, M.; Legumina,
R.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon,
I.; Link, K.; Lo Presti, D.; Lopes, L.; López, R.; López Casado,
A.; Lorek, R.; Luce, Q.; Lucero, A.; Malacari, M.; Mallamaci, M.;
Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Mariş, I. C.; Marsella,
G.; Martello, D.; Martinez, H.; Martínez Bravo, O.; Masías Meza,
J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.;
Matthiae, G.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco,
G.; Melo, D.; Menshikov, A.; Merenda, K. -D.; Michal, S.; Micheletti,
M. I.; Middendorf, L.; Miramonti, L.; Mitrica, B.; Mockler, D.;
Mollerach, S.; Montanet, F.; Morello, C.; Mostafá, M.; Müller,
A. L.; Müller, G.; Muller, M. A.; Müller, S.; Mussa, R.; Naranjo,
I.; Nellen, L.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.;
Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka,
L.; Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Palatka,
M.; Pallotta, J.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.;
Pech, M.; Pedreira, F.; Pękala, J.; Pelayo, R.; Peña-Rodriguez, J.;
Pereira, L. A. S.; Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.;
Phuntsok, J.; Piegaia, R.; Pierog, T.; Pimenta, M.; Pirronello, V.;
Platino, M.; Plum, M.; Porowski, C.; Prado, R. R.; Privitera, P.;
Prouza, M.; Quel, E. J.; Querchfeld, S.; Quinn, S.; Ramos-Pollan,
R.; Rautenberg, J.; Ravignani, D.; Ridky, J.; Riehn, F.; Risse, M.;
Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Fernandez,
G.; Rodriguez Rojo, J.; Rogozin, D.; Roncoroni, M. J.; Roth, M.;
Roulet, E.; Rovero, A. C.; Ruehl, P.; Saffi, S. J.; Saftoiu, A.;
Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.; Salina, G.;
Sánchez, F.; Sanchez-Lucas, P.; Santos, E. M.; Santos, E.; Sarazin,
F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.; Schauer, M.; Scherini,
V.; Schieler, H.; Schimp, M.; Schmidt, D.; Scholten, O.; Schovánek,
P.; Schröder, F. G.; Schröder, S.; Schulz, A.; Schumacher, J.;
Sciutto, S. J.; Segreto, A.; Shadkam, A.; Shellard, R. C.; Sigl, G.;
Silli, G.; Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.;
Sommers, P.; Sonntag, S.; Squartini, R.; Stanca, D.; Stanič, S.;
Stasielak, J.; Stassi, P.; Stolpovskiy, M.; Strafella, F.; Streich,
A.; Suarez, F.; Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.;
Supanitsky, A. D.; Šupík, J.; Swain, J.; Szadkowski, Z.; Taboada,
A.; Taborda, O. A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Tomankova, L.; Tomé, B.; Torralba Elipe, G.; Travnicek, P.;
Trini, M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.;
Valiño, I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg,
A. M.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.;
Vázquez, R. A.; Veberič, D.; Ventura, C.; Vergara Quispe, I. D.;
Verzi, V.; Vicha, J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.;
Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke,
L.; Wilczyński, H.; Wirtz, M.; Wittkowski, D.; Wundheiler, B.; Yang,
L.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zepeda, A.;
Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello, F.
2017arXiv171007249T Altcode:
We present a new method for probing the hadronic interaction models at
ultra-high energy and extracting details about mass composition. This
is done using the time profiles of the signals recorded with the
water-Cherenkov detectors of the Pierre Auger Observatory. The
profiles arise from a mix of the muon and electromagnetic components of
air-showers. Using the risetimes of the recorded signals we define a new
parameter, which we use to compare our observations with predictions
from simulations. We find, firstly, inconsistencies between our data
and predictions over a greater energy range and with substantially
more events than in previous studies. Secondly, by calibrating the new
parameter with fluorescence measurements from observations made at the
Auger Observatory, we can infer the depth of shower maximum for a sample
of over 81,000 events extending from 0.3 EeV to over 100 EeV. Above 30
EeV, the sample is nearly fourteen times larger than currently available
from fluorescence measurements and extending the covered energy range
by half a decade. The energy dependence of the average depth of shower
maximum is compared to simulations and interpreted in terms of the
mean of the logarithmic mass. We find good agreement with previous
work and extend the measurement of the mean depth of shower maximum to
greater energies than before, reducing significantly the statistical
uncertainty associated with the inferences about mass composition.
---------------------------------------------------------
Title: Spectral calibration of the fluorescence telescopes of the
Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Al Samarai, I.;
Albuquerque, I. F. M.; Allekotte, I.; Almela, A.; Alvarez Castillo,
J.; Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.;
Andringa, S.; Aramo, C.; Arqueros, F.; Arsene, N.; Asorey, H.; Assis,
P.; Aublin, J.; Avila, G.; Badescu, A. M.; Balaceanu, A.; Barbato, F.;
Barreira Luz, R. J.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.;
Berat, C.; Bertaina, M. E.; Biermann, P. L.; Biteau, J.; Blaess,
S. G.; Blanco, A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli,
D.; Bonifazi, C.; Borodai, N.; Botti, A. M.; Brack, J.; Brancus,
I.; Bretz, T.; Bridgeman, A.; Briechle, F. L.; Buchholz, P.; Bueno,
A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga,
L.; Cancio, A.; Canfora, F.; Caramete, L.; Caruso, R.; Castellina,
A.; Catalani, F.; Cataldi, G.; Cazon, L.; Chavez, A. G.; Chinellato,
J. A.; Chudoba, J.; Clay, R. W.; Cobos, A.; Colalillo, R.; Coleman,
A.; Collica, L.; Coluccia, M. R.; Conceição, R.; Consolati, G.;
Contreras, F.; Cooper, M. J.; Coutu, S.; Covault, C. E.; Cronin, J.;
D'Amico, S.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; de
Almeida, R. M.; de Jong, S. J.; De Mauro, G.; de Mello Neto, J. R. T.;
De Mitri, I.; de Oliveira, J.; de Souza, V.; Debatin, J.; Deligny,
O.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.;
Dorosti, Q.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.;
Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.;
Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar, G.; Fauth, A. C.;
Fazzini, N.; Fenu, F.; Fick, B.; Figueira, J. M.; Filipčič, A.;
Fratu, O.; Freire, M. M.; Fujii, T.; Fuster, A.; Gaior, R.; García,
B.; Garcia-Pinto, D.; Gaté, F.; Gemmeke, H.; Gherghel-Lascu, A.;
Giaccari, U.; Giammarchi, M.; Giller, M.; Głas, D.; Glaser, C.;
Golup, G.; Gómez Berisso, M.; Gómez Vitale, P. F.; González,
N.; Gookin, B.; Gorgi, A.; Gorham, P.; Grillo, A. F.; Grubb, T. D.;
Guarino, F.; Guedes, G. P.; Halliday, R.; Hampel, M. R.; Hansen, P.;
Harari, D.; Harrison, T. A.; Harton, J. L.; Haungs, A.; Hebbeker, T.;
Heck, D.; Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Holt,
E.; Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege,
T.; Hulsman, J.; Insolia, A.; Isar, P. G.; Jandt, I.; Johnsen, J. A.;
Josebachuili, M.; Jurysek, J.; Kääpä, A.; Kambeitz, O.; Kampert,
K. H.; Keilhauer, B.; Kemmerich, N.; Kemp, E.; Kemp, J.; Kieckhafer,
R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.;
Krohm, N.; Kuempel, D.; Kukec Mezek, G.; Kunka, N.; Kuotb Awad,
A.; Lago, B. L.; LaHurd, D.; Lang, R. G.; Lauscher, M.; Legumina,
R.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon,
I.; Link, K.; Lo Presti, D.; Lopes, L.; López, R.; López Casado,
A.; Lorek, R.; Luce, Q.; Lucero, A.; Malacari, M.; Mallamaci, M.;
Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Mariş, I. C.; Marsella, G.;
Martello, D.; Martinez, H.; Martínez Bravo, O.; Masías Meza, J. J.;
Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.; Matthiae,
G.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Melo,
D.; Menshikov, A.; Merenda, K. -D.; Michal, S.; Micheletti, M. I.;
Middendorf, L.; Miramonti, L.; Mitrica, B.; Mockler, D.; Mollerach,
S.; Montanet, F.; Morello, C.; Mostafá, M.; Müller, A. L.; Müller,
G.; Muller, M. A.; Müller, S.; Mussa, R.; Naranjo, I.; Nellen, L.;
Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.; Niemietz, L.;
Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.; Núñez,
L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Palatka, M.; Pallotta,
J.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.; Pech, M.;
Pedreira, F.; Pȩkala, J.; Pelayo, R.; Peña-Rodriguez, J.; Pereira,
L. A. S.; Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.; Phuntsok,
J.; Piegaia, R.; Pierog, T.; Pimenta, M.; Pirronello, V.; Platino, M.;
Plum, M.; Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Quel,
E. J.; Querchfeld, S.; Quinn, S.; Ramos-Pollan, R.; Rautenberg, J.;
Ravignani, D.; Ridky, J.; Riehn, F.; Risse, M.; Ristori, P.; Rizi,
V.; Rodrigues de Carvalho, W.; Rodriguez Fernandez, G.; Rodriguez
Rojo, J.; Rogozin, D.; Roncoroni, M. J.; Roth, M.; Roulet, E.;
Rovero, A. C.; Ruehl, P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.;
Salazar, H.; Saleh, A.; Salesa Greus, F.; Salina, G.; Sánchez, F.;
Sanchez-Lucas, P.; Santos, E. M.; Santos, E.; Sarazin, F.; Sarmento,
R.; Sarmiento-Cano, C.; Sato, R.; Schauer, M.; Scherini, V.; Schieler,
H.; Schimp, M.; Schmidt, D.; Scholten, O.; Schovánek, P.; Schröder,
F. G.; Schröder, S.; Schulz, A.; Schumacher, J.; Sciutto, S. J.;
Segreto, A.; Shadkam, A.; Shellard, R. C.; Sigl, G.; Silli, G.;
Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers, P.;
Sonntag, S.; Squartini, R.; Stanca, D.; Stanič, S.; Stasielak, J.;
Stassi, P.; Stolpovskiy, M.; Strafella, F.; Streich, A.; Suarez, F.;
Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky, A. D.;
Šupík, J.; Swain, J.; Szadkowski, Z.; Taboada, A.; Taborda, O. A.;
Theodoro, V. M.; Timmermans, C.; Todero Peixoto, C. J.; Tomankova, L.;
Tomé, B.; Torralba Elipe, G.; Travnicek, P.; Trini, M.; Ulrich, R.;
Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore,
L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.; van Vliet,
A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.; Vázquez, R. A.;
Veberič, D.; Ventura, C.; Vergara Quispe, I. D.; Verzi, V.; Vicha,
J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz,
D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński,
H.; Wirtz, M.; Wittkowski, D.; Wundheiler, B.; Yang, L.; Yushkov, A.;
Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zepeda, A.; Zimmermann, B.;
Ziolkowski, M.; Zong, Z.; Zuccarello, F.; Pierre Auger Collaboration
2017APh....95...44A Altcode: 2017arXiv170901537T
We present a novel method to measure precisely the relative
spectral response of the fluorescence telescopes of the Pierre Auger
Observatory. We used a portable light source based on a xenon flasher
and a monochromator to measure the relative spectral efficiencies of
eight telescopes in steps of 5 nm from 280 nm to 440 nm. Each point in
a scan had approximately 2 nm FWHM out of the monochromator. Different
sets of telescopes in the observatory have different optical components,
and the eight telescopes measured represent two each of the four
combinations of components represented in the observatory. We made an
end-to-end measurement of the response from different combinations
of optical components, and the monochromator setup allowed for more
precise and complete measurements than our previous multi-wavelength
calibrations. We find an overall uncertainty in the calibration of the
spectral response of most of the telescopes of 1.5% for all wavelengths;
the six oldest telescopes have larger overall uncertainties of about
2.2%. We also report changes in physics measurables due to the change
in calibration, which are generally small.
---------------------------------------------------------
Title: Slippage of Jets Explained by the Magnetic Topology of NOAA
Active Region 12035
Authors: Joshi, R.; Schmieder, B.; Chandra, R.; Aulanier, G.;
Zuccarello, F. P.; Uddin, W.
2017SoPh..292..152J Altcode: 2017arXiv170902791J
We present the investigation of 11 recurring solar jets that originated
from two different sites (site 1 and site 2) close to each other (≈11
Mm) in NOAA active region (AR) 12035 during 15 - 16 April 2014. The
jets were observed by the Atmospheric Imaging Assembly (AIA) telescope
on board the Solar Dynamics Observatory (SDO) satellite. Two jets
were observed by the telescope of the Aryabhatta Research Institute of
Observational Sciences (ARIES), Nainital, India, in Hα . On 15 April,
flux emergence is strong in site 1, while on 16 April, flux emergence
and cancellation mechanisms are involved in both sites. The jets of
both sites have parallel trajectories and move to the south with a
speed between 100 and 360 km s<SUP>−1</SUP>. The jets of site 2
occurred during the second day have a tendency to move toward the
jets of site 1 and merge with them. We conjecture that the slippage
of the jets could be explained by the complex topology of the region,
which included a few low-altitude null points and many quasi-separatrix
layers (QSLs), which could intersect with one another.
---------------------------------------------------------
Title: Calibration of the logarithmic-periodic dipole antenna (LPDA)
radio stations at the Pierre Auger Observatory using an octocopter
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Samarai, I. Al;
Albuquerque, I. F. M.; Allekotte, I.; Almela, A.; Alvarez Castillo,
J.; Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada,
B.; Andringa, S.; Aramo, C.; Arqueros, F.; Arsene, N.; Asorey, H.;
Assis, P.; Aublin, J.; Avila, G.; Badescu, A. M.; Balaceanu, A.;
Barbato, F.; Barreira Luz, R. J.; Beatty, J. J.; Becker, K. H.;
Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann,
P. L.; Billoir, P.; Biteau, J.; Blaess, S. G.; Blanco, A.; Blazek,
J.; Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi, C.; Borodai,
N.; Botti, A. M.; Brack, J.; Brancus, I.; Bretz, T.; Bridgeman,
A.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi,
M.; Caballero-Mora, K. S.; Caccianiga, L.; Cancio, A.; Canfora, F.;
Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.; Cazon, L.;
Chavez, A. G.; Chinellato, J. A.; Chudoba, J.; Clay, R. W.; Cobos, A.;
Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição,
R.; Consolati, G.; Contreras, F.; Cooper, M. J.; Coutu, S.; Covault,
C. E.; Cronin, J.; D'Amico, S.; Daniel, B.; Dasso, S.; Daumiller,
K.; Dawson, B. R.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza,
V.; Debatin, J.; Deligny, O.; Di Giulio, C.; Di Matteo, A.; Díaz
Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.; Dorosti,
Q.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.;
Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen,
A.; Falcke, H.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Fenu, F.;
Fick, B.; Figueira, J. M.; Filipčič, A.; Fratu, O.; Freire, M. M.;
Fujii, T.; Fuster, A.; Gaior, R.; García, B.; Garcia-Pinto, D.;
Gaté, F.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari,
U.; Giammarchi, M.; Giller, M.; Głas, D.; Glaser, C.; Golup, G.;
Gómez Berisso, M.; Gómez Vitale, P. F.; González, N.; Gorgi, A.;
Gorham, P.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.;
Hampel, M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Harton, J. L.;
Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill,
G. C.; Hojvat, C.; Holt, E.; Homola, P.; Hörandel, J. R.; Horvath,
P.; Hrabovský, M.; Huege, T.; Hulsman, J.; Insolia, A.; Isar, P. G.;
Jandt, I.; Jansen, S.; Johnsen, J. A.; Josebachuili, M.; Kääpä, A.;
Kambeitz, O.; Kampert, K. H.; Katkov, I.; Keilhauer, B.; Kemmerich,
N.; Kemp, E.; Kemp, J.; Kieckhafer, R. M.; Klages, H. O.; Kleifges,
M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Kuempel, D.; Kukec Mezek,
G.; Kunka, N.; Kuotb Awad, A.; LaHurd, D.; Lauscher, M.; Legumina,
R.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon,
I.; Link, K.; Lo Presti, D.; Lopes, L.; López, R.; López Casado,
A.; Luce, Q.; Lucero, A.; Malacari, M.; Mallamaci, M.; Mandat, D.;
Mantsch, P.; Mariazzi, A. G.; Mariş, I. C.; Marsella, G.; Martello,
D.; Martinez, H.; Martínez Bravo, O.; Masías Meza, J. J.; Mathes,
H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.; Matthiae, G.;
Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Melo, D.;
Menshikov, A.; Merenda, K. -D.; Micheletti, M. I.; Middendorf, L.;
Minaya, I. A.; Miramonti, L.; Mitrica, B.; Mockler, D.; Mollerach,
S.; Montanet, F.; Morello, C.; Mostafá, M.; Müller, A. L.; Müller,
G.; Muller, M. A.; Müller, S.; Mussa, R.; Naranjo, I.; Nellen, L.;
Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.; Niemietz,
L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, H.;
Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Palatka,
M.; Pallotta, J.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.;
Pech, M.; Pedreira, F.; Pȩkala, J.; Pelayo, R.; Peña-Rodriguez,
J.; Pereira, L. A. S.; Perlín, M.; Perrone, L.; Peters, C.; Petrera,
S.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.;
Pirronello, V.; Platino, M.; Plum, M.; Porowski, C.; Prado, R. R.;
Privitera, P.; Prouza, M.; Quel, E. J.; Querchfeld, S.; Quinn, S.;
Ramos-Pollan, R.; Rautenberg, J.; Ravignani, D.; Revenu, B.; Ridky,
J.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.;
Rodriguez Fernandez, G.; Rodriguez Rojo, J.; Rogozin, D.; Roncoroni,
M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl, P.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santos, E. M.; Santos,
E.; Sarazin, F.; Sarmento, R.; Sarmiento, C. A.; Sato, R.; Schauer,
M.; Scherini, V.; Schieler, H.; Schimp, M.; Schmidt, D.; Scholten,
O.; Schovánek, P.; Schröder, F. G.; Schulz, A.; Schumacher, J.;
Sciutto, S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard,
R. C.; Sigl, G.; Silli, G.; Sima, O.; Śmiałkowski, A.; Šmída,
R.; Snow, G. R.; Sommers, P.; Sonntag, S.; Sorokin, J.; Squartini,
R.; Stanca, D.; Stanič, S.; Stasielak, J.; Stassi, P.; Strafella,
F.; Suarez, F.; Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.;
Supanitsky, A. D.; Swain, J.; Szadkowski, Z.; Taboada, A.; Taborda,
O. A.; Tapia, A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Tomankova, L.; Tomé, B.; Torralba Elipe, G.; Travnicek, P.;
Trini, M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.;
Valiño, I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg,
A. M.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.;
Vázquez, R. A.; Veberič, D.; Vergara Quispe, I. D.; Verzi, V.; Vicha,
J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz,
D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński,
H.; Winchen, T.; Wirtz, M.; Wittkowski, D.; Wundheiler, B.; Yang,
L.; Yelos, D.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello, F.
2017JInst..1210005A Altcode: 2017arXiv170201392T
An in-situ calibration of a logarithmic periodic dipole antenna with
a frequency coverage of 30 MHz to 80 MHz is performed. Such antennas
are part of a radio station system used for detection of cosmic ray
induced air showers at the Engineering Radio Array of the Pierre
Auger Observatory, the so-called Auger Engineering Radio Array (AERA)
. The directional and frequency characteristics of the broadband
antenna are investigated using a remotely piloted aircraft carrying
a small transmitting antenna. The antenna sensitivity is described
by the vector effective length relating the measured voltage with
the electric-field components perpendicular to the incoming signal
direction. The horizontal and meridional components are determined
with an overall uncertainty of 7.4<SUP>+0.9</SUP><SUB>-0.3</SUB>% and
10.3<SUP>+2.8</SUP><SUB>-1.7</SUB>% respectively. The measurement
is used to correct a simulated response of the frequency and
directional response of the antenna. In addition, the influence of
the ground conductivity and permittivity on the antenna response
is simulated. Both have a negligible influence given the ground
conditions measured at the detector site. The overall uncertainties
of the vector effective length components result in an uncertainty of
8.8<SUP>+2.1</SUP><SUB>-1.3</SUB>% in the square root of the energy
fluence for incoming signal directions with zenith angles smaller
than 60°.
---------------------------------------------------------
Title: Multi-messenger Observations of a Binary Neutron Star Merger
Authors: Abbott, B. P.; Abbott, R.; Abbott, T. D.; Acernese, F.;
Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya,
V. B.; Affeldt, C.; Afrough, M.; Agarwal, B.; Agathos, M.; Agatsuma,
K.; Aggarwal, N.; Aguiar, O. D.; Aiello, L.; Ain, A.; Ajith, P.;
Allen, B.; Allen, G.; Allocca, A.; Altin, P. A.; Amato, A.; Ananyeva,
A.; Anderson, S. B.; Anderson, W. G.; Angelova, S. V.; Antier, S.;
Appert, S.; Arai, K.; Araya, M. C.; Areeda, J. S.; Arnaud, N.; Arun,
K. G.; Ascenzi, S.; Ashton, G.; Ast, M.; Aston, S. M.; Astone, P.;
Atallah, D. V.; Aufmuth, P.; Aulbert, C.; AultONeal, K.; Austin,
C.; Avila-Alvarez, A.; Babak, S.; Bacon, P.; Bader, M. K. M.; Bae,
S.; Baker, P. T.; Baldaccini, F.; Ballardin, G.; Ballmer, S. W.;
Banagiri, S.; Barayoga, J. C.; Barclay, S. E.; Barish, B. C.; Barker,
D.; Barkett, K.; Barone, F.; Barr, B.; Barsotti, L.; Barsuglia,
M.; Barta, D.; Barthelmy, S. D.; Bartlett, J.; Bartos, I.; Bassiri,
R.; Basti, A.; Batch, J. C.; Bawaj, M.; Bayley, J. C.; Bazzan, M.;
Bécsy, B.; Beer, C.; Bejger, M.; Belahcene, I.; Bell, A. S.; Berger,
B. K.; Bergmann, G.; Bero, J. J.; Berry, C. P. L.; Bersanetti, D.;
Bertolini, A.; Betzwieser, J.; Bhagwat, S.; Bhandare, R.; Bilenko,
I. A.; Billingsley, G.; Billman, C. R.; Birch, J.; Birney, R.;
Birnholtz, O.; Biscans, S.; Biscoveanu, S.; Bisht, A.; Bitossi, M.;
Biwer, C.; Bizouard, M. A.; Blackburn, J. K.; Blackman, J.; Blair,
C. D.; Blair, D. G.; Blair, R. M.; Bloemen, S.; Bock, O.; Bode, N.;
Boer, M.; Bogaert, G.; Bohe, A.; Bondu, F.; Bonilla, E.; Bonnand, R.;
Boom, B. A.; Bork, R.; Boschi, V.; Bose, S.; Bossie, K.; Bouffanais,
Y.; Bozzi, A.; Bradaschia, C.; Brady, P. R.; Branchesi, M.; Brau,
J. E.; Briant, T.; Brillet, A.; Brinkmann, M.; Brisson, V.; Brockill,
P.; Broida, J. E.; Brooks, A. F.; Brown, D. A.; Brown, D. D.; Brunett,
S.; Buchanan, C. C.; Buikema, A.; Bulik, T.; Bulten, H. J.; Buonanno,
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Schlunder, P.; Schmidt, T.; Schneider, A.; Schoenen, S.; Schöneberg,
S.; Schumacher, L.; Seckel, D.; Seunarine, S.; Soedingrekso, J.;
Soldin, D.; Song, M.; Spiczak, G. M.; Spiering, C.; Stachurska, J.;
Stamatikos, M.; Stanev, T.; Stasik, A.; Stettner, J.; Steuer, A.;
Stezelberger, T.; Stokstad, R. G.; Stössl, A.; Strotjohann, N. L.;
Stuttard, T.; Sullivan, G. W.; Sutherland, M.; Taboada, I.; Tatar,
J.; Tenholt, F.; Ter-Antonyan, S.; Terliuk, A.; Tešić, G.; Tilav,
S.; Toale, P. A.; Tobin, M. N.; Toscano, S.; Tosi, D.; Tselengidou,
M.; Tung, C. F.; Turcati, A.; Turley, C. F.; Ty, B.; Unger, E.;
Usner, M.; Vandenbroucke, J.; Van Driessche, W.; van Eijndhoven, N.;
Vanheule, S.; van Santen, J.; Vehring, M.; Vogel, E.; Vraeghe, M.;
Walck, C.; Wallace, A.; Wallraff, M.; Wandler, F. D.; Wandkowsky,
N.; Waza, A.; Weaver, C.; Weiss, M. J.; Wendt, C.; Werthebach, J.;
Whelan, B. J.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams,
D. R.; Wills, L.; Wolf, M.; Wood, T. R.; Woolsey, E.; Woschnagg,
K.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yanez, J. P.; Yodh, G.; Yoshida,
S.; Yuan, T.; Zoll, M.; IceCube Collaboration; Balasubramanian, A.;
Mate, S.; Bhalerao, V.; Bhattacharya, D.; Vibhute, A.; Dewangan,
G. C.; Rao, A. R.; Vadawale, S. V.; AstroSat Cadmium Zinc Telluride
Imager Team; Svinkin, D. S.; Hurley, K.; Aptekar, R. L.; Frederiks,
D. D.; Golenetskii, S. V.; Kozlova, A. V.; Lysenko, A. L.; Oleynik,
Ph. P.; Tsvetkova, A. E.; Ulanov, M. V.; Cline, T.; IPN Collaboration;
Li, T. P.; Xiong, S. L.; Zhang, S. N.; Lu, F. J.; Song, L. M.; Cao,
X. L.; Chang, Z.; Chen, G.; Chen, L.; Chen, T. X.; Chen, Y.; Chen,
Y. B.; Chen, Y. P.; Cui, W.; Cui, W. W.; Deng, J. K.; Dong, Y. W.; Du,
Y. Y.; Fu, M. X.; Gao, G. H.; Gao, H.; Gao, M.; Ge, M. Y.; Gu, Y. D.;
Guan, J.; Guo, C. C.; Han, D. W.; Hu, W.; Huang, Y.; Huo, J.; Jia,
S. M.; Jiang, L. H.; Jiang, W. C.; Jin, J.; Jin, Y. J.; Li, B.; Li,
C. K.; Li, G.; Li, M. S.; Li, W.; Li, X.; Li, X. B.; Li, X. F.; Li,
Y. G.; Li, Z. J.; Li, Z. W.; Liang, X. H.; Liao, J. Y.; Liu, C. Z.;
Liu, G. Q.; Liu, H. W.; Liu, S. Z.; Liu, X. J.; Liu, Y.; Liu, Y. N.;
Lu, B.; Lu, X. F.; Luo, T.; Ma, X.; Meng, B.; Nang, Y.; Nie, J. Y.;
Ou, G.; Qu, J. L.; Sai, N.; Sun, L.; Tan, Y.; Tao, L.; Tao, W. H.;
Tuo, Y. L.; Wang, G. F.; Wang, H. Y.; Wang, J.; Wang, W. S.; Wang,
Y. S.; Wen, X. Y.; Wu, B. B.; Wu, M.; Xiao, G. C.; Xu, H.; Xu, Y. P.;
Yan, L. L.; Yang, J. W.; Yang, S.; Yang, Y. J.; Zhang, A. M.; Zhang,
C. L.; Zhang, C. M.; Zhang, F.; Zhang, H. M.; Zhang, J.; Zhang, Q.;
Zhang, S.; Zhang, T.; Zhang, W.; Zhang, W. C.; Zhang, W. Z.; Zhang,
Y.; Zhang, Y.; Zhang, Y. F.; Zhang, Y. J.; Zhang, Z.; Zhang, Z. L.;
Zhao, H. S.; Zhao, J. L.; Zhao, X. F.; Zheng, S. J.; Zhu, Y.; Zhu,
Y. X.; Zou, C. L.; Insight-HXMT Collaboration; Albert, A.; André,
M.; Anghinolfi, M.; Ardid, M.; Aubert, J. -J.; Aublin, J.; Avgitas,
T.; Baret, B.; Barrios-Martí, J.; Basa, S.; Belhorma, B.; Bertin, V.;
Biagi, S.; Bormuth, R.; Bourret, S.; Bouwhuis, M. C.; Brânzaş, H.;
Bruijn, R.; Brunner, J.; Busto, J.; Capone, A.; Caramete, L.; Carr,
J.; Celli, S.; Cherkaoui El Moursli, R.; Chiarusi, T.; Circella,
M.; Coelho, J. A. B.; Coleiro, A.; Coniglione, R.; Costantini, H.;
Coyle, P.; Creusot, A.; Díaz, A. F.; Deschamps, A.; De Bonis,
G.; Distefano, C.; Di Palma, I.; Domi, A.; Donzaud, C.; Dornic,
D.; Drouhin, D.; Eberl, T.; El Bojaddaini, I.; El Khayati, N.;
Elsässer, D.; Enzenhöfer, A.; Ettahiri, A.; Fassi, F.; Felis, I.;
Fusco, L. A.; Gay, P.; Giordano, V.; Glotin, H.; Grégoire, T.; Ruiz,
R. Gracia; Graf, K.; Hallmann, S.; van Haren, H.; Heijboer, A. J.;
Hello, Y.; Hernández-Rey, J. J.; Hössl, J.; Hofestädt, J.; Hugon,
C.; Illuminati, G.; James, C. W.; de Jong, M.; Jongen, M.; Kadler,
M.; Kalekin, O.; Katz, U.; Kiessling, D.; Kouchner, A.; Kreter, M.;
Kreykenbohm, I.; Kulikovskiy, V.; Lachaud, C.; Lahmann, R.; Lefèvre,
D.; Leonora, E.; Lotze, M.; Loucatos, S.; Marcelin, M.; Margiotta, A.;
Marinelli, A.; Martínez-Mora, J. A.; Mele, R.; Melis, K.; Michael,
T.; Migliozzi, P.; Moussa, A.; Navas, S.; Nezri, E.; Organokov, M.;
Păvălaş, G. E.; Pellegrino, C.; Perrina, C.; Piattelli, P.; Popa,
V.; Pradier, T.; Quinn, L.; Racca, C.; Riccobene, G.; Sánchez-Losa,
A.; Saldaña, M.; Salvadori, I.; Samtleben, D. F. E.; Sanguineti,
M.; Sapienza, P.; Sieger, C.; Spurio, M.; Stolarczyk, Th.; Taiuti,
M.; Tayalati, Y.; Trovato, A.; Turpin, D.; Tönnis, C.; Vallage, B.;
Van Elewyck, V.; Versari, F.; Vivolo, D.; Vizzoca, A.; Wilms, J.;
Zornoza, J. D.; Zúñiga, J.; ANTARES Collaboration; Beardmore, A. P.;
Breeveld, A. A.; Burrows, D. N.; Cenko, S. B.; Cusumano, G.; D'Aì, A.;
de Pasquale, M.; Emery, S. W. K.; Evans, P. A.; Giommi, P.; Gronwall,
C.; Kennea, J. A.; Krimm, H. A.; Kuin, N. P. M.; Lien, A.; Marshall,
F. E.; Melandri, A.; Nousek, J. A.; Oates, S. R.; Osborne, J. P.;
Pagani, C.; Page, K. L.; Palmer, D. M.; Perri, M.; Siegel, M. H.;
Sbarufatti, B.; Tagliaferri, G.; Tohuvavohu, A.; Swift Collaboration;
Tavani, M.; Verrecchia, F.; Bulgarelli, A.; Evangelista, Y.; Pacciani,
L.; Feroci, M.; Pittori, C.; Giuliani, A.; Del Monte, E.; Donnarumma,
I.; Argan, A.; Trois, A.; Ursi, A.; Cardillo, M.; Piano, G.; Longo,
F.; Lucarelli, F.; Munar-Adrover, P.; Fuschino, F.; Labanti, C.;
Marisaldi, M.; Minervini, G.; Fioretti, V.; Parmiggiani, N.; Gianotti,
F.; Trifoglio, M.; Di Persio, G.; Antonelli, L. A.; Barbiellini, G.;
Caraveo, P.; Cattaneo, P. W.; Costa, E.; Colafrancesco, S.; D'Amico,
F.; Ferrari, A.; Morselli, A.; Paoletti, F.; Picozza, P.; Pilia,
M.; Rappoldi, A.; Soffitta, P.; Vercellone, S.; AGILE Team; Foley,
R. J.; Coulter, D. A.; Kilpatrick, C. D.; Drout, M. R.; Piro, A. L.;
Shappee, B. J.; Siebert, M. R.; Simon, J. D.; Ulloa, N.; Kasen, D.;
Madore, B. F.; Murguia-Berthier, A.; Pan, Y. -C.; Prochaska, J. X.;
Ramirez-Ruiz, E.; Rest, A.; Rojas-Bravo, C.; 1M2H Team; Berger, E.;
Soares-Santos, M.; Annis, J.; Alexander, K. D.; Allam, S.; Balbinot,
E.; Blanchard, P.; Brout, D.; Butler, R. E.; Chornock, R.; Cook,
E. R.; Cowperthwaite, P.; Diehl, H. T.; Drlica-Wagner, A.; Drout,
M. R.; Durret, F.; Eftekhari, T.; Finley, D. A.; Fong, W.; Frieman,
J. A.; Fryer, C. L.; García-Bellido, J.; Gruendl, R. A.; Hartley,
W.; Herner, K.; Kessler, R.; Lin, H.; Lopes, P. A. A.; Lourenço,
A. C. C.; Margutti, R.; Marshall, J. L.; Matheson, T.; Medina, G. E.;
Metzger, B. D.; Muñoz, R. R.; Muir, J.; Nicholl, M.; Nugent, P.;
Palmese, A.; Paz-Chinchón, F.; Quataert, E.; Sako, M.; Sauseda, M.;
Schlegel, D. J.; Scolnic, D.; Secco, L. F.; Smith, N.; Sobreira, F.;
Villar, V. A.; Vivas, A. K.; Wester, W.; Williams, P. K. G.; Yanny,
B.; Zenteno, A.; Zhang, Y.; Abbott, T. M. C.; Banerji, M.; Bechtol,
K.; Benoit-Lévy, A.; Bertin, E.; Brooks, D.; Buckley-Geer, E.; Burke,
D. L.; Capozzi, D.; Carnero Rosell, A.; Carrasco Kind, M.; Castander,
F. J.; Crocce, M.; Cunha, C. E.; D'Andrea, C. B.; da Costa, L. N.;
Davis, C.; DePoy, D. L.; Desai, S.; Dietrich, J. P.; Eifler, T. F.;
Fernandez, E.; Flaugher, B.; Fosalba, P.; Gaztanaga, E.; Gerdes,
D. W.; Giannantonio, T.; Goldstein, D. A.; Gruen, D.; Gschwend, J.;
Gutierrez, G.; Honscheid, K.; James, D. J.; Jeltema, T.; Johnson,
M. W. G.; Johnson, M. D.; Kent, S.; Krause, E.; Kron, R.; Kuehn, K.;
Lahav, O.; Lima, M.; Maia, M. A. G.; March, M.; Martini, P.; McMahon,
R. G.; Menanteau, F.; Miller, C. J.; Miquel, R.; Mohr, J. J.; Nichol,
R. C.; Ogando, R. L. C.; Plazas, A. A.; Romer, A. K.; Roodman, A.;
Rykoff, E. S.; Sanchez, E.; Scarpine, V.; Schindler, R.; Schubnell,
M.; Sevilla-Noarbe, I.; Sheldon, E.; Smith, M.; Smith, R. C.; Stebbins,
A.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thomas, R. C.; Troxel,
M. A.; Tucker, D. L.; Vikram, V.; Walker, A. R.; Wechsler, R. H.;
Weller, J.; Carlin, J. L.; Gill, M. S. S.; Li, T. S.; Marriner, J.;
Neilsen, E.; Dark Energy Camera GW-EM Collaboration; DES Collaboration;
Haislip, J. B.; Kouprianov, V. V.; Reichart, D. E.; Sand, D. J.;
Tartaglia, L.; Valenti, S.; Yang, S.; DLT40 Collaboration; Benetti,
S.; Brocato, E.; Campana, S.; Cappellaro, E.; Covino, S.; D'Avanzo,
P.; D'Elia, V.; Getman, F.; Ghirlanda, G.; Ghisellini, G.; Limatola,
L.; Nicastro, L.; Palazzi, E.; Pian, E.; Piranomonte, S.; Possenti,
A.; Rossi, A.; Salafia, O. S.; Tomasella, L.; Amati, L.; Antonelli,
L. A.; Bernardini, M. G.; Bufano, F.; Capaccioli, M.; Casella, P.;
Dadina, M.; De Cesare, G.; Di Paola, A.; Giuffrida, G.; Giunta,
A.; Israel, G. L.; Lisi, M.; Maiorano, E.; Mapelli, M.; Masetti,
N.; Pescalli, A.; Pulone, L.; Salvaterra, R.; Schipani, P.; Spera,
M.; Stamerra, A.; Stella, L.; Testa, V.; Turatto, M.; Vergani, D.;
Aresu, G.; Bachetti, M.; Buffa, F.; Burgay, M.; Buttu, M.; Caria,
T.; Carretti, E.; Casasola, V.; Castangia, P.; Carboni, G.; Casu,
S.; Concu, R.; Corongiu, A.; Deiana, G. L.; Egron, E.; Fara, A.;
Gaudiomonte, F.; Gusai, V.; Ladu, A.; Loru, S.; Leurini, S.; Marongiu,
L.; Melis, A.; Melis, G.; Migoni, Carlo; Milia, Sabrina; Navarrini,
Alessandro; Orlati, A.; Ortu, P.; Palmas, S.; Pellizzoni, A.; Perrodin,
D.; Pisanu, T.; Poppi, S.; Righini, S.; Saba, A.; Serra, G.; Serrau,
M.; Stagni, M.; Surcis, G.; Vacca, V.; Vargiu, G. P.; Hunt, L. K.;
Jin, Z. P.; Klose, S.; Kouveliotou, C.; Mazzali, P. A.; Møller, P.;
Nava, L.; Piran, T.; Selsing, J.; Vergani, S. D.; Wiersema, K.; Toma,
K.; Higgins, A. B.; Mundell, C. G.; di Serego Alighieri, S.; Gótz,
D.; Gao, W.; Gomboc, A.; Kaper, L.; Kobayashi, S.; Kopac, D.; Mao,
J.; Starling, R. L. C.; Steele, I.; van der Horst, A. J.; GRAWITA:
GRAvitational Wave Inaf TeAm; Acero, F.; Atwood, W. B.; Baldini,
L.; Barbiellini, G.; Bastieri, D.; Berenji, B.; Bellazzini, R.;
Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonino, R.; Bottacini,
E.; Bregeon, J.; Buehler, R.; Buson, S.; Cameron, R. A.; Caputo, R.;
Caraveo, P. A.; Cavazzuti, E.; Chekhtman, A.; Cheung, C. C.; Chiang,
J.; Ciprini, S.; Cohen-Tanugi, J.; Cominsky, L. R.; Costantin, D.;
Cuoco, A.; D'Ammando, F.; de Palma, F.; Digel, S. W.; Di Lalla,
N.; Di Mauro, M.; Di Venere, L.; Dubois, R.; Fegan, S. J.; Focke,
W. B.; Franckowiak, A.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano,
F.; Gasparrini, D.; Giglietto, N.; Giordano, F.; Giroletti, M.;
Glanzman, T.; Green, D.; Grondin, M. -H.; Guillemot, L.; Guiriec,
S.; Harding, A. K.; Horan, D.; Jóhannesson, G.; Kamae, T.; Kensei,
S.; Kuss, M.; La Mura, G.; Latronico, L.; Lemoine-Goumard, M.;
Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Magill,
J. D.; Maldera, S.; Manfreda, A.; Mazziotta, M. N.; McEnery, J. E.;
Meyer, M.; Michelson, P. F.; Mirabal, N.; Monzani, M. E.; Moretti,
E.; Morselli, A.; Moskalenko, I. V.; Negro, M.; Nuss, E.; Ojha, R.;
Omodei, N.; Orienti, M.; Orlando, E.; Palatiello, M.; Paliya, V. S.;
Paneque, D.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Principe, G.;
Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer,
O.; Reposeur, T.; Rochester, L. S.; Saz Parkinson, P. M.; Sgrò, C.;
Siskind, E. J.; Spada, F.; Spandre, G.; Suson, D. J.; Takahashi, M.;
Tanaka, Y.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo,
L.; Torres, D. F.; Torresi, E.; Troja, E.; Venters, T. M.; Vianello,
G.; Zaharijas, G.; Fermi Large Area Telescope Collaboration; Allison,
J. R.; Bannister, K. W.; Dobie, D.; Kaplan, D. L.; Lenc, E.; Lynch,
C.; Murphy, T.; Sadler, E. M.; Australia Telescope Compact Array,
ATCA:; Hotan, A.; James, C. W.; Oslowski, S.; Raja, W.; Shannon,
R. M.; Whiting, M.; Australian SKA Pathfinder, ASKAP:; Arcavi,
I.; Howell, D. A.; McCully, C.; Hosseinzadeh, G.; Hiramatsu, D.;
Poznanski, D.; Barnes, J.; Zaltzman, M.; Vasylyev, S.; Maoz, D.; Las
Cumbres Observatory Group; Cooke, J.; Bailes, M.; Wolf, C.; Deller,
A. T.; Lidman, C.; Wang, L.; Gendre, B.; Andreoni, I.; Ackley, K.;
Pritchard, T. A.; Bessell, M. S.; Chang, S. -W.; Möller, A.; Onken,
C. A.; Scalzo, R. A.; Ridden-Harper, R.; Sharp, R. G.; Tucker, B. E.;
Farrell, T. J.; Elmer, E.; Johnston, S.; Venkatraman Krishnan, V.;
Keane, E. F.; Green, J. A.; Jameson, A.; Hu, L.; Ma, B.; Sun, T.;
Wu, X.; Wang, X.; Shang, Z.; Hu, Y.; Ashley, M. C. B.; Yuan, X.; Li,
X.; Tao, C.; Zhu, Z.; Zhang, H.; Suntzeff, N. B.; Zhou, J.; Yang, J.;
Orange, B.; Morris, D.; Cucchiara, A.; Giblin, T.; Klotz, A.; Staff,
J.; Thierry, P.; Schmidt, B. P.; OzGrav; (Deeper, DWF; Wider; program,
Faster; AST3; CAASTRO Collaborations; Tanvir, N. R.; Levan, A. J.;
Cano, Z.; de Ugarte-Postigo, A.; González-Fernández, C.; Greiner,
J.; Hjorth, J.; Irwin, M.; Krühler, T.; Mandel, I.; Milvang-Jensen,
B.; O'Brien, P.; Rol, E.; Rosetti, S.; Rosswog, S.; Rowlinson, A.;
Steeghs, D. T. H.; Thöne, C. C.; Ulaczyk, K.; Watson, D.; Bruun,
S. H.; Cutter, R.; Figuera Jaimes, R.; Fujii, Y. I.; Fruchter, A. S.;
Gompertz, B.; Jakobsson, P.; Hodosan, G.; Jèrgensen, U. G.; Kangas,
T.; Kann, D. A.; Rabus, M.; Schrøder, S. L.; Stanway, E. R.; Wijers,
R. A. M. J.; VINROUGE Collaboration; Lipunov, V. M.; Gorbovskoy, E. S.;
Kornilov, V. G.; Tyurina, N. V.; Balanutsa, P. V.; Kuznetsov, A. S.;
Vlasenko, D. M.; Podesta, R. C.; Lopez, C.; Podesta, F.; Levato,
H. O.; Saffe, C.; Mallamaci, C. C.; Budnev, N. M.; Gress, O. A.;
Kuvshinov, D. A.; Gorbunov, I. A.; Vladimirov, V. V.; Zimnukhov,
D. S.; Gabovich, A. V.; Yurkov, V. V.; Sergienko, Yu. P.; Rebolo,
R.; Serra-Ricart, M.; Tlatov, A. G.; Ishmuhametova, Yu. V.; MASTER
Collaboration; Abe, F.; Aoki, K.; Aoki, W.; Asakura, Y.; Baar, S.;
Barway, S.; Bond, I. A.; Doi, M.; Finet, F.; Fujiyoshi, T.; Furusawa,
H.; Honda, S.; Itoh, R.; Kanda, N.; Kawabata, K. S.; Kawabata, M.; Kim,
J. H.; Koshida, S.; Kuroda, D.; Lee, C. -H.; Liu, W.; Matsubayashi,
K.; Miyazaki, S.; Morihana, K.; Morokuma, T.; Motohara, K.; Murata,
K. L.; Nagai, H.; Nagashima, H.; Nagayama, T.; Nakaoka, T.; Nakata,
F.; Ohsawa, R.; Ohshima, T.; Ohta, K.; Okita, H.; Saito, T.; Saito,
Y.; Sako, S.; Sekiguchi, Y.; Sumi, T.; Tajitsu, A.; Takahashi,
J.; Takayama, M.; Tamura, Y.; Tanaka, I.; Tanaka, M.; Terai, T.;
Tominaga, N.; Tristram, P. J.; Uemura, M.; Utsumi, Y.; Yamaguchi,
M. S.; Yasuda, N.; Yoshida, M.; Zenko, T.; J-GEM; Adams, S. M.;
Anupama, G. C.; Bally, J.; Barway, S.; Bellm, E.; Blagorodnova, N.;
Cannella, C.; Chandra, P.; Chatterjee, D.; Clarke, T. E.; Cobb, B. E.;
Cook, D. O.; Copperwheat, C.; De, K.; Emery, S. W. K.; Feindt, U.;
Foster, K.; Fox, O. D.; Frail, D. A.; Fremling, C.; Frohmaier, C.;
Garcia, J. A.; Ghosh, S.; Giacintucci, S.; Goobar, A.; Gottlieb, O.;
Grefenstette, B. W.; Hallinan, G.; Harrison, F.; Heida, M.; Helou,
G.; Ho, A. Y. Q.; Horesh, A.; Hotokezaka, K.; Ip, W. -H.; Itoh, R.;
Jacobs, Bob; Jencson, J. E.; Kasen, D.; Kasliwal, M. M.; Kassim,
N. E.; Kim, H.; Kiran, B. S.; Kuin, N. P. M.; Kulkarni, S. R.;
Kupfer, T.; Lau, R. M.; Madsen, K.; Mazzali, P. A.; Miller, A. A.;
Miyasaka, H.; Mooley, K.; Myers, S. T.; Nakar, E.; Ngeow, C. -C.;
Nugent, P.; Ofek, E. O.; Palliyaguru, N.; Pavana, M.; Perley, D. A.;
Peters, W. M.; Pike, S.; Piran, T.; Qi, H.; Quimby, R. M.; Rana, J.;
Rosswog, S.; Rusu, F.; Sadler, E. M.; Van Sistine, A.; Sollerman, J.;
Xu, Y.; Yan, L.; Yatsu, Y.; Yu, P. -C.; Zhang, C.; Zhao, W.; GROWTH;
JAGWAR; Caltech-NRAO; TTU-NRAO; NuSTAR Collaborations; Chambers,
K. C.; Huber, M. E.; Schultz, A. S. B.; Bulger, J.; Flewelling, H.;
Magnier, E. A.; Lowe, T. B.; Wainscoat, R. J.; Waters, C.; Willman,
M.; Pan-STARRS; Ebisawa, K.; Hanyu, C.; Harita, S.; Hashimoto, T.;
Hidaka, K.; Hori, T.; Ishikawa, M.; Isobe, N.; Iwakiri, W.; Kawai,
H.; Kawai, N.; Kawamuro, T.; Kawase, T.; Kitaoka, Y.; Makishima,
K.; Matsuoka, M.; Mihara, T.; Morita, T.; Morita, K.; Nakahira, S.;
Nakajima, M.; Nakamura, Y.; Negoro, H.; Oda, S.; Sakamaki, A.; Sasaki,
R.; Serino, M.; Shidatsu, M.; Shimomukai, R.; Sugawara, Y.; Sugita,
S.; Sugizaki, M.; Tachibana, Y.; Takao, Y.; Tanimoto, A.; Tomida, H.;
Tsuboi, Y.; Tsunemi, H.; Ueda, Y.; Ueno, S.; Yamada, S.; Yamaoka,
K.; Yamauchi, M.; Yatabe, F.; Yoneyama, T.; Yoshii, T.; MAXI Team;
Coward, D. M.; Crisp, H.; Macpherson, D.; Andreoni, I.; Laugier,
R.; Noysena, K.; Klotz, A.; Gendre, B.; Thierry, P.; Turpin, D.;
Consortium, TZAC; Im, M.; Choi, C.; Kim, J.; Yoon, Y.; Lim, G.; Lee,
S. -K.; Lee, C. -U.; Kim, S. -L.; Ko, S. -W.; Joe, J.; Kwon, M. -K.;
Kim, P. -J.; Lim, S. -K.; Choi, J. -S.; KU Collaboration; Fynbo,
J. P. U.; Malesani, D.; Xu, D.; Optical Telescope, Nordic; Smartt,
S. J.; Jerkstrand, A.; Kankare, E.; Sim, S. A.; Fraser, M.; Inserra,
C.; Maguire, K.; Leloudas, G.; Magee, M.; Shingles, L. J.; Smith,
K. W.; Young, D. R.; Kotak, R.; Gal-Yam, A.; Lyman, J. D.; Homan,
D. S.; Agliozzo, C.; Anderson, J. P.; Angus, C. R.; Ashall, C.;
Barbarino, C.; Bauer, F. E.; Berton, M.; Botticella, M. T.; Bulla,
M.; Cannizzaro, G.; Cartier, R.; Cikota, A.; Clark, P.; De Cia,
A.; Della Valle, M.; Dennefeld, M.; Dessart, L.; Dimitriadis, G.;
Elias-Rosa, N.; Firth, R. E.; Flörs, A.; Frohmaier, C.; Galbany, L.;
González-Gaitán, S.; Gromadzki, M.; Gutiérrez, C. P.; Hamanowicz,
A.; Harmanen, J.; Heintz, K. E.; Hernandez, M. -S.; Hodgkin, S. T.;
Hook, I. M.; Izzo, L.; James, P. A.; Jonker, P. G.; Kerzendorf, W. E.;
Kostrzewa-Rutkowska, Z.; Kromer, M.; Kuncarayakti, H.; Lawrence,
A.; Manulis, I.; Mattila, S.; McBrien, O.; Müller, A.; Nordin, J.;
O'Neill, D.; Onori, F.; Palmerio, J. T.; Pastorello, A.; Patat, F.;
Pignata, G.; Podsiadlowski, P.; Razza, A.; Reynolds, T.; Roy, R.;
Ruiter, A. J.; Rybicki, K. A.; Salmon, L.; Pumo, M. L.; Prentice,
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B.; Vos, J.; Walton, N. A.; Wright, D. E.; Wyrzykowski, Ł.; Yaron,
O.; pre="(">ePESSTO, <author; Chen, T. -W.; Krühler, T.; Schady,
P.; Wiseman, P.; Greiner, J.; Rau, A.; Schweyer, T.; Klose, S.;
Nicuesa Guelbenzu, A.; GROND; Palliyaguru, N. T.; Tech University,
Texas; Shara, M. M.; Williams, T.; Vaisanen, P.; Potter, S. B.; Romero
Colmenero, E.; Crawford, S.; Buckley, D. A. H.; Mao, J.; SALT Group;
Díaz, M. C.; Macri, L. M.; García Lambas, D.; Mendes de Oliveira,
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P.; Colazo, C.; Costa-Duarte, M. V.; Cuevas Larenas, H.; Domínguez
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C.; Ramírez Rivera, A.; Renzi, V.; Riguccini, L.; Ríos-López, E.;
Rodriguez, H.; Sampedro, L.; Schneiter, M.; Sodré, L.; Starck, M.;
Torres-Flores, S.; Tornatore, M.; Zadrożny, A.; Castillo, M.; TOROS:
Transient Robotic Observatory of South Collaboration; Castro-Tirado,
A. J.; Tello, J. C.; Hu, Y. -D.; Zhang, B. -B.; Cunniffe, R.;
Castellón, A.; Hiriart, D.; Caballero-García, M. D.; Jelínek,
M.; Kubánek, P.; Pérez del Pulgar, C.; Park, I. H.; Jeong, S.;
Castro Cerón, J. M.; Pandey, S. B.; Yock, P. C.; Querel, R.; Fan,
Y.; Wang, C.; BOOTES Collaboration; Beardsley, A.; Brown, I. S.;
Crosse, B.; Emrich, D.; Franzen, T.; Gaensler, B. M.; Horsley,
L.; Johnston-Hollitt, M.; Kenney, D.; Morales, M. F.; Pallot, D.;
Sokolowski, M.; Steele, K.; Tingay, S. J.; Trott, C. M.; Walker, M.;
Wayth, R.; Williams, A.; Wu, C.; Murchison Widefield Array, MWA:;
Yoshida, A.; Sakamoto, T.; Kawakubo, Y.; Yamaoka, K.; Takahashi,
I.; Asaoka, Y.; Ozawa, S.; Torii, S.; Shimizu, Y.; Tamura, T.;
Ishizaki, W.; Cherry, M. L.; Ricciarini, S.; Penacchioni, A. V.;
Marrocchesi, P. S.; CALET Collaboration; Pozanenko, A. S.; Volnova,
A. A.; Mazaeva, E. D.; Minaev, P. Yu.; Krugov, M. A.; Kusakin, A. V.;
Reva, I. V.; Moskvitin, A. S.; Rumyantsev, V. V.; Inasaridze, R.;
Klunko, E. V.; Tungalag, N.; Schmalz, S. E.; Burhonov, O.; IKI-GW
Follow-up Collaboration; Abdalla, H.; Abramowski, A.; Aharonian, F.;
Ait Benkhali, F.; Angüner, E. O.; Arakawa, M.; Arrieta, M.; Aubert,
P.; Backes, M.; Balzer, A.; Barnard, M.; Becherini, Y.; Becker Tjus,
J.; Berge, D.; Bernhard, S.; Bernlöhr, K.; Blackwell, R.; Böttcher,
M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bordas, P.; Bregeon, J.;
Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Capasso, M.;
Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.; Chakraborty, N.;
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Garrigoux, T.; Gaté, F.; Giavitto, G.; Giebels, B.; Glawion, D.;
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I.; Kastendieck, M. A.; Katarzyński, K.; Katsuragawa, M.; Kerszberg,
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Medina-Tanco, G.; Melo, D.; Menshikov, A.; Merenda, K. -D.; Michal,
S.; Micheletti, M. I.; Middendorf, L.; Miramonti, L.; Mitrica, B.;
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E. J.; Querchfeld, S.; Quinn, S.; Ramos-Pollan, R.; Rautenberg, J.;
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A.; Suarez, F.; Suarez-Durán, M.; Sudholz, T.; Suomijärvi, T.;
Supanitsky, A. D.; Šupík, J.; Swain, J.; Szadkowski, Z.; Taboada, A.;
Taborda, O. A.; Timmermans, C.; Todero Peixoto, C. J.; Tomankova, L.;
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2017ApJ...848L..12A Altcode: 2017arXiv171005833L
On 2017 August 17 a binary neutron star coalescence candidate (later
designated GW170817) with merger time 12:41:04 UTC was observed
through gravitational waves by the Advanced LIGO and Advanced Virgo
detectors. The Fermi Gamma-ray Burst Monitor independently detected a
gamma-ray burst (GRB 170817A) with a time delay of ∼ 1.7 {{s}} with
respect to the merger time. From the gravitational-wave signal, the
source was initially localized to a sky region of 31 deg<SUP>2</SUP>
at a luminosity distance of {40}<SUB>-8</SUB><SUP>+8</SUP> Mpc and
with component masses consistent with neutron stars. The component
masses were later measured to be in the range 0.86 to 2.26 {M}<SUB>⊙
</SUB>. An extensive observing campaign was launched across the
electromagnetic spectrum leading to the discovery of a bright optical
transient (SSS17a, now with the IAU identification of AT 2017gfo) in
NGC 4993 (at ∼ 40 {{Mpc}}) less than 11 hours after the merger by the
One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The
optical transient was independently detected by multiple teams
within an hour. Subsequent observations targeted the object and its
environment. Early ultraviolet observations revealed a blue transient
that faded within 48 hours. Optical and infrared observations showed
a redward evolution over ∼10 days. Following early non-detections,
X-ray and radio emission were discovered at the transient's position ∼
9 and ∼ 16 days, respectively, after the merger. Both the X-ray and
radio emission likely arise from a physical process that is distinct
from the one that generates the UV/optical/near-infrared emission. No
ultra-high-energy gamma-rays and no neutrino candidates consistent with
the source were found in follow-up searches. These observations support
the hypothesis that GW170817 was produced by the merger of two neutron
stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A)
and a kilonova/macronova powered by the radioactive decay of r-process
nuclei synthesized in the ejecta. <P />Any correspondence should be
addressed to .
---------------------------------------------------------
Title: Observational Evidence of a Flux Rope within a Sunspot Umbra
Authors: Guglielmino, Salvo L.; Romano, Paolo; Zuccarello, Francesca
2017ApJ...846L..16G Altcode: 2017arXiv170802398G
We observed an elongated filamentary bright structure inside the umbra
of the big sunspot in active region NOAA 12529, which differs from
the light bridges usually observed in sunspots for its morphology,
magnetic configuration, and velocity field. We used observations
taken with the Solar Dynamic Observatory satellite to characterize
this feature. Its lifetime is 5 days, during which it reaches a
maximum length of about 30″. In the maps of the vertical component
of the photospheric magnetic field, a portion of the feature has a
polarity opposite to that of the hosting sunspot. At the same time,
in the entire feature the horizontal component of the magnetic field is
about 2000 G, substantially stronger than in the surrounding penumbral
filaments. Doppler velocity maps reveal the presence of both upward
and downward plasma motions along the structure at the photospheric
level. Moreover, looking at the chromospheric level, we noted that it
is located in a region corresponding to the edge of a small filament
that seems rooted in the sunspot umbra. Therefore, we interpreted the
bright structure as the photospheric counterpart of a flux rope touching
the sunspot and giving rise to penumbral-like filaments in the umbra.
---------------------------------------------------------
Title: Comparison of different populations of granular features in
the solar photosphere
Authors: Falco, M.; Puglisi, G.; Guglielmino, S. L.; Romano, P.;
Ermolli, I.; Zuccarello, F.
2017A&A...605A..87F Altcode:
Context. The granulation is the most visible manifestation of
convective motions occurring in the uppermost layers of the solar
convection zone. Strong magnetic fields hinder these motions, but the
appearance of bright structures such as umbral dots (UDs) and light
bridges (LBs) in sunspots also shows that in strong magnetic field
regions, the convection is not completely suppressed. <BR /> Aims:
We aim to investigate the properties of the granules identified by
a new segmentation algorithm in regions characterized by different
magnetic field strength, in order to improve the current knowledge
of the mechanism behind the appearance of the different bright
structures in sunspots. <BR /> Methods: We analyzed data acquired by
the CRisp Imaging SpectroPolarimeter at the Swedish Solar Telescope
on 6 August 2011 relevant to a large sunspot with a LB observed in
NOAA AR 11263. We applied a new segmentation algorithm to the data
acquired along the Fe I 630.15 nm line. <BR /> Results: We found that
the granules in the LB have a diameter between 0.̋22 and 0.̋99, that
is, smaller than the granules in a nearby plage region (PL) and similar
to those of the UDs. We observed values of the mean continuum intensity
between 0.42 I<SUB>c</SUB> and 0.98 I<SUB>c</SUB> for the LB granules,
which are similar to those of the UDs. PL granules have higher values,
probably reflecting different conditions of the plasma convection. Mean
Doppler velocity and mean magnetic field strength have been studied and
even for these physical parameters we found similar values between LB
granules and UDs. <BR /> Conclusions: Different values for the physical
properties analyzed have been found between the granules of the PL
and LB granules of the three analyzed solar regions. In particular,
we show that the granules in PL and sunspot regions have different
physical properties. This clearly depends on the different physical
conditions of the regions where these two kind of granular structures
are embedded. We also confirm the recent findings on the similarity
between granules in PL and quiet Sun regions. We show values of the
various physical quantities analyzed in PL granules in agreement with
those reported in the literature for quiet Sun granules. Finally, a
noteworthy result is that the granules observed in the faint LB have
physical properties similar to those found for UDs.
---------------------------------------------------------
Title: Observation of a large-scale anisotropy in the arrival
directions of cosmic rays above 8 × 10<SUP>18</SUP> eV
Authors: Pierre Auger Collaboration; Aab, A.; Abreu, P.; Aglietta,
M.; Samarai, I. Al; Albuquerque, I. F. M.; Allekotte, I.; Almela,
A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Anastasi, G. A.;
Anchordoqui, L.; Andrada, B.; Andringa, S.; Aramo, C.; Arqueros, F.;
Arsene, N.; Asorey, H.; Assis, P.; Aublin, J.; Avila, G.; Badescu,
A. M.; Balaceanu, A.; Barbato, F.; Barreira Luz, R. J.; Beatty, J. J.;
Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou,
X.; Biermann, P. L.; Billoir, P.; Biteau, J.; Blaess, S. G.; Blanco,
A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Botti, A. M.; Brack, J.; Brancus, I.; Bretz, T.;
Bridgeman, A.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink,
S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, L.; Cancio, A.;
Canfora, F.; Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.;
Cazon, L.; Chavez, A. G.; Chinellato, J. A.; Chudoba, J.; Clay, R. W.;
Cobos, A.; Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.;
Conceição, R.; Consolati, G.; Contreras, F.; Cooper, M. J.; Coutu,
S.; Covault, C. E.; Cronin, J.; D'Amico, S.; Daniel, B.; Dasso, S.;
Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; de Jong, S. J.; De
Mauro, G.; de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.;
de Souza, V.; Debatin, J.; Deligny, O.; Di Giulio, C.; Di Matteo,
A.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.;
Dorosti, Q.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.;
Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.;
Etchegoyen, A.; Falcke, H.; Farrar, G.; Fauth, A. C.; Fazzini, N.;
Fenu, F.; Fick, B.; Figueira, J. M.; Filipčič, A.; Fratu, O.; Freire,
M. M.; Fujii, T.; Fuster, A.; Gaior, R.; García, B.; Garcia-Pinto,
D.; Gaté, F.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari,
U.; Giammarchi, M.; Giller, M.; Głas, D.; Glaser, C.; Golup, G.;
Gómez Berisso, M.; Gómez Vitale, P. F.; González, N.; Gorgi, A.;
Gorham, P.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.;
Hampel, M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Harton, J. L.;
Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill,
G. C.; Hojvat, C.; Holt, E.; Homola, P.; Hörandel, J. R.; Horvath,
P.; Hrabovský, M.; Huege, T.; Hulsman, J.; Insolia, A.; Isar, P. G.;
Jandt, I.; Jansen, S.; Johnsen, J. A.; Josebachuili, M.; Jurysek, J.;
Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Katkov, I.; Keilhauer, B.;
Kemmerich, N.; Kemp, E.; Kemp, J.; Kieckhafer, R. M.; Klages, H. O.;
Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Kuempel, D.;
Kukec Mezek, G.; Kunka, N.; Kuotb Awad, A.; LaHurd, D.; Lauscher,
M.; Legumina, R.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.;
Lhenry-Yvon, I.; Link, K.; Lo Presti, D.; Lopes, L.; López, R.;
López Casado, A.; Luce, Q.; Lucero, A.; Malacari, M.; Mallamaci, M.;
Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Mariş, I. C.; Marsella, G.;
Martello, D.; Martinez, H.; Martínez Bravo, O.; Masías Meza, J. J.;
Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.; Matthiae,
G.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Melo,
D.; Menshikov, A.; Merenda, K. -D.; Michal, S.; Micheletti, M. I.;
Middendorf, L.; Miramonti, L.; Mitrica, B.; Mockler, D.; Mollerach,
S.; Montanet, F.; Morello, C.; Mostafá, M.; Müller, A. L.; Müller,
G.; Muller, M. A.; Müller, S.; Mussa, R.; Naranjo, I.; Nellen, L.;
Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.; Niemietz,
L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.;
Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Palatka, M.;
Pallotta, J.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.; Pech,
M.; Pedreira, F.; Pkala, J.; Pelayo, R.; Peña-Rodriguez, J.; Pereira,
L. A. S.; Perlín, M.; Perrone, L.; Peters, C.; Petrera, S.; Phuntsok,
J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello,
V.; Platino, M.; Plum, M.; Porowski, C.; Prado, R. R.; Privitera, P.;
Prouza, M.; Quel, E. J.; Querchfeld, S.; Quinn, S.; Ramos-Pollan,
R.; Rautenberg, J.; Ravignani, D.; Revenu, B.; Ridky, J.; Riehn,
F.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.;
Rodriguez Fernandez, G.; Rodriguez Rojo, J.; Rogozin, D.; Roncoroni,
M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl, P.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santos, E. M.; Santos,
E.; Sarazin, F.; Sarmento, R.; Sarmiento, C. A.; Sato, R.; Schauer,
M.; Scherini, V.; Schieler, H.; Schimp, M.; Schmidt, D.; Scholten,
O.; Schovánek, P.; Schröder, F. G.; Schulz, A.; Schumacher, J.;
Sciutto, S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.;
Sigl, G.; Silli, G.; Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow,
G. R.; Sommers, P.; Sonntag, S.; Sorokin, J.; Squartini, R.; Stanca,
D.; Stanič, S.; Stasielak, J.; Stassi, P.; Strafella, F.; Suarez,
F.; Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky,
A. D.; Šupík, J.; Swain, J.; Szadkowski, Z.; Taboada, A.; Taborda,
O. A.; Tapia, A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Tomankova, L.; Tomé, B.; Torralba Elipe, G.; Travnicek, P.;
Trini, M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.;
Valiño, I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg,
A. M.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.;
Vázquez, R. A.; Veberič, D.; Ventura, C.; Vergara Quispe, I. D.;
Verzi, V.; Vicha, J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.;
Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke,
L.; Wilczyński, H.; Wirtz, M.; Wittkowski, D.; Wundheiler, B.; Yang,
L.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zepeda, A.;
Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello, F.
2017Sci...357.1266P Altcode: 2017Sci...357.1266.; 2017arXiv170907321T
Cosmic rays are high-energy particles arriving from space; some
have energies far beyond those that human-made particle accelerators
can achieve. The sources of higher-energy cosmic rays remain under
debate, although we know that lower-energy cosmic rays come from the
solar wind. The Pierre Auger Collaboration reports the observation of
thousands of cosmic rays with ultrahigh energies of several exa-electron
volts (about a Joule per particle), arriving in a slightly dipolar
distribution (see the Perspective by Gallagher and Halzen). The
direction of the rays indicates that the particles originated in other
galaxies and not from nearby sources within our own Milky Way Galaxy.
---------------------------------------------------------
Title: The Pierre Auger Observatory: Contributions to the 35th
International Cosmic Ray Conference (ICRC 2017)
Authors: The Pierre Auger Collaboration; Aab, A.; Abreu, P.; Aglietta,
M.; Albuquerque, I. F. M.; Allekotte, I.; Almela, A.; Alvarez
Castillo, J.; Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.;
Andrada, B.; Andringa, S.; Aramo, C.; Arsene, N.; Asorey, H.; Assis,
P.; Aublin, J.; Avila, G.; Badescu, A. M.; Balaceanu, A.; Barbato,
F.; Barreira Luz, R. J.; Becker, K. H.; Bellido, J. A.; Berat, C.;
Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Biteau, J.; Blaess,
S. G.; Blanco, A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli,
D.; Bonifazi, C.; Borodai, N.; Botti, A. M.; Brack, J.; Brancus,
I.; Bretz, T.; Bridgeman, A.; Briechle, F. L.; Buchholz, P.; Bueno,
A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, B.;
Caccianiga, L.; Cancio, A.; Canfora, F.; Caramete, L.; Caruso, R.;
Castellina, A.; Catalani, F.; Cataldi, G.; Cazon, L.; Chavez, A. G.;
Chinellato, J. A.; Chudoba, J.; Clay, R. W.; Cobos, A.; Colalillo,
R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição, R.;
Consolati, G.; Consolati, G.; Contreras, F.; Cooper, M. J.; Coutu,
S.; Covault, C. E.; Cronin, J.; D'Amico, S.; Daniel, B.; Dasso, S.;
Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; de Jong, S. J.; De
Mauro, G.; de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.;
de Souza, V.; Debatin, J.; Deligny, O.; Díaz Castro, M. L.; Diogo,
F.; Dobrigkeit, C.; D'Olivo, J. C.; Dorosti, Q.; dos Anjos, R. C.;
Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.; Erdmann, M.; Erfani, M.;
Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Falcke, H.; Farmer, J.;
Farrar, G.; Fauth, A. C.; Fazzini, N.; Fenu, F.; Fick, B.; Figueira,
J. M.; Filipčič, A.; Freire, M. M.; Fujii, T.; Fuster, A.; Gaïor,
R.; García, B.; Gaté, F.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia,
P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Głas, D.; Glaser,
C.; Golup, G.; Gómez Berisso, M.; Gómez Vitale, P. F.; González,
N.; Gorgi, A.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes,
G. P.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison,
T. A.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Herve, A. E.;
Hill, G. C.; Hojvat, C.; Holt, E.; Homola, P.; Hörandel, J. R.;
Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman, J.; Insolia, A.;
Isar, P. G.; Jandt, I.; Johnsen, J. A.; Josebachuili, M.; Jurysek,
J.; Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Keilhauer, B.;
Kemmerich, N.; Kemp, E.; Kemp, J.; Kieckhafer, R. M.; Klages, H. O.;
Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Kuempel, D.;
Kukec Mezek, G.; Kunka, N.; Kuotb Awad, A.; Lago, B. L.; LaHurd, D.;
Lang, R. G.; Lauscher, M.; Legumina, R.; Leigui de Oliveira, M. A.;
Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; Lo Presti, D.; Lopes,
L.; López, R.; López Casado, A.; Lorek, R.; Luce, Q.; Lucero, A.;
Malacari, M.; Mallamaci, M.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.;
Mariş, I. C.; Marsella, G.; Martello, D.; Martinez, H.; Martínez
Bravo, O.; Masías Meza, J. J.; Mathes, H. J.; Mathys, S.; Matthiae,
G.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Melo,
D.; Menshikov, A.; Merenda, K. -D.; Michal, S.; Micheletti, M. I.;
Middendorf, L.; Miramonti, L.; Mitrica, B.; Mockler, D.; Mollerach,
S.; Montanet, F.; Morello, C.; Morlino, G.; Mostafá, M.; Müller,
A. L.; Müller, G.; Muller, M. A.; Müller, S.; Mussa, R.; Naranjo,
I.; Nellen, L.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.;
Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka,
L.; Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Palatka,
M.; Pallotta, J.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.;
Pech, M.; Pedreira, F.; Pękala, J.; Pelayo, R.; Peña-Rodriguez, J.;
Pereira, L. A. S.; Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.;
Phuntsok, J.; Piegaia, R.; Pierog, T.; Pimenta, M.; Pirronello, V.;
Platino, M.; Plum, M.; Poh, J.; Porowski, C.; Prado, R. R.; Privitera,
P.; Prouza, M.; Quel, E. J.; Querchfeld, S.; Quinn, S.; Ramos-Pollan,
R.; Rautenberg, J.; Ravignani, D.; Ridky, J.; Riehn, F.; Risse, M.;
Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Fernandez,
G.; Rodriguez Rojo, J.; Roncoroni, M. J.; Roth, M.; Roulet, E.; Rovero,
A. C.; Ruehl, P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar,
H.; Saleh, A.; Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santos,
E. M.; Santos, E.; Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato,
R.; Schauer, M.; Scherini, V.; Schieler, H.; Schimp, M.; Schmidt,
D.; Scholten, O.; Schovánek, P.; Schröder, F. G.; Schröder, S.;
Schulz, A.; Schumacher, J.; Sciutto, S. J.; Segreto, A.; Shellard,
R. C.; Sigl, G.; Silli, G.; Šmída, R.; Snow, G. R.; Sommers, P.;
Sonntag, S.; Soriano, J. F.; Squartini, R.; Stanca, D.; Stanič, S.;
Stasielak, J.; Stassi, P.; Stolpovskiy, M.; Strafella, F.; Streich,
A.; Suarez, F.; Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.;
Supanitsky, A. D.; Šupík, J.; Swain, J.; Szadkowski, Z.; Taboada,
A.; Taborda, O. A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Tomankova, L.; Tomé, B.; Torralba Elipe, G.; Travnicek, P.;
Trini, M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.;
Valiño, I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg,
A. M.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Vázquez,
R. A.; Veberič, D.; Ventura, C.; Vergara Quispe, I. D.; Verzi, V.;
Vicha, J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.; Wainberg,
O.; Walz, D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiedeński, M.;
Wiencke, L.; Wilczyński, H.; Winchen, T.; Wirtz, M.; Wittkowski,
D.; Wundheiler, B.; Yang, L.; Yushkov, A.; Zas, E.; Zavrtanik, D.;
Zavrtanik, M.; Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.;
Zuccarello, F.
2017arXiv170806592T Altcode:
Contributions of the Pierre Auger Collaboration to the 35th
International Cosmic Ray Conference (ICRC 2017), 12-20 July 2017,
Bexco, Busan, Korea.
---------------------------------------------------------
Title: Expanding and Contracting Coronal Loops as Evidence of Vortex
Flows Induced by Solar Eruptions
Authors: Dudík, J.; Zuccarello, F. P.; Aulanier, G.; Schmieder, B.;
Démoulin, P.
2017ApJ...844...54D Altcode: 2017arXiv170604783D
Eruptive solar flares were predicted to generate large-scale vortex
flows at both sides of the erupting magnetic flux rope. This process
is analogous to a well-known hydrodynamic process creating vortex
rings. The vortices lead to advection of closed coronal loops located
at the peripheries of the flaring active region. Outward flows are
expected in the upper part and returning flows in the lower part of the
vortex. Here, we examine two eruptive solar flares, the X1.1-class flare
SOL2012-03-05T03:20 and the C3.5-class SOL2013-06-19T07:29. In both
flares, we find that the coronal loops observed by the Atmospheric
Imaging Assembly in its 171 Å, 193 Å, or 211 Å passbands show
coexistence of expanding and contracting motions, in accordance with
the model prediction. In the X-class flare, multiple expanding and
contracting loops coexist for more than 35 minutes, while in the C-class
flare, an expanding loop in 193 Å appears to be close by and cotemporal
with an apparently imploding loop arcade seen in 171 Å. Later, the 193
Å loop also switches to contraction. These observations are naturally
explained by vortex flows present in a model of eruptive solar flares.
---------------------------------------------------------
Title: Multi-resolution anisotropy studies of ultrahigh-energy cosmic
rays detected at the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Samarai, I. Al;
Albuquerque, I. F. M.; Allekotte, I.; Almela, A.; Alvarez Castillo,
J.; Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.;
Andringa, S.; Aramo, C.; Arqueros, F.; Arsene, N.; Asorey, H.; Assis,
P.; Aublin, J.; Avila, G.; Badescu, A. M.; Balaceanu, A.; Barreira Luz,
R. J.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.; Berat,
C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Billoir, P.; Biteau,
J.; Blaess, S. G.; Blanco, A.; Blazek, J.; Bleve, C.; Boháčová,
M.; Boncioli, D.; Bonifazi, C.; Borodai, N.; Botti, A. M.; Brack, J.;
Brancus, I.; Bretz, T.; Bridgeman, A.; Briechle, F. L.; Buchholz, P.;
Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga,
L.; Cancio, A.; Canfora, F.; Caramete, L.; Caruso, R.; Castellina, A.;
Cataldi, G.; Cazon, L.; Chavez, A. G.; Chinellato, J. A.; Chudoba, J.;
Clay, R. W.; Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.;
Conceição, R.; Contreras, F.; Cooper, M. J.; Coutu, S.; Covault,
C. E.; Cronin, J.; D'Amico, S.; Daniel, B.; Dasso, S.; Daumiller,
K.; Dawson, B. R.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza, V.;
Debatin, J.; Deligny, O.; Di Giulio, C.; Di Matteo, A.; Díaz Castro,
M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.; dos Anjos, R. C.;
Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.; Erdmann, M.; Erfani, M.;
Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Falcke, H.; Farrar, G.;
Fauth, A. C.; Fazzini, N.; Fick, B.; Figueira, J. M.; Filipčič, A.;
Fratu, O.; Freire, M. M.; Fujii, T.; Fuster, A.; Gaior, R.; García,
B.; Garcia-Pinto, D.; Gaté, F.; Gemmeke, H.; Gherghel-Lascu, A.;
Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Głas, D.;
Glaser, C.; Golup, G.; Gómez Berisso, M.; Gómez Vitale, P. F.;
González, N.; Gorgi, A.; Gorham, P.; Gouffon, P.; Grillo, A. F.;
Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel, M. R.; Hansen, P.;
Harari, D.; Harrison, T. A.; Harton, J. L.; Hasankiadeh, Q.; Haungs,
A.; Hebbeker, T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill, G. C.;
Hojvat, C.; Holt, E.; Homola, P.; Hörandel, J. R.; Horvath, P.;
Hrabovský, M.; Huege, T.; Hulsman, J.; Insolia, A.; Isar, P. G.;
Jandt, I.; Jansen, S.; Johnsen, J. A.; Josebachuili, M.; Kääpä,
A.; Kambeitz, O.; Kampert, K. H.; Katkov, I.; Keilhauer, B.; Kemp,
E.; Kemp, J.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.;
Kleinfeller, J.; Krause, R.; Krohm, N.; Kuempel, D.; Kukec Mezek,
G.; Kunka, N.; Kuotb Awad, A.; LaHurd, D.; Lauscher, M.; Legumina,
R.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon,
I.; Link, K.; Lopes, L.; López, R.; López Casado, A.; Luce, Q.;
Lucero, A.; Malacari, M.; Mallamaci, M.; Mandat, D.; Mantsch, P.;
Mariazzi, A. G.; Mariş, I. C.; Marsella, G.; Martello, D.; Martinez,
H.; Martínez Bravo, O.; Masías Meza, J. J.; Mathes, H. J.; Mathys,
S.; Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Mayotte, E.;
Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Melo, D.; Menshikov,
A.; Messina, S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.;
Miramonti, L.; Mitrica, B.; Mockler, D.; Mollerach, S.; Montanet,
F.; Morello, C.; Mostafá, M.; Müller, A. L.; Müller, G.; Muller,
M. A.; Müller, S.; Mussa, R.; Naranjo, I.; Nellen, L.; Nguyen, P. H.;
Niculescu-Oglinzanu, M.; Niechciol, M.; Niemietz, L.; Niggemann,
T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, H.; Núñez, L. A.;
Ochilo, L.; Oikonomou, F.; Olinto, A.; Pakk Selmi-Dei, D.; Palatka,
M.; Pallotta, J.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.;
Pech, M.; Pedreira, F.; Pȩkala, J.; Pelayo, R.; Peña-Rodriguez,
J.; Pereira, L. A. S.; Perlín, M.; Perrone, L.; Peters, C.; Petrera,
S.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.;
Pirronello, V.; Platino, M.; Plum, M.; Porowski, C.; Prado, R. R.;
Privitera, P.; Prouza, M.; Quel, E. J.; Querchfeld, S.; Quinn, S.;
Ramos-Pollan, R.; Rautenberg, J.; Ravignani, D.; Revenu, B.; Ridky,
J.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.;
Rodriguez Fernandez, G.; Rodriguez Rojo, J.; Rogozin, D.; Roncoroni,
M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl, P.; Saffi, S. J.;
Saftoiu, A.; Salazar, H.; Saleh, A.; Salesa Greus, F.; Salina, G.;
Sánchez, F.; Sanchez-Lucas, P.; Santos, E. M.; Santos, E.; Sarazin,
F.; Sarmento, R.; Sarmiento, C. A.; Sato, R.; Schauer, M.; Scherini,
V.; Schieler, H.; Schimp, M.; Schmidt, D.; Scholten, O.; Schovánek,
P.; Schröder, F. G.; Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto,
S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sigl,
G.; Silli, G.; Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.;
Sommers, P.; Sonntag, S.; Sorokin, J.; Squartini, R.; Stanca, D.;
Stanič, S.; Stasielak, J.; Stassi, P.; Strafella, F.; Suarez, F.;
Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky, A. D.;
Swain, J.; Szadkowski, Z.; Taboada, A.; Taborda, O. A.; Tapia, A.;
Theodoro, V. M.; Timmermans, C.; Todero Peixoto, C. J.; Tomankova, L.;
Tomé, B.; Torralba Elipe, G.; Torri, M.; Travnicek, P.; Trini, M.;
Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño,
I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.;
van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.; Vázquez,
J. R.; Vázquez, R. A.; Veberič, D.; Vergara Quispe, I. D.; Verzi,
V.; Vicha, J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.; Wainberg,
O.; Walz, D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.;
Wilczyński, H.; Winchen, T.; Wittkowski, D.; Wundheiler, B.; Yang,
L.; Yelos, D.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello, F.
2017JCAP...06..026A Altcode: 2016arXiv161106812T
We report a multi-resolution search for anisotropies in the arrival
directions of cosmic rays detected at the Pierre Auger Observatory with
local zenith angles up to 80<SUP>o</SUP> and energies in excess of 4
EeV (4 × 10<SUP>18</SUP> eV). This search is conducted by measuring
the angular power spectrum and performing a needlet wavelet analysis
in two independent energy ranges. Both analyses are complementary since
the angular power spectrum achieves a better performance in identifying
large-scale patterns while the needlet wavelet analysis, considering
the parameters used in this work, presents a higher efficiency in
detecting smaller-scale anisotropies, potentially providing directional
information on any observed anisotropies. No deviation from isotropy
is observed on any angular scale in the energy range between 4 and
8 EeV. Above 8 EeV, an indication for a dipole moment is captured;
while no other deviation from isotropy is observed for moments beyond
the dipole one. The corresponding p-values obtained after accounting
for searches blindly performed at several angular scales, are 1.3 ×
10<SUP>-5</SUP> in the case of the angular power spectrum, and 2.5
× 10<SUP>-3</SUP> in the case of the needlet analysis. While these
results are consistent with previous reports making use of the same
data set, they provide extensions of the previous works through the
thorough scans of the angular scales.
---------------------------------------------------------
Title: Transition from eruptive to confined flares in the same
active region
Authors: Zuccarello, F. P.; Chandra, R.; Schmieder, B.; Aulanier,
G.; Joshi, R.
2017A&A...601A..26Z Altcode: 2017arXiv170202477Z
Context. Solar flares are sudden and violent releases of magnetic
energy in the solar atmosphere that can be divided into two classes:
eruptive flares, where plasma is ejected from the solar atmosphere
resulting in a coronal mass ejection (CME), and confined flares,
where no CME is associated with the flare. <BR /> Aims: We present
a case study showing the evolution of key topological structures,
such as spines and fans, which may determine the eruptive versus
non-eruptive behavior of the series of eruptive flares followed by
confined flares, which all originate from the same site. <BR />
Methods: To study the connectivity of the different flux domains
and their evolution, we compute a potential magnetic field model of
the active region. Quasi-separatrix layers are retrieved from the
magnetic field extrapolation. <BR /> Results: The change in behavior
of the flares from one day to the next - from eruptive to confined -
can be attributed to the change in orientation of the magnetic field
below the fan with respect to the orientation of the overlaying spine
rather than an overall change in the stability of the large-scale
field. <BR /> Conclusions: Flares tend to be more confined when the
field that supports the filament and the overlying field gradually
becomes less anti-parallel as a direct result of changes in the
photospheric flux distribution, being themselves driven by continuous
shearing motions of the different magnetic flux concentrations. <P
/>Movies associated to Figs. 2, 3, and 5 are available at <A
href="http://www.aanda.org/10.1051/0004-6361/201629836/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: Relative magnetic helicity as a diagnostic of solar eruptivity
Authors: Pariat, E.; Leake, J. E.; Valori, G.; Linton, M. G.;
Zuccarello, F. P.; Dalmasse, K.
2017A&A...601A.125P Altcode: 2017arXiv170310562P
Context. The discovery of clear criteria that can deterministically
describe the eruptive state of a solar active region would lead
to major improvements on space weather predictions. <BR /> Aims:
Using series of numerical simulations of the emergence of a magnetic
flux rope in a magnetized coronal, leading either to eruptions or to
stable configurations, we test several global scalar quantities for
the ability to discriminate between the eruptive and the non-eruptive
simulations. <BR /> Methods: From the magnetic field generated by the
three-dimensional magnetohydrodynamical simulations, we compute and
analyze the evolution of the magnetic flux, of the magnetic energy
and its decomposition into potential and free energies, and of the
relative magnetic helicity and its decomposition. <BR /> Results:
Unlike the magnetic flux and magnetic energies, magnetic helicities
are able to markedly distinguish the eruptive from the non-eruptive
simulations. We find that the ratio of the magnetic helicity of the
current-carrying magnetic field to the total relative helicity presents
the highest values for the eruptive simulations, in the pre-eruptive
phase only. We observe that the eruptive simulations do not possess the
highest value of total magnetic helicity. <BR /> Conclusions: In the
framework of our numerical study, the magnetic energies and the total
relative helicity do not correspond to good eruptivity proxies. Our
study highlights that the ratio of magnetic helicities diagnoses very
clearly the eruptive potential of our parametric simulations. Our study
shows that magnetic-helicity-based quantities may be very efficient
for the prediction of solar eruptions.
---------------------------------------------------------
Title: Polarized Kink Waves in Magnetic Elements: Evidence for
Chromospheric Helical Waves
Authors: Stangalini, M.; Giannattasio, F.; Erdélyi, R.; Jafarzadeh,
S.; Consolini, G.; Criscuoli, S.; Ermolli, I.; Guglielmino, S. L.;
Zuccarello, F.
2017ApJ...840...19S Altcode: 2017arXiv170402155S
In recent years, new high spatial resolution observations of the Sun's
atmosphere have revealed the presence of a plethora of small-scale
magnetic elements down to the resolution limit of the current cohort
of solar telescopes (∼100-120 km on the solar photosphere). These
small magnetic field concentrations, due to the granular buffeting,
can support and guide several magnetohydrodynamic wave modes that
would eventually contribute to the energy budget of the upper layers
of the atmosphere. In this work, exploiting the high spatial and
temporal resolution chromospheric data acquired with the Swedish
1 m Solar Telescope, and applying the empirical mode decomposition
technique to the tracking of the solar magnetic features, we analyze
the perturbations of the horizontal velocity vector of a set of
chromospheric magnetic elements. We find observational evidence that
suggests a phase relation between the two components of the velocity
vector itself, resulting in its helical motion.
---------------------------------------------------------
Title: Plasma flows and magnetic field interplay during the formation
of a pore
Authors: Ermolli, I.; Cristaldi, A.; Giorgi, F.; Giannattasio, F.;
Stangalini, M.; Romano, P.; Tritschler, A.; Zuccarello, F.
2017A&A...600A.102E Altcode: 2017arXiv170106440E
<BR /> Aims: Recent simulations of solar magneto-convection have offered
new levels of understanding of the interplay between plasma motions
and magnetic fields in evolving active regions. We aim at verifying
some aspects of the formation of magnetic regions derived from recent
numerical studies in observational data. <BR /> Methods: We studied the
formation of a pore in the active region (AR) NOAA 11462. We analysed
data obtained with the Interferometric Bidimensional Spectrometer
(IBIS) at the Dunn Solar Telescope on April 17, 2012, consisting of
full Stokes measurements of the Fe I 617.3 nm lines. Furthermore, we
analysed SDO/HMI observations in the continuum and vector magnetograms
derived from the Fe I 617.3 nm line data taken from April 15 to 19,
2012. We estimated the magnetic field strength and vector components
and the line-of-sight (LOS) and horizontal motions in the photospheric
region hosting the pore formation. We discuss our results in light
of other observational studies and recent advances of numerical
simulations. <BR /> Results: The pore formation occurs in less than
1 h in the leading region of the AR. We observe that the evolution
of the flux patch in the leading part of the AR is faster (<12 h)
than the evolution (20-30 h) of the more diffuse and smaller scale
flux patches in the trailing region. During the pore formation,
the ratio between magnetic and dark area decreases from 5 to 2. We
observe strong downflows at the forming pore boundary and diverging
proper motions of plasma in the vicinity of the evolving feature that
are directed towards the forming pore. The average values and trends of
the various quantities estimated in the AR are in agreement with results
of former observational studies of steady pores and with their modelled
counterparts, as seen in recent numerical simulations of a rising-tube
process. The agreement with the outcomes of the numerical studies holds
for both the signatures of the flux emergence process (e.g. appearance
of small-scale mixed polarity patterns and elongated granules) and the
evolution of the region. The processes driving the formation of the pore
are identified with the emergence of a magnetic flux concentration and
the subsequent reorganization of the emerged flux, by the combined
effect of velocity and magnetic field, in and around the evolving
structure. <P />Movies associated to Figs. 1 and 4 are available at <A
href="http://www.aanda.org/10.1051/0004-6361/201526144/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: A Targeted Search for Point Sources of EeV Photons with the
Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Samarai, I. Al;
Albuquerque, I. F. M.; Allekotte, I.; Almela, A.; Alvarez Castillo,
J.; Alvarez-Muñiz, J.; Anastasi, G. A.; Anchordoqui, L.; Andrada, B.;
Andringa, S.; Aramo, C.; Arqueros, F.; Arsene, N.; Asorey, H.; Assis,
P.; Aublin, J.; Avila, G.; Badescu, A. M.; Balaceanu, A.; Barreira
Luz, R. J.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.; Berat, C.;
Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Billoir, P.; Biteau,
J.; Blaess, S. G.; Blanco, A.; Blazek, J.; Bleve, C.; Boháčová,
M.; Boncioli, D.; Bonifazi, C.; Borodai, N.; Botti, A. M.; Brack, J.;
Brancus, I.; Bretz, T.; Bridgeman, A.; Briechle, F. L.; Buchholz, P.;
Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga,
L.; Cancio, A.; Canfora, F.; Caramete, L.; Caruso, R.; Castellina, A.;
Cataldi, G.; Cazon, L.; Chavez, A. G.; Chinellato, J. A.; Chudoba, J.;
Clay, R. W.; Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.;
Conceição, R.; Contreras, F.; Cooper, M. J.; Coutu, S.; Covault,
C. E.; Cronin, J.; D'Amico, S.; Daniel, B.; Dasso, S.; Daumiller,
K.; Dawson, B. R.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza,
V.; Debatin, J.; Deligny, O.; Di Giulio, C.; Di Matteo, A.; Díaz
Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.; Dorosti,
Q.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.;
Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.;
Falcke, H.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Fick, B.; Figueira,
J. M.; Filipčič, A.; Fratu, O.; Freire, M. M.; Fujii, T.; Fuster,
A.; Gaior, R.; García, B.; Garcia-Pinto, D.; Gaté, F.; Gemmeke,
H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.;
Giller, M.; Głas, D.; Glaser, C.; Golup, G.; Gómez Berisso, M.;
Gómez Vitale, P. F.; González, N.; Gorgi, A.; Gorham, P.; Grillo,
A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel, M. R.; Hansen,
P.; Harari, D.; Harrison, T. A.; Harton, J. L.; Haungs, A.; Hebbeker,
T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.;
Holt, E.; Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský,
M.; Huege, T.; Hulsman, J.; Insolia, A.; Isar, P. G.; Jandt, I.;
Jansen, S.; Johnsen, J. A.; Josebachuili, M.; Kääpä, A.; Kambeitz,
O.; Kampert, K. H.; Katkov, I.; Keilhauer, B.; Kemp, E.; Kemp, J.;
Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.;
Krause, R.; Krohm, N.; Kuempel, D.; Kukec Mezek, G.; Kunka, N.; Kuotb
Awad, A.; LaHurd, D.; Lauscher, M.; Legumina, R.; Leigui de Oliveira,
M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; Lopes, L.;
López, R.; López Casado, A.; Luce, Q.; Lucero, A.; Malacari, M.;
Mallamaci, M.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Mariş,
I. C.; Marsella, G.; Martello, D.; Martinez, H.; Martínez Bravo,
O.; Masías Meza, J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.;
Matthews, J. A. J.; Matthiae, G.; Mayotte, E.; Mazur, P. O.; Medina,
C.; Medina-Tanco, G.; Melo, D.; Menshikov, A.; Micheletti, M. I.;
Middendorf, L.; Minaya, I. A.; Miramonti, L.; Mitrica, B.; Mockler,
D.; Mollerach, S.; Montanet, F.; Morello, C.; Mostafá, M.; Müller,
A. L.; Müller, G.; Muller, M. A.; Müller, S.; Mussa, R.; Naranjo,
I.; Nellen, L.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.;
Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka,
H.; Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Palatka,
M.; Pallotta, J.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.;
Pech, M.; Pedreira, F.; Pȩkala, J.; Pelayo, R.; Peña-Rodriguez,
J.; Pereira, L. A. S.; Perlín, M.; Perrone, L.; Peters, C.; Petrera,
S.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.;
Pirronello, V.; Platino, M.; Plum, M.; Porowski, C.; Prado, R. R.;
Privitera, P.; Prouza, M.; Quel, E. J.; Querchfeld, S.; Quinn, S.;
Ramos-Pollan, R.; Rautenberg, J.; Ravignani, D.; Revenu, B.; Ridky, J.;
Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez
Fernandez, G.; Rodriguez Rojo, J.; Rogozin, D.; Roncoroni, M. J.; Roth,
M.; Roulet, E.; Rovero, A. C.; Ruehl, P.; Saffi, S. J.; Saftoiu, A.;
Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.; Salina, G.;
Sánchez, F.; Sanchez-Lucas, P.; Santos, E. M.; Santos, E.; Sarazin,
F.; Sarmento, R.; Sarmiento, C. A.; Sato, R.; Schauer, M.; Scherini,
V.; Schieler, H.; Schimp, M.; Schmidt, D.; Scholten, O.; Schovánek,
P.; Schröder, F. G.; Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto,
S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sigl,
G.; Silli, G.; Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.;
Sommers, P.; Sonntag, S.; Sorokin, J.; Squartini, R.; Stanca, D.;
Stanič, S.; Stasielak, J.; Stassi, P.; Strafella, F.; Suarez, F.;
Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky, A. D.;
Swain, J.; Szadkowski, Z.; Taboada, A.; Taborda, O. A.; Tapia, A.;
Theodoro, V. M.; Timmermans, C.; Todero Peixoto, C. J.; Tomankova, L.;
Tomé, B.; Torralba Elipe, G.; Travnicek, P.; Trini, M.; Ulrich, R.;
Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore,
L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.; van Vliet,
A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.; Vázquez, J. R.;
Vázquez, R. A.; Veberič, D.; Vergara Quispe, I. D.; Verzi, V.; Vicha,
J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz,
D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński,
H.; Winchen, T.; Wirtz, M.; Wittkowski, D.; Wundheiler, B.; Yang,
L.; Yelos, D.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello, F.
2017ApJ...837L..25A Altcode: 2016arXiv161204155T
Simultaneous measurements of air showers with the fluorescence and
surface detectors of the Pierre Auger Observatory allow a sensitive
search for EeV photon point sources. Several Galactic and extragalactic
candidate objects are grouped in classes to reduce the statistical
penalty of many trials from that of a blind search and are analyzed
for a significant excess above the background expectation. The
presented search does not find any evidence for photon emission
at candidate sources, and combined p-values for every class are
reported. Particle and energy flux upper limits are given for selected
candidate sources. These limits significantly constrain predictions
of EeV proton emission models from non-transient Galactic and nearby
extragalactic sources, as illustrated for the particular case of the
Galactic center region.
---------------------------------------------------------
Title: Vortex and Sink Flows in Eruptive Flares as a Model for
Coronal Implosions
Authors: Zuccarello, F. P.; Aulanier, G.; Dudík, J.; Démoulin, P.;
Schmieder, B.; Gilchrist, S. A.
2017ApJ...837..115Z Altcode: 2017arXiv170200199Z
Eruptive flares are sudden releases of magnetic energy that
involve many phenomena, several of which can be explained by the
standard 2D flare model and its realizations in 3D. We analyze a 3D
magnetohydrodynamics simulation, in the framework of this model, that
naturally explains the contraction of coronal loops in the proximity
of the flare sites, as well as the inflow toward the region above the
cusp-shaped loops. We find that two vorticity arcs located along the
flanks of the erupting magnetic flux rope are generated as soon as the
eruption begins. The magnetic arcades above the flux rope legs are then
subjected to expansion, rotation, or contraction depending on which
part of the vortex flow advects them. In addition to the vortices,
an inward-directed magnetic pressure gradient exists in the current
sheet below the magnetic flux rope. It results in the formation of a
sink that is maintained by reconnection. We conclude that coronal loop
apparent implosions observed during eruptive flares are the result
of hydromagnetic effects related to the generation of vortex and sink
flows when a flux rope moves in a magnetized environment.
---------------------------------------------------------
Title: Muon counting using silicon photomultipliers in the AMIGA
detector of the Pierre Auger observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai,
I. Al; Albuquerque, I. F. M.; Allekotte, I.; Allison, P.; Almela, A.;
Alvarez Castillo, J.; Alvarez-Muñiz, J.; Ambrosio, M.; Anastasi,
G. A.; Anchordoqui, L.; Andrada, B.; Andringa, S.; Aramo, C.;
Arqueros, F.; Arsene, N.; Asorey, H.; Assis, P.; Aublin, J.; Avila,
G.; Badescu, A. M.; Balaceanu, A.; Baus, C.; Beatty, J. J.; Becker,
K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.;
Biermann, P. L.; Billoir, P.; Biteau, J.; Blaess, S. G.; Blanco,
A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Botti, A. M.; Brack, J.; Brancus, I.; Bretz, T.;
Bridgeman, A.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink,
S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga,
L.; Cancio, A.; Canfora, F.; Caramete, L.; Caruso, R.; Castellina,
A.; Cataldi, G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.;
Chinellato, J. A.; Chudoba, J.; Clay, R. W.; Colalillo, R.; Coleman,
A.; Collica, L.; Coluccia, M. R.; Conceição, R.; Contreras, F.;
Cooper, M. J.; Coutu, S.; Covault, C. E.; Cronin, J.; Dallier, R.;
D'Amico, S.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; de
Almeida, R. M.; de Jong, S. J.; De Mauro, G.; de Mello Neto, J. R. T.;
De Mitri, I.; de Oliveira, J.; de Souza, V.; Debatin, J.; del Peral,
L.; Deligny, O.; Di Giulio, C.; Di Matteo, A.; Díaz Castro, M. L.;
Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.; Dorofeev, A.; dos Anjos,
R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.; Erdmann, M.;
Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Falcke, H.;
Fang, K.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Fick, B.; Figueira,
J. M.; Filevich, A.; Filipčič, A.; Fratu, O.; Freire, M. M.; Fujii,
T.; Fuster, A.; García, B.; Garcia-Pinto, D.; Gaté, F.; Gemmeke, H.;
Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller,
M.; Głas, D.; Glaser, C.; Glass, H.; Golup, G.; Gómez Berisso, M.;
Gómez Vitale, P. F.; González, N.; Gookin, B.; Gordon, J.; Gorgi,
A.; Gorham, P.; Gouffon, P.; Grillo, A. F.; Grubb, T. D.; Guarino, F.;
Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison, T. A.;
Harton, J. L.; Hasankiadeh, Q.; Haungs, A.; Hebbeker, T.; Heck, D.;
Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Holt, E.; Homola,
P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman,
J.; Insolia, A.; Isar, P. G.; Jandt, I.; Jansen, S.; Johnsen, J. A.;
Josebachuili, M.; Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper,
P.; Katkov, I.; Keilhauer, B.; Kemp, E.; Kieckhafer, R. M.; Klages,
H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Kuempel,
D.; Kukec Mezek, G.; Kunka, N.; Kuotb Awad, A.; LaHurd, D.; Latronico,
L.; Lauscher, M.; Lebrun, P.; Legumina, R.; Leigui de Oliveira, M. A.;
Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; Lopes, L.; López, R.;
López Casado, A.; Luce, Q.; Lucero, A.; Malacari, M.; Mallamaci, M.;
Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Mariş, I. C.; Marsella, G.;
Martello, D.; Martinez, H.; Martínez Bravo, O.; Masías Meza, J. J.;
Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.; Matthiae,
G.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Melo,
D.; Menshikov, A.; Messina, S.; Micheletti, M. I.; Middendorf, L.;
Minaya, I. A.; Miramonti, L.; Mitrica, B.; Mockler, D.; Molina-Bueno,
L.; Mollerach, S.; Montanet, F.; Morello, C.; Mostafá, M.; Müller,
G.; Muller, M. A.; Müller, S.; Naranjo, I.; Navas, S.; Nellen,
L.; Neuser, J.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol,
M.; Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.;
Nožka, H.; Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.;
Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Papenbreer, P.; Parente,
G.; Parra, A.; Paul, T.; Pech, M.; Pedreira, F.; Pȩkala, J.; Pelayo,
R.; Peña-Rodriguez, J.; Pereira, L. A. S.; Perrone, L.; Peters, C.;
Petrera, S.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.;
Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.; Porowski, C.;
Prado, R. R.; Privitera, P.; Prouza, M.; Quel, E. J.; Querchfeld,
S.; Quinn, S.; Ramos-Pollant, R.; Rautenberg, J.; Ravignani, D.;
Reinert, D.; Revenu, B.; Ridky, J.; Risse, M.; Ristori, P.; Rizi,
V.; Rodrigues de Carvalho, W.; Rodriguez Fernandez, G.; Rodriguez
Rojo, J.; Rodríguez-Frías, M. D.; Rogozin, D.; Rosado, J.; Roth,
M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.; Saftoiu, A.; Salazar,
H.; Saleh, A.; Salesa Greus, F.; Salina, G.; Sanabria Gomez, J. D.;
Sánchez, F.; Sanchez-Lucas, P.; Santos, E. M.; Santos, E.; Sarazin,
F.; Sarkar, B.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.; Scarso,
C.; Schauer, M.; Scherini, V.; Schieler, H.; Schmidt, D.; Scholten, O.;
Schovánek, P.; Schröder, F. G.; Schulz, A.; Schulz, J.; Schumacher,
J.; Sciutto, S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard,
R. C.; Sigl, G.; Silli, G.; Sima, O.; Śmiałkowski, A.; Šmída,
R.; Snow, G. R.; Sommers, P.; Sonntag, S.; Sorokin, J.; Squartini,
R.; Stanca, D.; Stanič, S.; Stasielak, J.; Strafella, F.; Suarez,
F.; Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky,
A. D.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Taborda, O. A.;
Tapia, A.; Tepe, A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Tomankova, L.; Tomé, B.; Tonachini, A.; Torralba Elipe, G.;
Torres Machado, D.; Torri, M.; Travnicek, P.; Trini, M.; Ulrich, R.;
Unger, M.; Urban, M.; Valbuena-Delgado, A.; Valdés Galicia, J. F.;
Valiño, I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg,
A. M.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.;
Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha,
J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz,
D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński,
H.; Winchen, T.; Wittkowski, D.; Wundheiler, B.; Wykes, S.; Yang,
L.; Yelos, D.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello, F.
2017JInst..12P3002A Altcode: 2017arXiv170306193T
AMIGA (Auger Muons and Infill for the Ground Array) is an upgrade of
the Pierre Auger Observatory designed to extend its energy range of
detection and to directly measure the muon content of the cosmic ray
primary particle showers. The array will be formed by an infill of
surface water-Cherenkov detectors associated with buried scintillation
counters employed for muon counting. Each counter is composed of
three scintillation modules, with a 10 m<SUP>2</SUP> detection
area per module. In this paper, a new generation of detectors,
replacing the current multi-pixel photomultiplier tube (PMT) with
silicon photo sensors (aka. SiPMs), is proposed. The selection of
the new device and its front-end electronics is explained. A method
to calibrate the counting system that ensures the performance of the
detector is detailed. This method has the advantage of being able to be
carried out in a remote place such as the one where the detectors are
deployed. High efficiency results, i.e. 98% efficiency for the highest
tested overvoltage, combined with a low probability of accidental
counting (~2%), show a promising performance for this new system.
---------------------------------------------------------
Title: On the Formation of a Stable Penumbra in a Region of Flux
Emergence in the Sun
Authors: Murabito, M.; Romano, P.; Guglielmino, S. L.; Zuccarello, F.
2017ApJ...834...76M Altcode: 2016arXiv161104749M
We studied the formation of the first penumbral sector around a pore
in the following polarity of the NOAA Active Region (AR) 11490. We used
a high spatial, spectral, and temporal resolution data set acquired by
the Interferometric BIdimensional Spectrometer operating at the NSO/Dunn
Solar Telescope, as well as data taken by the Helioseismic and Magnetic
Imager on board the Solar Dynamics Observatory satellite. On the side
toward the leading polarity, elongated granules in the photosphere
and an arch filament system (AFS) in the chromosphere are present,
while the magnetic field shows a sea-serpent configuration, indicating
a region of magnetic flux emergence. We found that the formation of
a stable penumbra in the following polarity of the AR begins in the
area facing the opposite polarity located below the AFS in the flux
emergence region, different from what was found by Schlichenmaier
and colleagues. Moreover, during the formation of the first penumbral
sector, the area characterized by magnetic flux density larger than
900 G and the area of the umbra increase.
---------------------------------------------------------
Title: A Statistical Study of CME Properties and of the Correlation
Between Flares and CMEs over Solar Cycles 23 and 24
Authors: Compagnino, A.; Romano, P.; Zuccarello, F.
2017SoPh..292....5C Altcode: 2016arXiv160908943C
We investigated some properties of coronal mass ejections (CMEs),
such as speed, acceleration, polar angle, angular width, and mass,
using data acquired by the Large Angle Spectrometric Coronagraph (LASCO)
onboard the Solar and Heliospheric Observatory (SOHO) from 31 July 1997
to 31 March 2014, i.e. during the Solar Cycles 23 and 24. We used two
CME catalogs: one provided by the Coordinated Data Analysis Workshops
(CDAW) Data Center and one obtained by the Computer Aided CME Tracking
software (CACTus) detection algorithm. For each dataset, we found that
the number of CMEs observed during the peak of Cycle 24 was higher than
or comparable to the number during Cycle 23, although the photospheric
activity during Cycle 24 was weaker than during Cycle 23. Using the
CMEs detected by CACTus, we noted that the number of events [N ] is of
the same order of magnitude during the peaks of the two cycles, but the
peak of the CME distribution during Cycle 24 is more extended in time
(N >1500 during 2012 and 2013). We ascribe the discrepancy between
the CDAW and CACTus results to the observer bias for CME definition
in the CDAW catalog. We also used a dataset containing 19,811 flares
of C-, M-, and X-class observed by the Geostationary Operational
Environmental Satellite (GOES) during the same period. Using both
datasets, we studied the relationship between the mass ejected by the
CMEs and the flux emitted during the corresponding flares: we found
11,441 flares that were temporally correlated with CMEs for CDAW and
9120 for CACTus. Moreover, we found a log-linear relationship between
the flux of the flares integrated from the start to end in the 0.1 -
0.8 nm range and the CME mass. We also found some differences in the
mean CMEs velocity and acceleration between the events associated with
flares and those that were not.
---------------------------------------------------------
Title: Polarization signatures in the chromosphere during an X1.6
flare
Authors: Guglielmino, S. L.; Zuccarello, F.; Murabito, M.; Romano, P.
2017psio.confE.119G Altcode:
No abstract at ADS
---------------------------------------------------------
Title: SOLARNET WP30: Solar Physics Networking
Authors: Zuccarello, Francesca; SOLARNET Team
2017psio.confE..93Z Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Ultrahigh-energy neutrino follow-up of gravitational wave
events GW150914 and GW151226 with the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Al Samarai, I.;
Albuquerque, I. F. M.; Allekotte, I.; Almela, A.; Alvarez Castillo,
J.; Alvarez-Muñiz, J.; Ambrosio, M.; Anastasi, G. A.; Anchordoqui,
L.; Andrada, B.; Andringa, S.; Aramo, C.; Arqueros, F.; Arsene,
N.; Asorey, H.; Assis, P.; Aublin, J.; Avila, G.; Badescu, A. M.;
Balaceanu, A.; Barreira Luz, R. J.; Baus, C.; Beatty, J. J.; Becker,
K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.;
Biermann, P. L.; Billoir, P.; Biteau, J.; Blaess, S. G.; Blanco,
A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Botti, A. M.; Brack, J.; Brancus, I.; Bretz, T.;
Bridgeman, A.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink,
S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, L.; Cancio, A.;
Canfora, F.; Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.;
Cazon, L.; Cester, R.; Chavez, A. G.; Chinellato, J. A.; Chudoba, J.;
Clay, R. W.; Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.;
Conceição, R.; Contreras, F.; Cooper, M. J.; Coutu, S.; Covault,
C. E.; Cronin, J.; D'Amico, S.; Daniel, B.; Dasso, S.; Daumiller,
K.; Dawson, B. R.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza,
V.; Debatin, J.; Deligny, O.; Di Giulio, C.; Di Matteo, A.; Díaz
Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.; Dorofeev,
A.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.;
Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen,
A.; Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Fick,
B.; Figueira, J. M.; Filipčič, A.; Fratu, O.; Freire, M. M.; Fujii,
T.; Fuster, A.; Gaior, R.; García, B.; Garcia-Pinto, D.; Gaté, F.;
Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; Giammarchi,
M.; Giller, M.; Głas, D.; Glaser, C.; Glass, H.; Golup, G.; Gómez
Berisso, M.; Gómez Vitale, P. F.; González, N.; Gookin, B.; Gorgi,
A.; Gorham, P.; Gouffon, P.; Grillo, A. F.; Grubb, T. D.; Guarino, F.;
Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison, T. A.;
Harton, J. L.; Hasankiadeh, Q.; Haungs, A.; Hebbeker, T.; Heck, D.;
Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Holt, E.; Homola,
P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman,
J.; Insolia, A.; Isar, P. G.; Jandt, I.; Jansen, S.; Johnsen, J. A.;
Josebachuili, M.; Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper,
P.; Katkov, I.; Keilhauer, B.; Kemp, E.; Kemp, J.; Kieckhafer, R. M.;
Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.;
Kuempel, D.; Kukec Mezek, G.; Kunka, N.; Kuotb Awad, A.; LaHurd, D.;
Lauscher, M.; Lebrun, P.; Legumina, R.; Leigui de Oliveira, M. A.;
Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; Lopes, L.; López, R.;
López Casado, A.; Luce, Q.; Lucero, A.; Malacari, M.; Mallamaci, M.;
Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Mariş, I. C.; Marsella, G.;
Martello, D.; Martinez, H.; Martínez Bravo, O.; Masías Meza, J. J.;
Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.; Matthiae,
G.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Melo,
D.; Menshikov, A.; Messina, S.; Micheletti, M. I.; Middendorf, L.;
Minaya, I. A.; Miramonti, L.; Mitrica, B.; Mockler, D.; Molina-Bueno,
L.; Mollerach, S.; Montanet, F.; Morello, C.; Mostafá, M.; Müller,
G.; Muller, M. A.; Müller, S.; Naranjo, I.; Nellen, L.; Neuser, J.;
Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.; Niemietz, L.;
Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, H.; Núñez,
L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Pakk Selmi-Dei, D.;
Palatka, M.; Pallotta, J.; Papenbreer, P.; Parente, G.; Parra,
A.; Paul, T.; Pech, M.; Pedreira, F.; Pekala, J.; Pelayo, R.;
Peña-Rodriguez, J.; Pereira, L. A. S.; Perrone, L.; Peters, C.;
Petrera, S.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.;
Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.; Porowski, C.;
Prado, R. R.; Privitera, P.; Prouza, M.; Quel, E. J.; Querchfeld,
S.; Quinn, S.; Ramos-Pollan, R.; Rautenberg, J.; Ravignani, D.;
Reinert, D.; Revenu, B.; Ridky, J.; Risse, M.; Ristori, P.; Rizi,
V.; Rodrigues de Carvalho, W.; Rodriguez Fernandez, G.; Rodriguez
Rojo, J.; Rogozin, D.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi,
S. J.; Saftoiu, A.; Salazar, H.; Saleh, A.; Salesa Greus, F.; Salina,
G.; Sanabria Gomez, J. D.; Sánchez, F.; Sanchez-Lucas, P.; Santos,
E. M.; Santos, E.; Sarazin, F.; Sarkar, B.; Sarmento, R.; Sarmiento,
C. A.; Sato, R.; Schauer, M.; Scherini, V.; Schieler, H.; Schimp,
M.; Schmidt, D.; Scholten, O.; Schovánek, P.; Schröder, F. G.;
Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto, S. J.; Segreto, A.;
Settimo, M.; Shadkam, A.; Shellard, R. C.; Sigl, G.; Silli, G.; Sima,
O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers, P.; Sonntag,
S.; Sorokin, J.; Squartini, R.; Stanca, D.; Stanič, S.; Stasielak,
J.; Stassi, P.; Strafella, F.; Suarez, F.; Suarez Durán, M.; Sudholz,
T.; Suomijärvi, T.; Supanitsky, A. D.; Swain, J.; Szadkowski, Z.;
Taboada, A.; Taborda, O. A.; Tapia, A.; Theodoro, V. M.; Timmermans,
C.; Todero Peixoto, C. J.; Tomankova, L.; Tomé, B.; Torralba Elipe,
G.; Torres Machado, D.; Torri, M.; Travnicek, P.; Trini, M.; Ulrich,
R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore,
L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.; van Vliet,
A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.; Vázquez, J. R.;
Vázquez, R. A.; Veberič, D.; Vergara Quispe, I. D.; Verzi, V.; Vicha,
J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz,
D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński,
H.; Winchen, T.; Wittkowski, D.; Wundheiler, B.; Wykes, S.; Yang,
L.; Yelos, D.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello,
F.; Pierre Auger Collaboration
2016PhRvD..94l2007A Altcode: 2016arXiv160807378T
On September 14, 2015 the Advanced LIGO detectors observed their
first gravitational wave (GW) transient GW150914. This was followed
by a second GW event observed on December 26, 2015. Both events were
inferred to have arisen from the merger of black holes in binary
systems. Such a system may emit neutrinos if there are magnetic
fields and disk debris remaining from the formation of the two black
holes. With the surface detector array of the Pierre Auger Observatory
we can search for neutrinos with energy E<SUB>ν</SUB> above 100 PeV
from pointlike sources across the sky with equatorial declination from
about -6 5 ° to +6 0 ° , and, in particular, from a fraction of the
90% confidence-level inferred positions in the sky of GW150914 and
GW151226. A targeted search for highly inclined extensive air showers,
produced either by interactions of downward-going neutrinos of all
flavors in the atmosphere or by the decays of tau leptons originating
from tau-neutrino interactions in the Earth's crust (Earth-skimming
neutrinos), yielded no candidates in the Auger data collected within
±500 s around or 1 day after the coordinated universal time (UTC)
of GW150914 and GW151226, as well as in the same search periods
relative to the UTC time of the GW candidate event LVT151012. From
the nonobservation we constrain the amount of energy radiated in
ultrahigh-energy neutrinos from such remarkable events.
---------------------------------------------------------
Title: Multi-spectral observations of flares
Authors: Zuccarello, F.
2016AN....337.1070Z Altcode:
Observations show that during solar flares radiation can be emitted
across the entire electromagnetic spectrum, spanning from gamma
rays to radio waves. These emissions, related to the conversion of
magnetic energy into other forms of energy (kinetic, thermal, waves)
through magnetic reconnection, are due to different physical processes
that can occur in different layers of the Sun. This means that flare
observations need to be carried out using instruments operating in
different wave-bands in order to achieve a complete scenario of the
processes going on. Taking into account that most of the radiative
energy is emitted at optical and UV wavelengths, observations carried
out from space, need to be complemented by observations carried out
from ground-based telescopes. Nowadays, the possibility to carry on high
temporal, spatial and spectral resolution from ground-based telescopes
in coordinated campaigns with space-borne instruments (like, i.e.,
IRIS and HINODE) gives the opportunity to investigate the details of
the flare emission at different wavelengths and can provide useful
hints to understand these phenomena and compare observations with
models. However, it is undoubted that sometimes the pointing to the
flaring region is not an easy task, due to the necessity to provide
the target coordinates to satellites with some hours in advance. Some
problems arising from this issue will be discussed. Moreover, new
projects related to flare catalogues and archives will be presented.
---------------------------------------------------------
Title: Evidence for a mixed mass composition at the 'ankle' in the
cosmic-ray spectrum
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Al Samarai,
I.; Albuquerque, I. F. M.; Allekotte, I.; Allison, P.; Almela, A.;
Alvarez Castillo, J.; Alvarez-Muñiz, J.; Ambrosio, M.; Anastasi,
G. A.; Anchordoqui, L.; Andrada, B.; Andringa, S.; Aramo, C.;
Arqueros, F.; Arsene, N.; Asorey, H.; Assis, P.; Aublin, J.; Avila,
G.; Badescu, A. M.; Balaceanu, A.; Baus, C.; Beatty, J. J.; Becker,
K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.; Biermann, P. L.;
Billoir, P.; Biteau, J.; Blaess, S. G.; Blanco, A.; Blazek, J.;
Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi, C.; Borodai,
N.; Botti, A. M.; Brack, J.; Brancus, I.; Bretz, T.; Bridgeman,
A.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi,
M.; Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga, L.; Cancio,
A.; Canfora, F.; Caramete, L.; Caruso, R.; Castellina, A.; Cataldi,
G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.; Chinellato,
J. A.; Chudoba, J.; Clay, R. W.; Colalillo, R.; Coleman, A.; Collica,
L.; Coluccia, M. R.; Conceição, R.; Contreras, F.; Cooper, M. J.;
Coutu, S.; Covault, C. E.; Cronin, J.; Dallier, R.; D'Amico, S.;
Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; de Almeida, R. M.;
de Jong, S. J.; De Mauro, G.; de Mello Neto, J. R. T.; De Mitri, I.;
de Oliveira, J.; de Souza, V.; Debatin, J.; del Peral, L.; Deligny,
O.; Di Giulio, C.; Di Matteo, A.; Díaz Castro, M. L.; Diogo, F.;
Dobrigkeit, C.; D'Olivo, J. C.; Dorofeev, A.; dos Anjos, R. C.; Dova,
M. T.; Dundovic, A.; Ebr, J.; Engel, R.; Erdmann, M.; Erfani, M.;
Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Falcke, H.; Fang, K.;
Farrar, G.; Fauth, A. C.; Fazzini, N.; Fick, B.; Figueira, J. M.;
Filevich, A.; Filipčič, A.; Fratu, O.; Freire, M. M.; Fujii, T.;
Fuster, A.; García, B.; Garcia-Pinto, D.; Gaté, F.; Gemmeke, H.;
Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller,
M.; Głas, D.; Glaser, C.; Glass, H.; Golup, G.; Gómez Berisso, M.;
Gómez Vitale, P. F.; González, N.; Gookin, B.; Gordon, J.; Gorgi,
A.; Gorham, P.; Gouffon, P.; Grillo, A. F.; Grubb, T. D.; Guarino,
F.; Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison,
T. A.; Harton, J. L.; Hasankiadeh, Q.; Haungs, A.; Hebbeker, T.; Heck,
D.; Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Holt, E.;
Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.;
Hulsman, J.; Insolia, A.; Isar, P. G.; Jandt, I.; Jansen, S.; Johnsen,
J. A.; Josebachuili, M.; Kääpä, A.; Kambeitz, O.; Kampert, K. H.;
Kasper, P.; Katkov, I.; Keilhauer, B.; Kemp, E.; Kieckhafer, R. M.;
Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.;
Kuempel, D.; Kukec Mezek, G.; Kunka, N.; Kuotb Awad, A.; LaHurd, D.;
Latronico, L.; Lauscher, M.; Lautridou, P.; Lebrun, P.; Legumina,
R.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon,
I.; Link, K.; Lopes, L.; López, R.; López Casado, A.; Luce, Q.;
Lucero, A.; Malacari, M.; Mallamaci, M.; Mandat, D.; Mantsch, P.;
Mariazzi, A. G.; Mariş, I. C.; Marsella, G.; Martello, D.; Martinez,
H.; Martínez Bravo, O.; Masías Meza, J. J.; Mathes, H. J.; Mathys,
S.; Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Mayotte, E.; Mazur,
P. O.; Medina, C.; Medina-Tanco, G.; Melo, D.; Menshikov, A.; Messina,
S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.; Miramonti, L.;
Mitrica, B.; Mockler, D.; Molina-Bueno, L.; Mollerach, S.; Montanet,
F.; Morello, C.; Mostafá, M.; Müller, G.; Muller, M. A.; Müller,
S.; Naranjo, I.; Navas, S.; Nellen, L.; Neuser, J.; Nguyen, P. H.;
Niculescu-Oglinzanu, M.; Niechciol, M.; Niemietz, L.; Niggemann,
T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, H.; Núñez, L. A.;
Ochilo, L.; Oikonomou, F.; Olinto, A.; Pakk Selmi-Dei, D.; Palatka,
M.; Pallotta, J.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.;
Pech, M.; Pedreira, F.; Pȩkala, J.; Pelayo, R.; Peña-Rodriguez, J.;
Pereira, L. A. S.; Perrone, L.; Peters, C.; Petrera, S.; Phuntsok,
J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello,
V.; Platino, M.; Plum, M.; Porowski, C.; Prado, R. R.; Privitera, P.;
Prouza, M.; Quel, E. J.; Querchfeld, S.; Quinn, S.; Ramos-Pollant, R.;
Rautenberg, J.; Ravel, O.; Ravignani, D.; Reinert, D.; Revenu, B.;
Ridky, J.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho,
W.; Rodriguez Fernandez, G.; Rodriguez Rojo, J.; Rodríguez-Frías,
M. D.; Rogozin, D.; Rosado, J.; Roth, M.; Roulet, E.; Rovero, A. C.;
Saffi, S. J.; Saftoiu, A.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Sanchez-Lucas, P.;
Santos, E. M.; Santos, E.; Sarazin, F.; Sarkar, B.; Sarmento, R.;
Sarmiento-Cano, C.; Sato, R.; Scarso, C.; Schauer, M.; Scherini, V.;
Schieler, H.; Schmidt, D.; Scholten, O.; Schovánek, P.; Schröder,
F. G.; Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto, S. J.; Segreto,
A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sigl, G.; Silli, G.;
Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers, P.;
Sonntag, S.; Sorokin, J.; Squartini, R.; Stanca, D.; Stanič, S.;
Stasielak, J.; Strafella, F.; Suarez, F.; Suarez Durán, M.; Sudholz,
T.; Suomijärvi, T.; Supanitsky, A. D.; Sutherland, M. S.; Swain,
J.; Szadkowski, Z.; Taborda, O. A.; Tapia, A.; Tepe, A.; Theodoro,
V. M.; Timmermans, C.; Todero Peixoto, C. J.; Tomankova, L.; Tomé,
B.; Tonachini, A.; Torralba Elipe, G.; Torres Machado, D.; Torri,
M.; Travnicek, P.; Trini, M.; Ulrich, R.; Unger, M.; Urban, M.;
Valbuena-Delgado, A.; Valdés Galicia, J. F.; Valiño, I.; Valore,
L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.; van Vliet,
A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.; Vázquez, J. R.;
Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha, J.; Villaseñor, L.;
Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz, D.; Watson, A. A.;
Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński, H.; Winchen, T.;
Wittkowski, D.; Wundheiler, B.; Wykes, S.; Yang, L.; Yelos, D.; Younk,
P.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zepeda, A.;
Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello, F.; Pierre
Auger Collaboration
2016PhLB..762..288A Altcode: 2016arXiv160908567T
We report a first measurement for ultrahigh energy cosmic rays
of the correlation between the depth of shower maximum and the
signal in the water Cherenkov stations of air-showers registered
simultaneously by the fluorescence and the surface detectors of the
Pierre Auger Observatory. Such a correlation measurement is a unique
feature of a hybrid air-shower observatory with sensitivity to both
the electromagnetic and muonic components. It allows an accurate
determination of the spread of primary masses in the cosmic-ray
flux. Up till now, constraints on the spread of primary masses have
been dominated by systematic uncertainties. The present correlation
measurement is not affected by systematics in the measurement of
the depth of shower maximum or the signal in the water Cherenkov
stations. The analysis relies on general characteristics of air showers
and is thus robust also with respect to uncertainties in hadronic
event generators. The observed correlation in the energy range around
the 'ankle' at lg (E /eV) = 18.5- 19.0 differs significantly
from expectations for pure primary cosmic-ray compositions. A light
composition made up of proton and helium only is equally inconsistent
with observations. The data are explained well by a mixed composition
including nuclei with mass A > 4. Scenarios such as the proton dip
model, with almost pure compositions, are thus disfavored as the sole
explanation of the ultrahigh-energy cosmic-ray flux at Earth.
---------------------------------------------------------
Title: The Pre-penumbral Magnetic Canopy in the Solar Atmosphere
Authors: MacTaggart, David; Guglielmino, Salvo L.; Zuccarello,
Francesca
2016ApJ...831L...4M Altcode: 2016arXiv161005554M
Penumbrae are the manifestation of magnetoconvection in highly inclined
(to the vertical direction) magnetic field. The penumbra of a sunspot
tends to form, initially, along the arc of the umbra antipodal to the
main region of flux emergence. The question of how highly inclined
magnetic field can concentrate along the antipodal curves of umbrae,
at least initially, remains to be answered. Previous observational
studies have suggested the existence of some form of overlying magnetic
canopy that acts as the progenitor for penumbrae. We propose that such
overlying magnetic canopies are a consequence of how the magnetic field
emerges into the atmosphere and are, therefore, part of the emerging
region. We show, through simulations of twisted flux tube emergence,
that canopies of highly inclined magnetic field form preferentially
at the required locations above the photosphere.
---------------------------------------------------------
Title: Testing Hadronic Interactions at Ultrahigh Energies with Air
Showers Measured by the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Al Samarai,
I.; Albuquerque, I. F. M.; Allekotte, I.; Allen, J. D.; Allison, P.;
Almela, A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Ambrosio, M.;
Anastasi, G. A.; Anchordoqui, L.; Andrada, B.; Andringa, S.; Aramo,
C.; Arqueros, F.; Arsene, N.; Asorey, H.; Assis, P.; Aublin, J.;
Avila, G.; Badescu, A. M.; Baus, C.; Beatty, J. J.; Becker, K. H.;
Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann,
P. L.; Billoir, P.; Biteau, J.; Blaess, S. G.; Blanco, A.; Blazek,
J.; Bleve, C.; Blümer, H.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Botti, A. M.; Brack, J.; Brancus, I.; Bretz, T.;
Bridgeman, A.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink, S.;
Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga, L.;
Cancio, A.; Canfora, F.; Caramete, L.; Caruso, R.; Castellina, A.;
Cataldi, G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.;
Chinellato, J. A.; Chirinos Diaz, J. C.; Chudoba, J.; Clay, R. W.;
Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição,
R.; Contreras, F.; Cooper, M. J.; Coutu, S.; Covault, C. E.; Cronin,
J.; Dallier, R.; D'Amico, S.; Daniel, B.; Dasso, S.; Daumiller, K.;
Dawson, B. R.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.; de
Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza, V.;
Debatin, J.; del Peral, L.; Deligny, O.; Dhital, N.; Di Giulio, C.;
Di Matteo, A.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo,
J. C.; Dorofeev, A.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr,
J.; Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.;
Etchegoyen, A.; Falcke, H.; Fang, K.; Farrar, G. R.; Fauth, A. C.;
Fazzini, N.; Ferguson, A. P.; Fick, B.; Figueira, J. M.; Filevich,
A.; Filipčič, A.; Fratu, O.; Freire, M. M.; Fujii, T.; Fuster,
A.; Gallo, F.; García, B.; Garcia-Pinto, D.; Gate, F.; Gemmeke, H.;
Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller,
M.; Głas, D.; Glaser, C.; Glass, H.; Golup, G.; Gómez Berisso, M.;
Gómez Vitale, P. F.; González, N.; Gookin, B.; Gordon, J.; Gorgi, A.;
Gorham, P.; Gouffon, P.; Griffith, N.; Grillo, A. F.; Grubb, T. D.;
Guarino, F.; Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.;
Harrison, T. A.; Harton, J. L.; Hasankiadeh, Q.; Haungs, A.; Hebbeker,
T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.;
Hollon, N.; Holt, E.; Homola, P.; Hörandel, J. R.; Horvath, P.;
Hrabovský, M.; Huege, T.; Hulsman, J.; Insolia, A.; Isar, P. G.;
Jandt, I.; Jansen, S.; Jarne, C.; Johnsen, J. A.; Josebachuili, M.;
Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.;
Keilhauer, B.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges,
M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Kuempel, D.; Kukec Mezek,
G.; Kunka, N.; Kuotb Awad, A.; LaHurd, D.; Latronico, L.; Lauscher, M.;
Lautridou, P.; Lebrun, P.; Legumina, R.; Leigui de Oliveira, M. A.;
Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; Lopes, L.; López,
R.; López Casado, A.; Lucero, A.; Malacari, M.; Mallamaci, M.; Mandat,
D.; Mantsch, P.; Mariazzi, A. G.; Marin, V.; Mariş, I. C.; Marsella,
G.; Martello, D.; Martinez, H.; Martínez Bravo, O.; Masías Meza,
J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.;
Matthiae, G.; Maurizio, D.; Mayotte, E.; Mazur, P. O.; Medina, C.;
Medina-Tanco, G.; Mello, V. B. B.; Melo, D.; Menshikov, A.; Messina,
S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.; Miramonti,
L.; Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Montanet, F.;
Morello, C.; Mostafá, M.; Moura, C. A.; Müller, G.; Muller, M. A.;
Müller, S.; Naranjo, I.; Navas, S.; Necesal, P.; Nellen, L.; Nelles,
A.; Neuser, J.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol,
M.; Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.;
Nožka, H.; Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.;
Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Papenbreer, P.; Parente,
G.; Parra, A.; Paul, T.; Pech, M.; Pedreira, F.; Pekala, J.; Pelayo,
R.; Peña-Rodriguez, J.; Pepe, I. M.; Pereira, L. A. S.; Perrone,
L.; Petermann, E.; Peters, C.; Petrera, S.; Phuntsok, J.; Piegaia,
R.; Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello, V.; Platino,
M.; Plum, M.; Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.;
Quel, E. J.; Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.;
Ravignani, D.; Revenu, B.; Ridky, J.; Risse, M.; Ristori, P.; Rizi,
V.; Rodrigues de Carvalho, W.; Rodriguez Rojo, J.; Rodríguez-Frías,
M. D.; Rogozin, D.; Rosado, J.; Roth, M.; Roulet, E.; Rovero, A. C.;
Saffi, S. J.; Saftoiu, A.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Sanchez-Lucas, P.;
Santos, E. M.; Santos, E.; Sarazin, F.; Sarkar, B.; Sarmento, R.;
Sarmiento-Cano, C.; Sato, R.; Scarso, C.; Schauer, M.; Scherini, V.;
Schieler, H.; Schmidt, D.; Scholten, O.; Schoorlemmer, H.; Schovánek,
P.; Schröder, F. G.; Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto,
S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sigl,
G.; Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers,
P.; Sonntag, S.; Sorokin, J.; Squartini, R.; Stanca, D.; Stanič,
S.; Stapleton, J.; Stasielak, J.; Strafella, F.; Stutz, A.; Suarez,
F.; Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky,
A. D.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Taborda, O. A.;
Tapia, A.; Tepe, A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Tomankova, L.; Tomé, B.; Tonachini, A.; Torralba Elipe, G.;
Torres Machado, D.; Travnicek, P.; Trini, M.; Ulrich, R.; Unger, M.;
Urban, M.; Valbuena-Delgado, A.; Valdés Galicia, J. F.; Valiño,
I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.;
van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.; Vázquez,
J. R.; Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha, J.; Videla,
M.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz,
D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński,
H.; Winchen, T.; Wittkowski, D.; Wundheiler, B.; Wykes, S.; Yang,
L.; Yapici, T.; Yelos, D.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello,
F.; Pierre Auger Collaboration
2016PhRvL.117s2001A Altcode: 2016arXiv161008509T
Ultrahigh energy cosmic ray air showers probe particle physics at
energies beyond the reach of accelerators. Here we introduce a new
method to test hadronic interaction models without relying on the
absolute energy calibration, and apply it to events with primary
energy 6-16 EeV (E<SUB>CM</SUB>=110 - 170 TeV ), whose longitudinal
development and lateral distribution were simultaneously measured by
the Pierre Auger Observatory. The average hadronic shower is 1.33 ±0.16
(1.61 ±0.21 ) times larger than predicted using the leading LHC-tuned
models EPOS-LHC (QGSJetII-04), with a corresponding excess of muons.
---------------------------------------------------------
Title: Search for ultrarelativistic magnetic monopoles with the
Pierre Auger observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Al Samarai, I.;
Albuquerque, I. F. M.; Allekotte, I.; Almela, A.; Alvarez Castillo,
J.; Alvarez-Muñiz, J.; Ambrosio, M.; Anastasi, G. A.; Anchordoqui,
L.; Andrada, B.; Andringa, S.; Aramo, C.; Arqueros, F.; Arsene,
N.; Asorey, H.; Assis, P.; Aublin, J.; Avila, G.; Badescu, A. M.;
Balaceanu, A.; Barreira Luz, R. J.; Baus, C.; Beatty, J. J.; Becker,
K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.;
Biermann, P. L.; Billoir, P.; Biteau, J.; Blaess, S. G.; Blanco,
A.; Blazek, J.; Bleve, C.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Botti, A. M.; Brack, J.; Brancus, I.; Bretz, T.;
Bridgeman, A.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink,
S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, L.; Cancio, A.;
Canfora, F.; Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.;
Cazon, L.; Cester, R.; Chavez, A. G.; Chinellato, J. A.; Chudoba, J.;
Clay, R. W.; Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.;
Conceição, R.; Contreras, F.; Cooper, M. J.; Coutu, S.; Covault,
C. E.; Cronin, J.; D'Amico, S.; Daniel, B.; Dasso, S.; Daumiller,
K.; Dawson, B. R.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza,
V.; Debatin, J.; Deligny, O.; Di Giulio, C.; Di Matteo, A.; Díaz
Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.; Dorofeev,
A.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.;
Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen,
A.; Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Fick,
B.; Figueira, J. M.; Filipčič, A.; Fratu, O.; Freire, M. M.; Fujii,
T.; Fuster, A.; Gaior, R.; García, B.; Garcia-Pinto, D.; Gaté, F.;
Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; Giammarchi,
M.; Giller, M.; Głas, D.; Glaser, C.; Glass, H.; Golup, G.; Gómez
Berisso, M.; Gómez Vitale, P. F.; González, N.; Gookin, B.; Gorgi,
A.; Gorham, P.; Gouffon, P.; Grillo, A. F.; Grubb, T. D.; Guarino, F.;
Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison, T. A.;
Harton, J. L.; Hasankiadeh, Q.; Haungs, A.; Hebbeker, T.; Heck, D.;
Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Holt, E.; Homola,
P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman,
J.; Insolia, A.; Isar, P. G.; Jandt, I.; Jansen, S.; Johnsen, J. A.;
Josebachuili, M.; Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper,
P.; Katkov, I.; Keilhauer, B.; Kemp, E.; Kemp, J.; Kieckhafer, R. M.;
Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.;
Kuempel, D.; Kukec Mezek, G.; Kunka, N.; Kuotb Awad, A.; LaHurd, D.;
Lauscher, M.; Lebrun, P.; Legumina, R.; Leigui de Oliveira, M. A.;
Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; Lopes, L.; López, R.;
López Casado, A.; Luce, Q.; Lucero, A.; Malacari, M.; Mallamaci, M.;
Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Mariş, I. C.; Marsella, G.;
Martello, D.; Martinez, H.; Martínez Bravo, O.; Masías Meza, J. J.;
Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.; Matthiae,
G.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Melo,
D.; Menshikov, A.; Messina, S.; Micheletti, M. I.; Middendorf, L.;
Minaya, I. A.; Miramonti, L.; Mitrica, B.; Mockler, D.; Molina-Bueno,
L.; Mollerach, S.; Montanet, F.; Morello, C.; Mostafá, M.; Müller,
G.; Muller, M. A.; Müller, S.; Naranjo, I.; Nellen, L.; Neuser, J.;
Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.; Niemietz, L.;
Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka, H.; Núñez,
L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Pakk Selmi-Dei, D.;
Palatka, M.; Pallotta, J.; Papenbreer, P.; Parente, G.; Parra,
A.; Paul, T.; Pech, M.; Pedreira, F.; Pękala, J.; Pelayo, R.;
Peña-Rodriguez, J.; Pereira, L. A. S.; Perrone, L.; Peters, C.;
Petrera, S.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.;
Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.; Porowski, C.;
Prado, R. R.; Privitera, P.; Prouza, M.; Quel, E. J.; Querchfeld,
S.; Quinn, S.; Ramos-Pollan, R.; Rautenberg, J.; Ravignani, D.;
Reinert, D.; Revenu, B.; Ridky, J.; Risse, M.; Ristori, P.; Rizi, V.;
Rodrigues de Carvalho, W.; Rodriguez Fernandez, G.; Rodriguez Rojo,
J.; Rogozin, D.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus,
F.; Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Sanchez-Lucas,
P.; Santos, E. M.; Santos, E.; Sarazin, F.; Sarkar, B.; Sarmento,
R.; Sarmiento, C. A.; Sato, R.; Schauer, M.; Scherini, V.; Schieler,
H.; Schimp, M.; Schmidt, D.; Scholten, O.; Schovánek, P.; Schröder,
F. G.; Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto, S. J.; Segreto,
A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sigl, G.; Silli, G.;
Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers, P.;
Sonntag, S.; Sorokin, J.; Squartini, R.; Stanca, D.; Stanič, S.;
Stasielak, J.; Stassi, P.; Strafella, F.; Suarez, F.; Suarez Durán,
M.; Sudholz, T.; Suomijärvi, T.; Supanitsky, A. D.; Swain, J.;
Szadkowski, Z.; Taboada, A.; Taborda, O. A.; Tapia, A.; Theodoro,
V. M.; Timmermans, C.; Todero Peixoto, C. J.; Tomankova, L.; Tomé,
B.; Torralba Elipe, G.; Torres Machado, D.; Torri, M.; Travnicek, P.;
Trini, M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.;
Valiño, I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg,
A. M.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.;
Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Vergara Quispe, I. D.;
Verzi, V.; Vicha, J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.;
Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke,
L.; Wilczyński, H.; Winchen, T.; Wittkowski, D.; Wundheiler, B.;
Wykes, S.; Yang, L.; Yelos, D.; Yushkov, A.; Zas, E.; Zavrtanik, D.;
Zavrtanik, M.; Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.;
Zuccarello, F.; Pierre Auger Collaboration
2016PhRvD..94h2002A Altcode: 2016arXiv160904451T
We present a search for ultrarelativistic magnetic monopoles with the
Pierre Auger observatory. Such particles, possibly a relic of phase
transitions in the early Universe, would deposit a large amount of
energy along their path through the atmosphere, comparable to that
of ultrahigh-energy cosmic rays (UHECRs). The air-shower profile
of a magnetic monopole can be effectively distinguished by the
fluorescence detector from that of standard UHECRs. No candidate was
found in the data collected between 2004 and 2012, with an expected
background of less than 0.1 event from UHECRs. The corresponding 90%
confidence level (C.L.) upper limits on the flux of ultrarelativistic
magnetic monopoles range from 10<SUP>-19</SUP>(cm<SUP>2</SUP> sr
s )<SUP>-1</SUP> for a Lorentz factor γ =1 0<SUP>9</SUP> to 2.5
×10<SUP>-21</SUP>(cm<SUP>2</SUP> sr s )<SUP>-1</SUP> for γ =1
0<SUP>12</SUP>. These results—the first obtained with a UHECR
detector—improve previously published limits by up to an order
of magnitude.
---------------------------------------------------------
Title: Kinematics and Magnetic Properties of a Light Bridge in a
Decaying Sunspot
Authors: Falco, M.; Borrero, J. M.; Guglielmino, S. L.; Romano, P.;
Zuccarello, F.; Criscuoli, S.; Cristaldi, A.; Ermolli, I.; Jafarzadeh,
S.; Rouppe van der Voort, L.
2016SoPh..291.1939F Altcode: 2016arXiv160607229F; 2016SoPh..tmp..107F
We present the results obtained by analysing high spatial and spectral
resolution data of the solar photosphere acquired by the CRisp Imaging
SpectroPolarimeter at the Swedish Solar Telescope on 6 August 2011 of a
large sunspot with a light bridge (LB) observed in NOAA AR 11263. These
data are complemented by simultaneous Hinode Spectropolarimeter (SP)
observation in the Fe I 630.15 nm and 630.25 nm lines. The continuum
intensity map shows a discontinuity in the radial distribution of the
penumbral filaments in correspondence with the LB, which shows a dark
lane (≈0.3<SUP>″</SUP> wide and ≈8.0<SUP>″</SUP> long) along its
main axis. The available data were inverted with the Stokes Inversion
based on Response functions (SIR) code and physical parameters maps were
obtained. The line-of-sight (LOS) velocity of the plasma along the LB
derived from the Doppler effect shows motions towards and away from the
observer up to 0.6 kms−<SUP>1</SUP> that are lower in value than the
LOS velocities observed in the neighbouring penumbral filaments. The
noteworthy result is that we find motions towards the observer of up to
0.6 kms−<SUP>1</SUP> in the dark lane where the LB is located between
two umbral cores, while the LOS velocity motion towards the observer
is strongly reduced where the LB is located between an umbral core
at one side and penumbral filaments on the other side. Statistically,
the LOS velocities correspond to upflows or downflows, and comparing
these results with Hinode/SP data, we conclude that the surrounding
magnetic field configuration (whether more or less inclined) could have
a role in maintaining the conditions for the process of plasma pile-up
along the dark lane. The results obtained from our study support and
confirm outcomes of recent magneto-hydrodynamic simulations showing
upflows along the main axis of an LB.
---------------------------------------------------------
Title: Formation of the Penumbra and Start of the Evershed Flow
Authors: Murabito, M.; Romano, P.; Guglielmino, S. L.; Zuccarello,
F.; Solanki, S. K.
2016ApJ...825...75M Altcode: 2016arXiv160405610M
We studied the variations of line of sight photospheric plasma flows
during the formation phase of the penumbra around a pore in active
region NOAA 11490. We used a high spatial, spectral, and temporal
resolution data set acquired by the Interferometric BIdimensional
Spectrometer operating at the NSO/Dunn Solar Telescope as well as
data taken by the Helioseismic and Magnetic Imager on board the
Solar Dynamics Observatory satellite (SDO/HMI). Before the penumbra
formed we observed a redshift of the spectral line in the inner part
of the annular zone surrounding the pore as well as a blueshift of
material associated with opposite magnetic polarity farther away from
the pore. We found that the onset of the classical Evershed flow
occurs on a very short timescale (1 to 3 hr) while the penumbra is
forming. During the same time interval we found changes in the magnetic
field inclination in the penumbra, with the vertical field actually
changing sign near the penumbral edge, while the total magnetic field
showed a significant increase, about 400 G. To explain these and other
observations related to the formation of the penumbra and the onset
of the Evershed flow we propose a scenario in which the penumbra is
formed by magnetic flux dragged down from the canopy surrounding the
initial pore. The Evershed flow starts when the sinking magnetic field
dips below the solar surface and magnetoconvection sets in.
---------------------------------------------------------
Title: Measurement of the Radiation Energy in the Radio Signal of
Extensive Air Showers as a Universal Estimator of Cosmic-Ray Energy
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Al Samarai,
I.; Albuquerque, I. F. M.; Allekotte, I.; Allison, P.; Almela, A.;
Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves Batista, R.; Ambrosio,
M.; Aminaei, A.; Anastasi, G. A.; Anchordoqui, L.; Andringa, S.; Aramo,
C.; Arqueros, F.; Arsene, N.; Asorey, H.; Assis, P.; Aublin, J.; Avila,
G.; Awal, N.; Badescu, A. M.; Baus, C.; Beatty, J. J.; Becker, K. H.;
Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann,
P. L.; Billoir, P.; Blaess, S. G.; Blanco, A.; Blanco, M.; Blazek,
J.; Bleve, C.; Blümer, H.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Brack, J.; Brancus, I.; Bretz, T.; Bridgeman, A.;
Brogueira, P.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.;
Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga, L.; Candusso, M.;
Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.; Cazon, L.;
Cester, R.; Chavez, A. G.; Chiavassa, A.; Chinellato, J. A.; Chudoba,
J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.; Colalillo, R.; Coleman,
A.; Collica, L.; Coluccia, M. R.; Conceição, R.; Contreras, F.;
Cooper, M. J.; Cordier, A.; Coutu, S.; Covault, C. E.; Cronin, J.;
Dallier, R.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.;
de Almeida, R. M.; de Jong, S. J.; De Mauro, G.; de Mello Neto,
J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza, V.; del Peral,
L.; Deligny, O.; Dhital, N.; Di Giulio, C.; Di Matteo, A.; Diaz,
J. C.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; Docters, W.;
D'Olivo, J. C.; Dorofeev, A.; Dorosti Hasankiadeh, Q.; dos Anjos,
R. C.; Dova, M. T.; Ebr, J.; Engel, R.; Erdmann, M.; Erfani, M.;
Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Falcke, H.; Fang, K.;
Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Fick, B.;
Figueira, J. M.; Filevich, A.; Filipčič, A.; Fratu, O.; Freire,
M. M.; Fujii, T.; García, B.; Garcia-Gamez, D.; Garcia-Pinto, D.;
Gate, F.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.;
Giammarchi, M.; Giller, M.; Głas, D.; Glaser, C.; Glass, H.; Golup,
G.; Gómez Berisso, M.; Gómez Vitale, P. F.; González, N.; Gookin,
B.; Gordon, J.; Gorgi, A.; Gorham, P.; Gouffon, P.; Griffith, N.;
Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel, M. R.;
Hansen, P.; Harari, D.; Harrison, T. A.; Hartmann, S.; Harton, J. L.;
Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill,
G. C.; Hojvat, C.; Hollon, N.; Holt, E.; Homola, P.; Hörandel, J. R.;
Horvath, P.; Hrabovský, M.; Huber, D.; Huege, T.; Insolia, A.; Isar,
P. G.; Jandt, I.; Jansen, S.; Jarne, C.; Johnsen, J. A.; Josebachuili,
M.; Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.;
Keilhauer, B.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges,
M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Kuempel, D.; Kukec Mezek,
G.; Kunka, N.; Kuotb Awad, A. W.; LaHurd, D.; Latronico, L.; Lauer,
R.; Lauscher, M.; Lautridou, P.; Le Coz, S.; Lebrun, D.; Lebrun, P.;
Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link,
K.; Lopes, L.; López, R.; López Casado, A.; Louedec, K.; Lucero,
A.; Malacari, M.; Mallamaci, M.; Maller, J.; Mandat, D.; Mantsch, P.;
Mariazzi, A. G.; Marin, V.; Mariş, I. C.; Marsella, G.; Martello,
D.; Martinez, H.; Martínez Bravo, O.; Martraire, D.; Masías Meza,
J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.;
Matthiae, G.; Maurizio, D.; Mayotte, E.; Mazur, P. O.; Medina, C.;
Medina-Tanco, G.; Meissner, R.; Mello, V. B. B.; Melo, D.; Menshikov,
A.; Messina, S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.;
Miramonti, L.; Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Montanet,
F.; Morello, C.; Mostafá, M.; Moura, C. A.; Muller, M. A.; Müller,
G.; Müller, S.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.;
Neuser, J.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.;
Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka,
L.; Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Pacheco,
N.; Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Papenbreer, P.;
Parente, G.; Parra, A.; Paul, T.; Pech, M.; Pękala, J.; Pelayo,
R.; Pepe, I. M.; Perrone, L.; Petermann, E.; Peters, C.; Petrera,
S.; Petrov, Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.;
Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.; Porcelli, A.;
Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Quel, E. J.;
Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.;
Reinert, D.; Revenu, B.; Ridky, J.; Risse, M.; Ristori, P.; Rizi,
V.; Rodrigues de Carvalho, W.; Rodriguez Rojo, J.; Rodríguez-Frías,
M. D.; Rogozin, D.; Rosado, J.; Roth, M.; Roulet, E.; Rovero, A. C.;
Saffi, S. J.; Saftoiu, A.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Sanchez-Lucas, P.;
Santos, E.; Santos, E. M.; Sarazin, F.; Sarkar, B.; Sarmento, R.;
Sarmiento-Cano, C.; Sato, R.; Scarso, C.; Schauer, M.; Scherini, V.;
Schieler, H.; Schmidt, D.; Scholten, O.; Schoorlemmer, H.; Schovánek,
P.; Schröder, F. G.; Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto,
S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sigl,
G.; Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers,
P.; Sonntag, S.; Sorokin, J.; Squartini, R.; Srivastava, Y. N.;
Stanca, D.; Stanič, S.; Stapleton, J.; Stasielak, J.; Stephan, M.;
Stutz, A.; Suarez, F.; Suarez Durán, M.; Suomijärvi, T.; Supanitsky,
A. D.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Taborda, O. A.;
Tapia, A.; Tepe, A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Toma, G.; Tomankova, L.; Tomé, B.; Tonachini, A.; Torralba
Elipe, G.; Torres Machado, D.; Travnicek, P.; Trini, M.; Ulrich, R.;
Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore,
L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.; van Velzen,
S.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.;
Vasquez, R.; Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Verzi,
V.; Vicha, J.; Videla, M.; Villaseñor, L.; Vlcek, B.; Vorobiov,
S.; Wahlberg, H.; Wainberg, O.; Walz, D.; Watson, A. A.; Weber,
M.; Weidenhaupt, K.; Weindl, A.; Welling, C.; Werner, F.; Widom, A.;
Wiencke, L.; Wilczyński, H.; Winchen, T.; Wittkowski, D.; Wundheiler,
B.; Wykes, S.; Yang, L.; Yapici, T.; Yushkov, A.; Zas, E.; Zavrtanik,
D.; Zavrtanik, M.; Zepeda, A.; Zimmermann, B.; Ziolkowski, M.;
Zuccarello, F.; Pierre Auger Collaboration
2016PhRvL.116x1101A Altcode: 2016arXiv160502564T
We measure the energy emitted by extensive air showers in the form of
radio emission in the frequency range from 30 to 80 MHz. Exploiting
the accurate energy scale of the Pierre Auger Observatory, we obtain
a radiation energy of 15.8 ±0.7 (stat)±6.7 (syst) MeV for cosmic
rays with an energy of 1 EeV arriving perpendicularly to a geomagnetic
field of 0.24 G, scaling quadratically with the cosmic-ray energy. A
comparison with predictions from state-of-the-art first-principles
calculations shows agreement with our measurement. The radiation energy
provides direct access to the calorimetric energy in the electromagnetic
cascade of extensive air showers. Comparison with our result thus
allows the direct calibration of any cosmic-ray radio detector against
the well-established energy scale of the Pierre Auger Observatory.
---------------------------------------------------------
Title: Energy estimation of cosmic rays with the Engineering Radio
Array of the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Al Samarai,
I.; Albuquerque, I. F. M.; Allekotte, I.; Allison, P.; Almela, A.;
Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves Batista, R.; Ambrosio,
M.; Aminaei, A.; Anastasi, G. A.; Anchordoqui, L.; Andringa, S.; Aramo,
C.; Arqueros, F.; Arsene, N.; Asorey, H.; Assis, P.; Aublin, J.; Avila,
G.; Awal, N.; Badescu, A. M.; Baus, C.; Beatty, J. J.; Becker, K. H.;
Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann,
P. L.; Billoir, P.; Blaess, S. G.; Blanco, A.; Blanco, M.; Blazek,
J.; Bleve, C.; Blümer, H.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Brack, J.; Brancus, I.; Bretz, T.; Bridgeman, A.;
Brogueira, P.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.;
Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga, L.; Candusso, M.;
Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.; Cazon, L.;
Cester, R.; Chavez, A. G.; Chiavassa, A.; Chinellato, J. A.; Chudoba,
J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.; Colalillo, R.; Coleman,
A.; Collica, L.; Coluccia, M. R.; Conceição, R.; Contreras, F.;
Cooper, M. J.; Cordier, A.; Coutu, S.; Covault, C. E.; Cronin, J.;
Dallier, R.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.;
de Almeida, R. M.; de Jong, S. J.; De Mauro, G.; de Mello Neto,
J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza, V.; del Peral,
L.; Deligny, O.; Dhital, N.; Di Giulio, C.; Di Matteo, A.; Diaz,
J. C.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; Docters, W.;
D'Olivo, J. C.; Dorofeev, A.; Dorosti Hasankiadeh, Q.; dos Anjos,
R. C.; Dova, M. T.; Ebr, J.; Engel, R.; Erdmann, M.; Erfani, M.;
Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Falcke, H.; Fang, K.;
Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Fick, B.;
Figueira, J. M.; Filevich, A.; Filipčič, A.; Fratu, O.; Freire,
M. M.; Fujii, T.; García, B.; Garcia-Gamez, D.; Garcia-Pinto, D.;
Gate, F.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.;
Giammarchi, M.; Giller, M.; Głas, D.; Glaser, C.; Glass, H.; Golup,
G.; Gómez Berisso, M.; Gómez Vitale, P. F.; González, N.; Gookin,
B.; Gordon, J.; Gorgi, A.; Gorham, P.; Gouffon, P.; Griffith, N.;
Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel, M. R.;
Hansen, P.; Harari, D.; Harrison, T. A.; Hartmann, S.; Harton, J. L.;
Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill,
G. C.; Hojvat, C.; Hollon, N.; Holt, E.; Homola, P.; Hörandel, J. R.;
Horvath, P.; Hrabovský, M.; Huber, D.; Huege, T.; Insolia, A.; Isar,
P. G.; Jandt, I.; Jansen, S.; Jarne, C.; Johnsen, J. A.; Josebachuili,
M.; Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.;
Keilhauer, B.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges,
M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Kuempel, D.; Kukec Mezek,
G.; Kunka, N.; Kuotb Awad, A. W.; LaHurd, D.; Latronico, L.; Lauer,
R.; Lauscher, M.; Lautridou, P.; Le Coz, S.; Lebrun, D.; Lebrun, P.;
Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link,
K.; Lopes, L.; López, R.; López Casado, A.; Louedec, K.; Lucero,
A.; Malacari, M.; Mallamaci, M.; Maller, J.; Mandat, D.; Mantsch, P.;
Mariazzi, A. G.; Marin, V.; Mariş, I. C.; Marsella, G.; Martello,
D.; Martinez, H.; Martínez Bravo, O.; Martraire, D.; Masías Meza,
J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.;
Matthiae, G.; Maurizio, D.; Mayotte, E.; Mazur, P. O.; Medina, C.;
Medina-Tanco, G.; Meissner, R.; Mello, V. B. B.; Melo, D.; Menshikov,
A.; Messina, S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.;
Miramonti, L.; Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Montanet,
F.; Morello, C.; Mostafá, M.; Moura, C. A.; Muller, M. A.; Müller,
G.; Müller, S.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.;
Neuser, J.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.;
Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka,
L.; Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Pacheco,
N.; Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Papenbreer, P.;
Parente, G.; Parra, A.; Paul, T.; Pech, M.; Pękala, J.; Pelayo,
R.; Pepe, I. M.; Perrone, L.; Petermann, E.; Peters, C.; Petrera,
S.; Petrov, Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.;
Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.; Porcelli, A.;
Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Quel, E. J.;
Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.;
Reinert, D.; Revenu, B.; Ridky, J.; Risse, M.; Ristori, P.; Rizi,
V.; Rodrigues de Carvalho, W.; Rodriguez Rojo, J.; Rodríguez-Frías,
M. D.; Rogozin, D.; Rosado, J.; Roth, M.; Roulet, E.; Rovero, A. C.;
Saffi, S. J.; Saftoiu, A.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Sanchez-Lucas, P.;
Santos, E.; Santos, E. M.; Sarazin, F.; Sarkar, B.; Sarmento, R.;
Sarmiento-Cano, C.; Sato, R.; Scarso, C.; Schauer, M.; Scherini, V.;
Schieler, H.; Schmidt, D.; Scholten, O.; Schoorlemmer, H.; Schovánek,
P.; Schröder, F. G.; Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto,
S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sigl,
G.; Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers,
P.; Sonntag, S.; Sorokin, J.; Squartini, R.; Srivastava, Y. N.;
Stanca, D.; Stanič, S.; Stapleton, J.; Stasielak, J.; Stephan, M.;
Stutz, A.; Suarez, F.; Suarez Durán, M.; Suomijärvi, T.; Supanitsky,
A. D.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Taborda, O. A.;
Tapia, A.; Tepe, A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Toma, G.; Tomankova, L.; Tomé, B.; Tonachini, A.; Torralba
Elipe, G.; Torres Machado, D.; Travnicek, P.; Trini, M.; Ulrich, R.;
Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore,
L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.; van Velzen,
S.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.;
Vasquez, R.; Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Verzi,
V.; Vicha, J.; Videla, M.; Villaseñor, L.; Vlcek, B.; Vorobiov,
S.; Wahlberg, H.; Wainberg, O.; Walz, D.; Watson, A. A.; Weber,
M.; Weidenhaupt, K.; Weindl, A.; Welling, C.; Werner, F.; Widom, A.;
Wiencke, L.; Wilczyński, H.; Winchen, T.; Wittkowski, D.; Wundheiler,
B.; Wykes, S.; Yang, L.; Yapici, T.; Yushkov, A.; Zas, E.; Zavrtanik,
D.; Zavrtanik, M.; Zepeda, A.; Zimmermann, B.; Ziolkowski, M.;
Zuccarello, F.; Pierre Auger Collaboration
2016PhRvD..93l2005A Altcode: 2015arXiv150804267T
The Auger Engineering Radio Array (AERA) is part of the Pierre Auger
Observatory and is used to detect the radio emission of cosmic-ray air
showers. These observations are compared to the data of the surface
detector stations of the Observatory, which provide well-calibrated
information on the cosmic-ray energies and arrival directions. The
response of the radio stations in the 30-80 MHz regime has been
thoroughly calibrated to enable the reconstruction of the incoming
electric field. For the latter, the energy deposit per area is
determined from the radio pulses at each observer position and is
interpolated using a two-dimensional function that takes into account
signal asymmetries due to interference between the geomagnetic and
charge-excess emission components. The spatial integral over the signal
distribution gives a direct measurement of the energy transferred
from the primary cosmic ray into radio emission in the AERA frequency
range. We measure 15.8 MeV of radiation energy for a 1 EeV air shower
arriving perpendicularly to the geomagnetic field. This radiation
energy—corrected for geometrical effects—is used as a cosmic-ray
energy estimator. Performing an absolute energy calibration against
the surface-detector information, we observe that this radio-energy
estimator scales quadratically with the cosmic-ray energy as expected
for coherent emission. We find an energy resolution of the radio
reconstruction of 22% for the data set and 17% for a high-quality subset
containing only events with at least five radio stations with signal.
---------------------------------------------------------
Title: Azimuthal asymmetry in the risetime of the surface detector
signals of the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Al Samarai,
I.; Albuquerque, I. F. M.; Allekotte, I.; Allison, P.; Almela,
A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves Batista, R.;
Ambrosio, M.; Anchordoqui, L.; Andrada, B.; Andringa, S.; Aramo, C.;
Arqueros, F.; Arsene, N.; Asorey, H.; Assis, P.; Aublin, J.; Avila,
G.; Awal, N.; Badescu, A. M.; Baus, C.; Beatty, J. J.; Becker, K. H.;
Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann,
P. L.; Billoir, P.; Blaess, S. G.; Blanco, A.; Blazek, J.; Bleve, C.;
Blümer, H.; Boháčová, M.; Boncioli, D.; Bonifazi, C.; Borodai,
N.; Botti, A. M.; Brack, J.; Brancus, I.; Bretz, T.; Bridgeman, A.;
Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.;
Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga, L.; Cancio, A.;
Candusso, M.; Caramete, L.; Caruso, R.; Castellina, A.; Cataldi,
G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.; Chinellato,
J. A.; Chirinos Diaz, J. C.; Chudoba, J.; Clay, R. W.; Colalillo, R.;
Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição, R.; Contreras,
F.; Cooper, M. J.; Coutu, S.; Covault, C. E.; Cronin, J.; Dallier, R.;
D'Amico, S.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; de
Almeida, R. M.; de Jong, S. J.; De Mauro, G.; de Mello Neto, J. R. T.;
De Mitri, I.; de Oliveira, J.; de Souza, V.; Debatin, J.; Deligny,
O.; Dhital, N.; Di Giulio, C.; Di Matteo, A.; Díaz Castro, M. L.;
Diogo, F.; Dobrigkeit, C.; Docters, W.; D'Olivo, J. C.; Dorofeev,
A.; dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.; Engel, R.;
Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.;
Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson,
A. P.; Fick, B.; Figueira, J. M.; Filevich, A.; Filipčič, A.; Fratu,
O.; Freire, M. M.; Fujii, T.; Fuster, A.; Gallo, F.; García, B.;
Garcia-Pinto, D.; Gate, F.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia,
P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Głas, D.; Glaser,
C.; Glass, H.; Golup, G.; Gómez Berisso, M.; Gómez Vitale, P. F.;
González, N.; Gookin, B.; Gordon, J.; Gorgi, A.; Gorham, P.; Gouffon,
P.; Griffith, N.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes,
G. P.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Harton,
J. L.; Hasankiadeh, Q.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann,
P.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Hollon, N.; Holt, E.;
Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.;
Insolia, A.; Isar, P. G.; Jandt, I.; Jansen, S.; Jarne, C.; Johnsen,
J. A.; Josebachuili, M.; Kääpä, A.; Kambeitz, O.; Kampert, K. H.;
Kasper, P.; Katkov, I.; Keilhauer, B.; Kemp, E.; Kieckhafer, R. M.;
Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm,
N.; Kuempel, D.; Kukec Mezek, G.; Kunka, N.; Kuotb Awad, A.; LaHurd,
D.; Latronico, L.; Lauscher, M.; Lautridou, P.; Lebrun, P.; Leigui
de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.;
Lopes, L.; López, R.; López Casado, A.; Lucero, A.; Malacari, M.;
Mallamaci, M.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, V.;
Mariş, I. C.; Marsella, G.; Martello, D.; Martinez, H.; Martínez
Bravo, O.; Masías Meza, J. J.; Mathes, H. J.; Mathys, S.; Matthews,
J.; Matthews, J. A. J.; Matthiae, G.; Maurizio, D.; Mayotte, E.;
Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Mello, V. B. B.; Melo,
D.; Menshikov, A.; Messina, S.; Micheletti, M. I.; Middendorf, L.;
Minaya, I. A.; Miramonti, L.; Mitrica, B.; Molina-Bueno, L.; Mollerach,
S.; Montanet, F.; Morello, C.; Mostafá, M.; Moura, C. A.; Müller,
G.; Muller, M. A.; Müller, S.; Naranjo, I.; Navas, S.; Necesal, P.;
Nellen, L.; Nelles, A.; Neuser, J.; Nguyen, P. H.; Niculescu-Oglinzanu,
M.; Niechciol, M.; Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.;
Novotny, V.; Nožka, H.; Núñez, L. A.; Ochilo, L.; Oikonomou, F.;
Olinto, A.; Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Papenbreer,
P.; Parente, G.; Parra, A.; Paul, T.; Pech, M.; Pekala, J.; Pelayo,
R.; Peña-Rodriguez, J.; Pepe, I. M.; Pereira, L. A. S.; Perrone,
L.; Petermann, E.; Peters, C.; Petrera, S.; Phuntsok, J.; Piegaia,
R.; Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello, V.; Platino,
M.; Plum, M.; Porowski, C.; Prado, R. R.; Privitera, P.; Prouza,
M.; Quel, E. J.; Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel,
O.; Ravignani, D.; Reinert, D.; Revenu, B.; Ridky, J.; Risse, M.;
Ristori, P.; Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Rojo,
J.; Rogozin, D.; Rosado, J.; Roth, M.; Roulet, E.; Rovero, A. C.;
Saffi, S. J.; Saftoiu, A.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Sanchez-Lucas, P.;
Santos, E. M.; Santos, E.; Sarazin, F.; Sarkar, B.; Sarmento, R.;
Sarmiento-Cano, C.; Sato, R.; Scarso, C.; Schauer, M.; Scherini, V.;
Schieler, H.; Schmidt, D.; Scholten, O.; Schoorlemmer, H.; Schovánek,
P.; Schröder, F. G.; Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto,
S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sigl,
G.; Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers,
P.; Sonntag, S.; Sorokin, J.; Squartini, R.; Stanca, D.; Stanič,
S.; Stapleton, J.; Stasielak, J.; Strafella, F.; Stutz, A.; Suarez,
F.; Suarez Durán, M.; Sudholz, T.; Suomijärvi, T.; Supanitsky,
A. D.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Taborda, O. A.;
Tapia, A.; Tepe, A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Tomankova, L.; Tomé, B.; Tonachini, A.; Torralba Elipe, G.;
Torres Machado, D.; Travnicek, P.; Trini, M.; Ulrich, R.; Unger,
M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.;
van Aar, G.; van Bodegom, P.; van den Berg, A. M.; van Vliet, A.;
Varela, E.; Vargas Cárdenas, B.; Varner, G.; Vasquez, R.; Vázquez,
J. R.; Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha, J.; Videla,
M.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz,
D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiencke, L.; Wilczyński,
H.; Winchen, T.; Wittkowski, D.; Wundheiler, B.; Wykes, S.; Yang, L.;
Yapici, T.; Yelos, D.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik,
M.; Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello,
F.; Pierre Auger Collaboration
2016PhRvD..93g2006A Altcode: 2016arXiv160400978T
The azimuthal asymmetry in the risetime of signals in Auger
surface detector stations is a source of information on shower
development. The azimuthal asymmetry is due to a combination of the
longitudinal evolution of the shower and geometrical effects related
to the angles of incidence of the particles into the detectors. The
magnitude of the effect depends upon the zenith angle and state
of development of the shower and thus provides a novel observable,
(sec θ )<SUB>max</SUB> , sensitive to the mass composition of cosmic
rays above 3 ×10<SUP>18</SUP> eV . By comparing measurements with
predictions from shower simulations, we find for both of our adopted
models of hadronic physics (QGSJETII-04 and EPOS-LHC) an indication
that the mean cosmic-ray mass increases slowly with energy, as has been
inferred from other studies. However, the mass estimates are dependent
on the shower model and on the range of distance from the shower core
selected. Thus the method has uncovered further deficiencies in our
understanding of shower modeling that must be resolved before the mass
composition can be inferred from (sec θ )ma<SUB>x</SUB>.
---------------------------------------------------------
Title: The Apparent Critical Decay Index at the Onset of Solar
Prominence Eruptions
Authors: Zuccarello, F. P.; Aulanier, G.; Gilchrist, S. A.
2016ApJ...821L..23Z Altcode:
A magnetic flux rope (MFR) embedded in a line-tied external magnetic
field that decreases with height as {z}<SUP>-n</SUP> is unstable
to perturbations if the decay index of the field n is larger
than a critical value. The onset of this instability, called torus
instability, is one of the main mechanisms that can initiate coronal
mass ejections. Since flux ropes often possess magnetic dips that
can support prominence plasma, this is also a valuable mechanism to
trigger prominence eruptions. Magnetohydrodynamic (MHD) simulations of
the formation and/or emergence of MFRs suggest a critical value for
the onset of the instability in the range [1.4-2]. However, detailed
observations of prominences suggest a value in the range [0.9-1.1]. In
this Letter, by using a set of MHD simulations, we show why the large
discrepancy between models and observations is only apparent. Our
simulations indeed show that the critical decay index at the onset of
the eruption is n=1.4+/- 0.1 when computed at the apex of the flux rope
axis, while it is n=1.1+/- 0.1 when it is computed at the altitude of
the topmost part of the distribution of magnetic dips. The discrepancy
only arises because weakly twisted curved flux ropes do not have dips
up to the altitude of their axis.
---------------------------------------------------------
Title: The Pierre Auger Observatory Upgrade - Preliminary Design
Report
Authors: The Pierre Auger Collaboration; Aab, A.; Abreu, P.; Aglietta,
M.; Ahn, E. J.; Samarai, I. Al; Albuquerque, I. F. M.; Allekotte,
I.; Allison, P.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muñiz,
J.; Alves Batista, R.; Ambrosio, M.; Aminaei, A.; Anchordoqui,
L.; Andringa, S.; Aramo, C.; Arqueros, F.; Arsene, N.; Asorey, H.;
Assis, P.; Aublin, J.; Ave, M.; Avenier, M.; Avila, G.; Awal, N.;
Badescu, A. M.; Barber, K. B.; Bäuml, J.; Baus, C.; Beatty, J. J.;
Becker, K. H.; Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou,
X.; Biermann, P. L.; Billoir, P.; Blaess, S. G.; Blanco, A.; Blanco,
M.; Blazek, J.; Bleve, C.; Blümer, H.; Boháčová, M.; Boncioli,
D.; Bonifazi, C.; Borodai, N.; Brack, J.; Brancus, I.; Bridgeman,
A.; Brogueira, P.; Brown, W. C.; Buchholz, P.; Bueno, A.; Buitink,
S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga,
L.; Candusso, M.; Caramete, L.; Caruso, R.; Castellina, A.; Cataldi,
G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.; Chinellato,
J. A.; Chudoba, J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.; Colalillo,
R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição, R.;
Contreras, F.; Cooper, M. J.; Cordier, A.; Coutu, S.; Covault, C. E.;
Cronin, J.; Dallier, R.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson,
B. R.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.; de Mello Neto,
J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza, V.; del Peral, L.;
Deligny, O.; Dembinski, H.; Dhital, N.; Di Giulio, C.; Di Matteo,
A.; Diaz, J. C.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.;
Docters, W.; D'Olivo, J. C.; Dorofeev, A.; Dorosti Hasankiadeh, Q.;
Dova, M. T.; Ebr, J.; Engel, R.; Erdmann, M.; Erfani, M.; Escobar,
C. O.; Espadanal, J.; Etchegoyen, A.; Falcke, H.; Fang, K.; Farrar,
G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Fernandes, M.; Fick,
B.; Figueira, J. M.; Filevich, A.; Filipčič, A.; Fox, B. D.; Fratu,
O.; Freire, M. M.; Fuchs, B.; Fujii, T.; García, B.; Garcia-Pinto,
D.; Gate, F.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari,
U.; Giammarchi, M.; Giller, M.; Głas, D.; Glaser, C.; Glass, H.;
Golup, G.; Gómez Berisso, M.; Gómez Vitale, P. F.; González, N.;
Gookin, B.; Gordon, J.; Gorgi, A.; Gorham, P.; Gouffon, P.; Griffith,
N.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel,
M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Hartmann, S.; Harton,
J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Hemery,
N.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Hollon, N.; Holt, E.;
Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huber, D.;
Huege, T.; Insolia, A.; Isar, P. G.; Jandt, I.; Jansen, S.; Jarne,
C.; Johnsen, J. A.; Josebachuili, M.; Kääpä, A.; Kambeitz, O.;
Kampert, K. H.; Kasper, P.; Katkov, I.; Kégl, B.; Keilhauer, B.;
Keivani, A.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges,
M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Krömer, O.; Kuempel,
D.; Kukec Mezek, G.; Kunka, N.; LaHurd, D.; Latronico, L.; Lauer,
R.; Lauscher, M.; Lautridou, P.; Le Coz, S.; Lebrun, D.; Lebrun,
P.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon,
I.; Link, K.; Lopes, L.; López, R.; López Casado, A.; Louedec,
K.; Lu, L.; Lucero, A.; Malacari, M.; Maldera, S.; Mallamaci, M.;
Maller, J.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, V.;
Mariş, I. C.; Marsella, G.; Martello, D.; Martin, L.; Martinez, H.;
Martínez Bravo, O.; Martraire, D.; Masías Meza, J. J.; Mathes, H. J.;
Mathys, S.; Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Maurizio,
D.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Meissner,
R.; Mello, V. B. B.; Melo, D.; Menshikov, A.; Messina, S.; Meyhandan,
R.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.; Miramonti, L.;
Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Montanet, F.; Morello,
C.; Mostafá, M.; Moura, C. A.; Muller, M. A.; Müller, G.; Müller,
S.; Mussa, R.; Navarra, G.; Navas, S.; Necesal, P.; Nellen, L.; Nelles,
A.; Neuser, J.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol,
M.; Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.;
Nožka, L.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Pacheco, N.; Pakk
Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Papenbreer, P.; Parente,
G.; Parra, A.; Paul, T.; Pech, M.; Pȩkala, J.; Pelayo, R.; Pepe,
I. M.; Perrone, L.; Petermann, E.; Peters, C.; Petrera, S.; Petrov,
Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.;
Pirronello, V.; Platino, M.; Plum, M.; Porcelli, A.; Porowski, C.;
Prado, R. R.; Privitera, P.; Prouza, M.; Purrello, V.; Quel, E. J.;
Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.;
Reinert, D.; Revenu, B.; Ridky, J.; Riggi, S.; Risse, M.; Ristori,
P.; Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Fernandez, G.;
Rodriguez Rojo, J.; Rodríguez-Frías, M. D.; Rogozin, D.; Rosado,
J.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.; Saftoiu, A.;
Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.; Salina, G.;
Sánchez, F.; Sanchez-Lucas, P.; Santos, E.; Santos, E. M.; Sarazin,
F.; Sarkar, B.; Sarmento, R.; Sato, R.; Scarso, C.; Schauer, M.;
Scherini, V.; Schieler, H.; Schmidt, D.; Scholten, O.; Schoorlemmer,
H.; Schovánek, P.; Schröder, F. G.; Schulz, A.; Schulz, J.;
Schumacher, J.; Sciutto, S. J.; Segreto, A.; Settimo, M.; Shadkam,
A.; Shellard, R. C.; Sidelnik, I.; Sigl, G.; Sima, O.; Śmiałkowski,
A.; Šmída, R.; Snow, G. R.; Sommers, P.; Sorokin, J.; Squartini, R.;
Srivastava, Y. N.; Stanca, D.; Stanič, S.; Stapleton, J.; Stasielak,
J.; Stephan, M.; Stutz, A.; Suarez, F.; Suomijärvi, T.; Supanitsky,
A. D.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Taborda, O. A.;
Tapia, A.; Tepe, A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Toma, G.; Tomankova, L.; Tomé, B.; Tonachini, A.; Torralba
Elipe, G.; Torres Machado, D.; Travnicek, P.; Trini, M.; Ulrich, R.;
Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.;
van Aar, G.; van Bodegom, P.; van den Berg, A. M.; van Velzen, S.;
van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.; Vasquez,
R.; Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha,
J.; Videla, M.; Villaseñor, L.; Vlcek, B.; Vorobiov, S.; Wahlberg,
H.; Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weidenhaupt,
K.; Weindl, A.; Werner, F.; Widom, A.; Wiencke, L.; Wilczyński,
H.; Winchen, T.; Wittkowski, D.; Wundheiler, B.; Wykes, S.; Yang, L.;
Yapici, T.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zepeda,
A.; Zhu, Y.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello, F.
2016arXiv160403637T Altcode:
The Pierre Auger Observatory has begun a major Upgrade of its already
impressive capabilities, with an emphasis on improved mass composition
determination using the surface detectors of the Observatory. Known as
AugerPrime, the upgrade will include new 4 m$^2$ plastic scintillator
detectors on top of all 1660 water-Cherenkov detectors, updated and
more flexible surface detector electronics, a large array of buried
muon detectors, and an extended duty cycle for operations of the
fluorescence detectors. This Preliminary Design Report was produced by
the Collaboration in April 2015 as an internal document and information
for funding agencies. It outlines the scientific and technical case for
AugerPrime. We now release it to the public via the arXiv server. We
invite you to review the large number of fundamental results already
achieved by the Observatory and our plans for the future.
---------------------------------------------------------
Title: A Multi-instrument Analysis of a C4.1 Flare Occurring in a
δ Sunspot
Authors: Guglielmino, S. L.; Zuccarello, F.; Romano, P.; Cristaldi,
A.; Ermolli, I.; Criscuoli, S.; Falco, M.; Zuccarello, F. P.
2016ApJ...819..157G Altcode:
We present an analysis of multi-instrument space- and ground-based
observations relevant to a C4.1 solar flare that occurred in the
active region (AR) NOAA 11267 on 2011 August 6. Solar Dynamics
Observatory observations indicate that at the flare’s beginning,
it was localized in the preceding sunspot of the AR, which exhibits
a δ configuration. Along the polarity inversion line between its
opposite polarities we find a large shear angle of about 80°. The
helicity accumulation shows that the AR does not obey the general
hemispheric helicity rule. At the flare peak, unique observations
taken with the X-Ray Telescope aboard Hinode reveal that the bulk
of the X-ray emission takes place in the δ-spot region, where
the plasma heats up to ≈ 1.9\cdot {10}<SUP>7</SUP> K. During the
gradual phase, we observe the development of a Y-shaped structure in
the corona and in the high chromosphere. An extruding structure forms,
being directed from the emitting region above the δ spot toward the
following sunspot. This structure cools down in a few tens of minutes
while moving eastward along a direction opposite to the flare ribbon
expansion. Finally, remote brightenings are found at the easternmost
footpoint of this structure, appearing as a third flare ribbon in the
chromosphere. After some minutes, RHESSI measurements show that the
X-ray emission is localized in the region close to the crossing point
of the coronal Y-shaped structure. Simultaneously, high-resolution
(0.″15) observations performed at the Swedish 1 m Solar Telescope
indicate a decreasing trend of the Ca II H intensity in the flare
ribbons with some transient enhancements. All these findings suggest
that this event is a manifestation of magnetic reconnection, likely
induced by an asymmetric magnetic configuration in a highly sheared
region.
---------------------------------------------------------
Title: Role of "X point” in Flares and Filament Interactions
Authors: Schmieder, B.; Zuccarello, F. P.; Aulanier, G.; Chandra,
R.; Joshi, N. C.; Filippov, B.
2016CEAB...40...35S Altcode:
Explaining the trigger and energy release processes of flares is a
fundamental problem of solar physics. It is commonly held that magnetic
reconnection plays a key role in converting magnetic energy into other
forms of energy. In 2D magnetic field configurations, when oppositely
directed magnetic fields are brought together they may reconnect thereby
releasing stored magnetic energy eventually resulting in a flare. In
3D configurations, the magnetic topology should be considered and the
reconnection is favored at the intersection of magnetic quasi-separatrix
layers, which is an extension of what is called "X point" in 2D. The
evolution of key topological structures, such as null point, spines
and fans may determine the eruptive behavior of a flare. The presence
of a null point can be very important. We present a few examples, i.e.,
a flare with a circular flare ribbon and the interaction of two parallel
filaments. <P />In the case of flux rope destabilization and triggering
eruption due to the torus instability, the important parameter is
the decay index and not the topology itself. However the complexity
of active regions leads to interpretations where different mechanisms
may be intermixed. The breakout mechanism, which requires a quadrupolar
configuration with QSLs and separator where the reconnection can occur,
is present in many models. That is not always a sufficient condition
to explain the eruptive flares. For one case study, the different
behaviour of a series of eruptive flares followed by confined flares,
all originating in the same site has been attributed to the change of
orientation of the magnetic field below the fan with respect to the
orientation of the spine. Flares tend to be more confined when the
two fields become less antiparallel.
---------------------------------------------------------
Title: Critical Decay Index at the Onset of Solar Eruptions
Authors: Zuccarello, F. P.; Aulanier, G.; Gilchrist, S. A.
2015ApJ...814..126Z Altcode: 2015arXiv151003713Z
Magnetic flux ropes are topological structures consisting of twisted
magnetic field lines that globally wrap around an axis. The torus
instability model predicts that a magnetic flux rope of major radius R
undergoes an eruption when its axis reaches a location where the decay
index -d({ln}{B}<SUB>{ex</SUB>})/d({ln}R) of the ambient magnetic field
B<SUB>ex</SUB> is larger than a critical value. In the current-wire
model, the critical value depends on the thickness and time evolution
of the current channel. We use magnetohydrodynamic simulations to
investigate whether the critical value of the decay index at the onset
of the eruption is affected by the magnetic flux rope’s internal
current profile and/or by the particular pre-eruptive photospheric
dynamics. The evolution of an asymmetric, bipolar active region is
driven by applying different classes of photospheric motions. We find
that the critical value of the decay index at the onset of the eruption
is not significantly affected by either the pre-erupitve photospheric
evolution of the active region or the resulting different magnetic
flux ropes. As in the case of the current-wire model, we find that
there is a “critical range” [1.3-1.5], rather than a “critical
value” for the onset of the torus instability. This range is in good
agreement with the predictions of the current-wire model, despite the
inclusion of line-tying effects and the occurrence of tether-cutting
magnetic reconnection.
---------------------------------------------------------
Title: Pierre Auger Observatory and Telescope Array: Joint
Contributions to the 34th International Cosmic Ray Conference
(ICRC 2015)
Authors: Telescope Array Collaboration; Abbasi, R. U.; Abe, M.;
Abu-Zayyad, T.; Allen, M.; Azuma, R.; Barcikowski, E.; Belz, J. W.;
Bergman, D. R.; Blake, S. A.; Cady, R.; Chae, M. J.; Cheon, B. G.;
Chiba, J.; Chikawa, M.; Cho, W. R.; Fujii, T.; Fukushima, M.; Goto,
T.; Hanlon, W.; Hayashi, Y.; Hayashida, N.; Hibino, K.; Honda, K.;
Ikeda, D.; Inoue, N.; Ishii, T.; Ishimori, R.; Ito, H.; Ivanov, D.;
Jui, C. C. H.; Kadota, K.; Kakimoto, F.; Kalashev, O.; Kasahara,
K.; Kawai, H.; Kawakami, S.; Kawana, S.; Kawata, K.; Kido, E.; Kim,
H. B.; Kim, J. H.; Kim, J. H.; Kitamura, S.; Kitamura, Y.; Kuzmin,
V.; Kwon, Y. J.; Lan, J.; Lim, S. I.; Lundquist, J. P.; Machida, K.;
Martens, K.; Matsuda, T.; Matsuyama, T.; Matthews, J. N.; Minamino,
M.; Mukai, Y.; Myers, I.; Nagasawa, K.; Nagataki, S.; Nakamura, T.;
Nonaka, T.; Nozato, A.; Ogio, S.; Ogura, J.; Ohnishi, M.; Ohoka,
H.; Oki, K.; Okuda, T.; Ono, M.; Oshima, A.; Ozawa, S.; Park, I. H.;
Pshirkov, M. S.; Rodriguez, D. C.; Rubtsov, G.; Ryu, D.; Sagawa, H.;
Sakurai, N.; Scott, L. M.; Shah, P. D.; Shibata, F.; Shibata, T.;
Shimodaira, H.; Shin, B. K.; Shin, H. S.; Smith, J. D.; Sokolsky,
P.; Springer, R. W.; Stokes, B. T.; Stratton, S. R.; Stroman, T. A.;
Suzawa, T.; Takamura, M.; Takeda, M.; Takeishi, R.; Taketa, A.;
Takita, M.; Tameda, Y.; Tanaka, H.; Tanaka, K.; Tanaka, M.; Thomas,
S. B.; Thomson, G. B.; Tinyakov, P.; Tkachev, I.; Tokuno, H.; Tomida,
T.; Troitsky, S.; Tsunesada, Y.; Tsutsumi, K.; Uchihori, Y.; Udo, S.;
Urban, F.; Vasiloff, G.; Wong, T.; Yamane, R.; Yamaoka, H.; Yamazaki,
K.; Yang, J.; Yashiro, K.; Yoneda, Y.; Yoshida, S.; Yoshii, H.;
Zollinger, R.; Zundel, Z.; Pierre Auger Collaboration; :; Aab, A.;
Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai, I. Al; Albuquerque,
I. F. M.; Allekotte, I.; Allison, P.; Almela, A.; Alvarez Castillo,
J.; Alvarez-Muñiz, J.; Alves Batista, R.; Ambrosio, M.; Aminaei, A.;
Anastasi, G. A.; Anchordoqui, L.; Andringa, S.; Aramo, C.; Arqueros,
F.; Arsene, N.; Asorey, H.; Assis, P.; Aublin, J.; Avila, G.; Awal,
N.; Badescu, A. M.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido,
J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.;
Billoir, P.; Blaess, S. G.; Blanco, A.; Blanco, M.; Blazek, J.;
Bleve, C.; Blümer, H.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Brack, J.; Brancus, I.; Bretz, T.; Bridgeman, A.;
Brogueira, P.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.;
Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga, L.; Candusso, M.;
Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.; Cazon, L.;
Cester, R.; Chavez, A. G.; Chiavassa, A.; Chinellato, J. A.; Chudoba,
J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.; Colalillo, R.; Coleman, A.;
Collica, L.; Coluccia, M. R.; Conceição, R.; Contreras, F.; Cooper,
M. J.; Cordier, A.; Coutu, S.; Covault, C. E.; Dallier, R.; Daniel,
B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; de
Jong, S. J.; De Mauro, G.; de Mello Neto, J. R. T.; De Mitri, I.;
de Oliveira, J.; de Souza, V.; del Peral, L.; Deligny, O.; Dhital,
N.; Di Giulio, C.; Di Matteo, A.; Diaz, J. C.; Díaz Castro, M. L.;
Diogo, F.; Dobrigkeit, C.; Docters, W.; D'Olivo, J. C.; Dorofeev,
A.; Dorosti Hasankiadeh, Q.; dos Anjos, R. C.; Dova, M. T.; Ebr,
J.; Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal,
J.; Etchegoyen, A.; Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.;
Fazzini, N.; Ferguson, A. P.; Fick, B.; Figueira, J. M.; Filevich,
A.; Filipčič, A.; Fratu, O.; Freire, M. M.; Fujii, T.; García,
B.; García-Gámez, D.; Garcia-Pinto, D.; Gate, F.; Gemmeke, H.;
Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller,
M.; Głas, D.; Glaser, C.; Glass, H.; Golup, G.; Gómez Berisso, M.;
Gómez Vitale, P. F.; González, N.; Gookin, B.; Gordon, J.; Gorgi, A.;
Gorham, P.; Gouffon, P.; Griffith, N.; Grillo, A. F.; Grubb, T. D.;
Guarino, F.; Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.;
Harrison, T. A.; Hartmann, S.; Harton, J. L.; Haungs, A.; Hebbeker,
T.; Heck, D.; Heimann, P.; Hervé, A. E.; Hill, G. C.; Hojvat, C.;
Hollon, N.; Holt, E.; Homola, P.; Hörandel, J. R.; Horvath, P.;
Hrabovský, M.; Huber, D.; Huege, T.; Insolia, A.; Isar, P. G.;
Jandt, I.; Jansen, S.; Jarne, C.; Johnsen, J. A.; Josebachuili, M.;
Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.;
Keilhauer, B.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges,
M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Kuempel, D.; Kukec Mezek,
G.; Kunka, N.; Kuotb Awad, A. W.; LaHurd, D.; Latronico, L.; Lauer,
R.; Lauscher, M.; Lautridou, P.; Le Coz, S.; Lebrun, D.; Lebrun, P.;
Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link,
K.; Lopes, L.; López, R.; López Casado, A.; Louedec, K.; Lucero,
A.; Malacari, M.; Mallamaci, M.; Maller, J.; Mandat, D.; Mantsch, P.;
Mariazzi, A. G.; Marin, V.; Mariş, I. C.; Marsella, G.; Martello,
D.; Martinez, H.; Martínez Bravo, O.; Martraire, D.; Masías Meza,
J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.;
Matthiae, G.; Maurizio, D.; Mayotte, E.; Mazur, P. O.; Medina, C.;
Medina-Tanco, G.; Meissner, R.; Mello, V. B. B.; Melo, D.; Menshikov,
A.; Messina, S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.;
Miramonti, L.; Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Montanet,
F.; Morello, C.; Mostafá, M.; Moura, C. A.; Müller, G.; Muller,
M. A.; Müller, S.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.;
Neuser, J.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.;
Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka,
L.; Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Pacheco,
N.; Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Papenbreer, P.;
Parente, G.; Parra, A.; Paul, T.; Pech, M.; Pȩkala, J.; Pelayo,
R.; Pepe, I. M.; Perrone, L.; Petermann, E.; Peters, C.; Petrera,
S.; Petrov, Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.;
Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.; Porcelli, A.;
Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Quel, E. J.;
Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.;
Reinert, D.; Revenu, B.; Ridky, J.; Risse, M.; Ristori, P.; Rizi,
V.; Rodrigues de Carvalho, W.; Rodriguez Rojo, J.; Rodríguez-Frías,
M. D.; Rogozin, D.; Rosado, J.; Roth, M.; Roulet, E.; Rovero, A. C.;
Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.;
Salesa Greus, F.; Salina, G.; Sanabria Gomez, J. D.; Sánchez,
F.; Sanchez-Lucas, P.; Santos, E. M.; Santos, E.; Sarazin, F.;
Sarkar, B.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.; Scarso,
C.; Schauer, M.; Scherini, V.; Schieler, H.; Schmidt, D.; Scholten,
O.; Schoorlemmer, H.; Schovánek, P.; Schröder, F. G.; Schulz, A.;
Schulz, J.; Schumacher, J.; Sciutto, S. J.; Segreto, A.; Settimo,
M.; Shadkam, A.; Shellard, R. C.; Sigl, G.; Sima, O.; Śmiałkowski,
A.; Šmída, R.; Snow, G. R.; Sommers, P.; Sonntag, S.; Sorokin, J.;
Squartini, R.; Srivastava, Y. N.; Stanca, D.; Stanič, S.; Stapleton,
J.; Stasielak, J.; Stephan, M.; Stutz, A.; Suarez, F.; Suarez Durán,
M.; Suomijärvi, T.; Supanitsky, A. D.; Sutherland, M. S.; Swain,
J.; Szadkowski, Z.; Taborda, O. A.; Tapia, A.; Tepe, A.; Theodoro,
V. M.; Tibolla, O.; Timmermans, C.; Todero Peixoto, C. J.; Toma, G.;
Tomankova, L.; Tomé, B.; Tonachini, A.; Torralba Elipe, G.; Torres
Machado, D.; Travnicek, P.; Trini, M.; Ulrich, R.; Unger, M.; Urban,
M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.; van Aar, G.;
van Bodegom, P.; van den Berg, A. M.; van Velzen, S.; van Vliet, A.;
Varela, E.; Vargas Cárdenas, B.; Varner, G.; Vasquez, R.; Vázquez,
J. R.; Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha, J.; Videla,
M.; Villaseñor, L.; Vlcek, B.; Vorobiov, S.; Wahlberg, H.; Wainberg,
O.; Walz, D.; Watson, A. A.; Weber, M.; Weidenhaupt, K.; Weindl,
A.; Welling, C.; Werner, F.; Widom, A.; Wiencke, L.; Wilczyński,
H.; Winchen, T.; Wittkowski, D.; Wundheiler, B.; Wykes, S.; Yang,
L.; Yapici, T.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zuccarello, F.
2015arXiv151102103T Altcode:
Joint contributions of the Pierre Auger Collaboration and the Telescope
Array Collaboration to the 34th International Cosmic Ray Conference,
30 July - 6 August 2015, The Hague, The Netherlands.
---------------------------------------------------------
Title: The IceCube Neutrino Observatory, the Pierre Auger Observatory
and the Telescope Array: Joint Contribution to the 34th International
Cosmic Ray Conference (ICRC 2015)
Authors: IceCube Collaboration; Aartsen, M. G.; Abraham, K.;
Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.;
Altmann, D.; Anderson, T.; Ansseau, I.; Archinger, M.; Arguelles,
C.; Arlen, T. C.; Auffenberg, J.; Bai, X.; Barwick, S. W.; Baum, V.;
Bay, R.; Beatty, J. J.; Becker Tjus, J.; Becker, K. -H.; Beiser, E.;
BenZvi, S.; Berghaus, P.; Berley, D.; Bernardini, E.; Bernhard, A.;
Besson, D. Z.; Binder, G.; Bindig, D.; Bissok, M.; Blaufuss, E.;
Blumenthal, J.; Boersma, D. J.; Bohm, C.; Börner, M.; Bos, F.;
Bose, D.; Böser, S.; Botner, O.; Braun, J.; Brayeur, L.; Bretz,
H. -P.; Buzinsky, N.; Casey, J.; Casier, M.; Cheung, E.; Chirkin,
D.; Christov, A.; Clark, K.; Classen, L.; Coenders, S.; Cowen, D. F.;
Cruz Silva, A. H.; Daughhetee, J.; Davis, J. C.; Day, M.; de André,
J. P. A. M.; De Clercq, C.; del Pino Rosendo, E.; Dembinski, H.; De
Ridder, S.; Desiati, P.; de Vries, K. D.; de Wasseige, G.; de With,
M.; DeYoung, T.; Díaz-Vélez, J. C.; di Lorenzo, V.; Dumm, J. P.;
Dunkman, M.; Eagan, R.; Eberhardt, B.; Ehrhardt, T.; Eichmann, B.;
Euler, S.; Evenson, P. A.; Fadiran, O.; Fahey, S.; Fazely, A. R.;
Fedynitch, A.; Feintzeig, J.; Felde, J.; Filimonov, K.; Finley, C.;
Fischer-Wasels, T.; Flis, S.; Fösig, C. -C.; Fuchs, T.; Gaisser,
T. K.; Gaior, R.; Gallagher, J.; Gerhardt, L.; Ghorbani, K.; Gier,
D.; Gladstone, L.; Glagla, M.; Glüsenkamp, T.; Goldschmidt, A.;
Golup, G.; Gonzalez, J. G.; Góra, D.; Grant, D.; Groh, J. C.; Groß,
A.; Ha, C.; Haack, C.; Haj Ismail, A.; Hallgren, A.; Halzen, F.;
Hansmann, B.; Hanson, K.; Hebecker, D.; Heereman, D.; Helbing, K.;
Hellauer, R.; Hellwig, D.; Hickford, S.; Hignight, J.; Hill, G. C.;
Hoffman, K. D.; Hoffmann, R.; Holzapfel, K.; Homeier, A.; Hoshina,
K.; Huang, F.; Huber, M.; Huelsnitz, W.; Hulth, P. O.; Hultqvist,
K.; In, S.; Ishihara, A.; Jacobi, E.; Japaridze, G. S.; Jero, K.;
Jurkovic, M.; Kaminsky, B.; Kappes, A.; Karg, T.; Karle, A.; Kauer,
M.; Keivani, A.; Kelley, J. L.; Kemp, J.; Kheirandish, A.; Kiryluk,
J.; Kläs, J.; Klein, S. R.; Kohnen, G.; Koirala, R.; Kolanoski, H.;
Konietz, R.; Koob, A.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen,
D. J.; Kowalski, M.; Krings, K.; Kroll, G.; Kroll, M.; Kunnen, J.;
Kurahashi, N.; Kuwabara, T.; Labare, M.; Lanfranchi, J. L.; Larson,
M. J.; Lesiak-Bzdak, M.; Leuermann, M.; Leuner, J.; Lu, L.; Lünemann,
J.; Madsen, J.; Maggi, G.; Mahn, K. B. M.; Maruyama, R.; Mase, K.;
Matis, H. S.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Meli,
A.; Menne, T.; Merino, G.; Meures, T.; Miarecki, S.; Middell, E.;
Middlemas, E.; Mohrmann, L.; Montaruli, T.; Morse, R.; Nahnhauer, R.;
Naumann, U.; Neer, G.; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.;
Obertacke, A.; Olivas, A.; Omairat, A.; O'Murchadha, A.; Palczewski,
T.; Pandya, H.; Paul, L.; Pepper, J. A.; Pérez de los Heros, C.;
Pfendner, C.; Pieloth, D.; Pinat, E.; Posselt, J.; Price, P. B.;
Przybylski, G. T.; Pütz, J.; Quinnan, M.; Raab, C.; Rädel, L.;
Rameez, M.; Rawlins, K.; Reimann, R.; Relich, M.; Resconi, E.; Rhode,
W.; Richman, M.; Richter, S.; Riedel, B.; Robertson, S.; Rongen, M.;
Rott, C.; Ruhe, T.; Ryckbosch, D.; Saba, S. M.; Sabbatini, L.; Sander,
H. -G.; Sandrock, A.; Sandroos, J.; Sarkar, S.; Schatto, K.; Scheriau,
F.; Schimp, M.; Schmidt, T.; Schmitz, M.; Schoenen, S.; Schöneberg,
S.; Schönwald, A.; Schulte, L.; Seckel, D.; Seunarine, S.; Shanidze,
R.; Smith, M. W. E.; Soldin, D.; Song, M.; Spiczak, G. M.; Spiering,
C.; Stahlberg, M.; Stamatikos, M.; Stanev, T.; Stanisha, N. A.;
Stasik, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Ström,
R.; Strotjohann, N. L.; Sullivan, G. W.; Sutherland, M.; Taavola,
H.; Taboada, I.; Ter-Antonyan, S.; Terliuk, A.; Tešić, G.; Tilav,
S.; Toale, P. A.; Tobin, M. N.; Toscano, S.; Tosi, D.; Tselengidou,
M.; Turcati, A.; Unger, E.; Usner, M.; Vallecorsa, S.; Vandenbroucke,
J.; van Eijndhoven, N.; Vanheule, S.; van Santen, J.; Veenkamp, J.;
Vehring, M.; Voge, M.; Vraeghe, M.; Walck, C.; Wallace, A.; Wallraff,
M.; Wandkowsky, N.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whelan,
B. J.; Whitehorn, N.; Wichary, C.; Wiebe, K.; Wiebusch, C. H.;
Wille, L.; Williams, D. R.; Wissing, H.; Wolf, M.; Wood, T. R.;
Woschnagg, K.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yanez, J. P.; Yodh,
G.; Yoshida, S.; Zoll, M.; Pierre Auger Collaboration; :; Aab, A.;
Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai, I. Al; Albuquerque,
I. F. M.; Allekotte, I.; Allison, P.; Almela, A.; Alvarez Castillo,
J.; Alvarez-Muñiz, J.; Alves Batista, R.; Ambrosio, M.; Aminaei, A.;
Anastasi, G. A.; Anchordoqui, L.; Andringa, S.; Aramo, C.; Arqueros,
F.; Arsene, N.; Asorey, H.; Assis, P.; Aublin, J.; Avila, G.; Awal,
N.; Badescu, A. M.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido,
J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.;
Billoir, P.; Blaess, S. G.; Blanco, A.; Blanco, M.; Blazek, J.;
Bleve, C.; Blümer, H.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Borodai, N.; Brack, J.; Brancus, I.; Bretz, T.; Bridgeman, A.;
Brogueira, P.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.;
Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga, L.; Candusso, M.;
Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.; Cazon, L.;
Cester, R.; Chavez, A. G.; Chiavassa, A.; Chinellato, J. A.; Chudoba,
J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.; Colalillo, R.; Coleman, A.;
Collica, L.; Coluccia, M. R.; Conceição, R.; Contreras, F.; Cooper,
M. J.; Cordier, A.; Coutu, S.; Covault, C. E.; Dallier, R.; Daniel,
B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; de
Jong, S. J.; De Mauro, G.; de Mello Neto, J. R. T.; De Mitri, I.;
de Oliveira, J.; de Souza, V.; del Peral, L.; Deligny, O.; Dhital,
N.; Di Giulio, C.; Di Matteo, A.; Diaz, J. C.; Díaz Castro, M. L.;
Diogo, F.; Dobrigkeit, C.; Docters, W.; D'Olivo, J. C.; Dorofeev,
A.; Dorosti Hasankiadeh, Q.; dos Anjos, R. C.; Dova, M. T.; Ebr, J.;
Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.;
Etchegoyen, A.; Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.;
Fazzini, N.; Ferguson, A. P.; Fick, B.; Figueira, J. M.; Filevich,
A.; Filipčič, A.; Fratu, O.; Freire, M. M.; Fujii, T.; García,
B.; García-Gámez, D.; Garcia-Pinto, D.; Gate, F.; Gemmeke, H.;
Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller,
M.; Głas, D.; Glaser, C.; Glass, H.; Golup, G.; Gómez Berisso, M.;
Gómez Vitale, P. F.; González, N.; Gookin, B.; Gordon, J.; Gorgi, A.;
Gorham, P.; Gouffon, P.; Griffith, N.; Grillo, A. F.; Grubb, T. D.;
Guarino, F.; Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.;
Harrison, T. A.; Hartmann, S.; Harton, J. L.; Haungs, A.; Hebbeker,
T.; Heck, D.; Heimann, P.; Hervé, A. E.; Hill, G. C.; Hojvat, C.;
Hollon, N.; Holt, E.; Homola, P.; Hörandel, J. R.; Horvath, P.;
Hrabovský, M.; Huber, D.; Huege, T.; Insolia, A.; Isar, P. G.;
Jandt, I.; Jansen, S.; Jarne, C.; Johnsen, J. A.; Josebachuili, M.;
Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.;
Keilhauer, B.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges,
M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Kuempel, D.; Kukec Mezek,
G.; Kunka, N.; Kuotb Awad, A. W.; LaHurd, D.; Latronico, L.; Lauer,
R.; Lauscher, M.; Lautridou, P.; Le Coz, S.; Lebrun, D.; Lebrun, P.;
Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link,
K.; Lopes, L.; López, R.; López Casado, A.; Louedec, K.; Lucero,
A.; Malacari, M.; Mallamaci, M.; Maller, J.; Mandat, D.; Mantsch, P.;
Mariazzi, A. G.; Marin, V.; Mariş, I. C.; Marsella, G.; Martello,
D.; Martinez, H.; Martínez Bravo, O.; Martraire, D.; Masías Meza,
J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.;
Matthiae, G.; Maurizio, D.; Mayotte, E.; Mazur, P. O.; Medina, C.;
Medina-Tanco, G.; Meissner, R.; Mello, V. B. B.; Melo, D.; Menshikov,
A.; Messina, S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.;
Miramonti, L.; Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Montanet,
F.; Morello, C.; Mostafá, M.; Moura, C. A.; Müller, G.; Muller,
M. A.; Müller, S.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.;
Neuser, J.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.;
Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka,
L.; Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Pacheco, N.;
Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Papenbreer, P.; Parente,
G.; Parra, A.; Paul, T.; Pech, M.; Pȩkala, J.; Pelayo, R.; Pepe,
I. M.; Perrone, L.; Petermann, E.; Peters, C.; Petrera, S.; Petrov,
Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.;
Pirronello, V.; Platino, M.; Plum, M.; Porcelli, A.; Porowski, C.;
Prado, R. R.; Privitera, P.; Prouza, M.; Quel, E. J.; Querchfeld,
S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.; Reinert, D.;
Revenu, B.; Ridky, J.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de
Carvalho, W.; Rodriguez Rojo, J.; Rodríguez-Frías, M. D.; Rogozin,
D.; Rosado, J.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Sanchez-Lucas, P.;
Santos, E. M.; Santos, E.; Sarazin, F.; Sarkar, B.; Sarmento, R.;
Sarmiento-Cano, C.; Sato, R.; Scarso, C.; Schauer, M.; Scherini, V.;
Schieler, H.; Schmidt, D.; Scholten, O.; Schoorlemmer, H.; Schovánek,
P.; Schröder, F. G.; Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto,
S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sigl,
G.; Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers,
P.; Sonntag, S.; Sorokin, J.; Squartini, R.; Srivastava, Y. N.;
Stanca, D.; Stanič, S.; Stapleton, J.; Stasielak, J.; Stephan, M.;
Stutz, A.; Suarez, F.; Suarez Durán, M.; Suomijärvi, T.; Supanitsky,
A. D.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Taborda, O. A.;
Tapia, A.; Tepe, A.; Theodoro, V. M.; Tibolla, O.; Timmermans, C.;
Todero Peixoto, C. J.; Toma, G.; Tomankova, L.; Tomé, B.; Tonachini,
A.; Torralba Elipe, G.; Torres Machado, D.; Travnicek, P.; Trini, M.;
Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño,
I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.;
van Velzen, S.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.;
Varner, G.; Vasquez, R.; Vázquez, J. R.; Vázquez, R. A.; Veberič,
D.; Verzi, V.; Vicha, J.; Videla, M.; Villaseñor, L.; Vlcek, B.;
Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz, D.; Watson, A. A.;
Weber, M.; Weidenhaupt, K.; Weindl, A.; Welling, C.; Werner, F.;
Widom, A.; Wiencke, L.; Wilczyński, H.; Winchen, T.; Wittkowski, D.;
Wundheiler, B.; Wykes, S.; Yang, L.; Yapici, T.; Yushkov, A.; Zas, E.;
Zavrtanik, D.; Zavrtanik, M.; Zepeda, A.; Zimmermann, B.; Ziolkowski,
M.; Zuccarello, F.; Telescope Array Collaboration; :; Abbasi, R. U.;
Abe, M.; Abu-Zayyad, T.; Allen, M.; Azuma, R.; Barcikowski, E.; Belz,
J. W.; Bergman, D. R.; Blake, S. A.; Cady, R.; Chae, M. J.; Cheon,
B. G.; Chiba, J.; Chikawa, M.; Cho, W. R.; Fujii, T.; Fukushima, M.;
Goto, T.; Hanlon, W.; Hayashi, Y.; Hayashida, N.; Hibino, K.; Honda,
K.; Ikeda, D.; Inoue, N.; Ishii, T.; Ishimori, R.; Ito, H.; Ivanov,
D.; Jui, C. C. H.; Kadota, K.; Kakimoto, F.; Kalashev, O.; Kasahara,
K.; Kawai, H.; Kawakami, S.; Kawana, S.; Kawata, K.; Kido, E.; Kim,
H. B.; Kim, J. H.; Kim, J. H.; Kitamura, S.; Kitamura, Y.; Kuzmin,
V.; Kwon, Y. J.; Lan, J.; Lim, S. I.; Lundquist, J. P.; Machida, K.;
Martens, K.; Matsuda, T.; Matsuyama, T.; Matthews, J. N.; Minamino,
M.; Mukai, Y.; Myers, I.; Nagasawa, K.; Nagataki, S.; Nakamura, T.;
Nonaka, T.; Nozato, A.; Ogio, S.; Ogura, J.; Ohnishi, M.; Ohoka,
H.; Oki, K.; Okuda, T.; Ono, M.; Oshima, A.; Ozawa, S.; Park, I. H.;
Pshirkov, M. S.; Rodriguez, D. C.; Rubtsov, G.; Ryu, D.; Sagawa, H.;
Sakurai, N.; Scott, L. M.; Shah, P. D.; Shibata, F.; Shibata, T.;
Shimodaira, H.; Shin, B. K.; Shin, H. S.; Smith, J. D.; Sokolsky,
P.; Springer, R. W.; Stokes, B. T.; Stratton, S. R.; Stroman, T. A.;
Suzawa, T.; Takamura, M.; Takeda, M.; Takeishi, R.; Taketa, A.;
Takita, M.; Tameda, Y.; Tanaka, H.; Tanaka, K.; Tanaka, M.; Thomas,
S. B.; Thomson, G. B.; Tinyakov, P.; Tkachev, I.; Tokuno, H.; Tomida,
T.; Troitsky, S.; Tsunesada, Y.; Tsutsumi, K.; Uchihori, Y.; Udo, S.;
Urban, F.; Vasiloff, G.; Wong, T.; Yamane, R.; Yamaoka, H.; Yamazaki,
K.; Yang, J.; Yashiro, K.; Yoneda, Y.; Yoshida, S.; Yoshii, H.;
Zollinger, R.; Zundel, Z.
2015arXiv151102109I Altcode:
We have conducted three searches for correlations between ultra-high
energy cosmic rays detected by the Telescope Array and the Pierre Auger
Observatory, and high-energy neutrino candidate events from IceCube. Two
cross-correlation analyses with UHECRs are done: one with 39 cascades
from the IceCube `high-energy starting events' sample and the other
with 16 high-energy `track events'. The angular separation between the
arrival directions of neutrinos and UHECRs is scanned over. The same
events are also used in a separate search using a maximum likelihood
approach, after the neutrino arrival directions are stacked. To
estimate the significance we assume UHECR magnetic deflections to
be inversely proportional to their energy, with values $3^\circ$,
$6^\circ$ and $9^\circ$ at 100 EeV to allow for the uncertainties on
the magnetic field strength and UHECR charge. A similar analysis is
performed on stacked UHECR arrival directions and the IceCube sample
of through-going muon track events which were optimized for neutrino
point-source searches.
---------------------------------------------------------
Title: ADAHELI: exploring the fast, dynamic Sun in the x-ray, optical,
and near-infrared
Authors: Berrilli, Francesco; Soffitta, Paolo; Velli, Marco; Sabatini,
Paolo; Bigazzi, Alberto; Bellazzini, Ronaldo; Bellot Rubio, Luis
Ramon; Brez, Alessandro; Carbone, Vincenzo; Cauzzi, Gianna; Cavallini,
Fabio; Consolini, Giuseppe; Curti, Fabio; Del Moro, Dario; Di Giorgio,
Anna Maria; Ermolli, Ilaria; Fabiani, Sergio; Faurobert, Marianne;
Feller, Alex; Galsgaard, Klaus; Gburek, Szymon; Giannattasio, Fabio;
Giovannelli, Luca; Hirzberger, Johann; Jefferies, Stuart M.; Madjarska,
Maria S.; Manni, Fabio; Mazzoni, Alessandro; Muleri, Fabio; Penza,
Valentina; Peres, Giovanni; Piazzesi, Roberto; Pieralli, Francesca;
Pietropaolo, Ermanno; Martinez Pillet, Valentin; Pinchera, Michele;
Reale, Fabio; Romano, Paolo; Romoli, Andrea; Romoli, Marco; Rubini,
Alda; Rudawy, Pawel; Sandri, Paolo; Scardigli, Stefano; Spandre,
Gloria; Solanki, Sami K.; Stangalini, Marco; Vecchio, Antonio;
Zuccarello, Francesca
2015JATIS...1d4006B Altcode:
Advanced Astronomy for Heliophysics Plus (ADAHELI) is a project concept
for a small solar and space weather mission with a budget compatible
with an European Space Agency (ESA) S-class mission, including launch,
and a fast development cycle. ADAHELI was submitted to the European
Space Agency by a European-wide consortium of solar physics research
institutes in response to the "Call for a small mission opportunity
for a launch in 2017," of March 9, 2012. The ADAHELI project builds
on the heritage of the former ADAHELI mission, which had successfully
completed its phase-A study under the Italian Space Agency 2007 Small
Mission Programme, thus proving the soundness and feasibility of
its innovative low-budget design. ADAHELI is a solar space mission
with two main instruments: ISODY: an imager, based on Fabry-Pérot
interferometers, whose design is optimized to the acquisition of
highest cadence, long-duration, multiline spectropolarimetric images
in the visible/near-infrared region of the solar spectrum. XSPO: an
x-ray polarimeter for solar flares in x-rays with energies in the 15
to 35 keV range. ADAHELI is capable of performing observations that
cannot be addressed by other currently planned solar space missions,
due to their limited telemetry, or by ground-based facilities, due to
the problematic effect of the terrestrial atmosphere.
---------------------------------------------------------
Title: Recurrent flares in active region NOAA 11283
Authors: Romano, P.; Zuccarello, F.; Guglielmino, S. L.; Berrilli, F.;
Bruno, R.; Carbone, V.; Consolini, G.; de Lauretis, M.; Del Moro, D.;
Elmhamdi, A.; Ermolli, I.; Fineschi, S.; Francia, P.; Kordi, A. S.;
Landi Degl'Innocenti, E.; Laurenza, M.; Lepreti, F.; Marcucci, M. F.;
Pallocchia, G.; Pietropaolo, E.; Romoli, M.; Vecchio, A.; Vellante,
M.; Villante, U.
2015A&A...582A..55R Altcode:
Context. Flares and coronal mass ejections (CMEs) are solar phenomena
that are not yet fully understood. Several investigations have
been performed to single out their related physical parameters that
can be used as indices of the magnetic complexity leading to their
occurrence. <BR /> Aims: In order to shed light on the occurrence of
recurrent flares and subsequent associated CMEs, we studied the active
region NOAA 11283 where recurrent M and X GOES-class flares and CMEs
occurred. <BR /> Methods: We use vector magnetograms taken by HMI/SDO
to calculate the horizontal velocity fields of the photospheric
magnetic structures, the shear and the dip angles of the magnetic
field, the magnetic helicity flux distribution, and the Poynting
fluxes across the photosphere due to the emergence and the shearing
of the magnetic field. <BR /> Results: Although we do not observe
consistent emerging magnetic flux through the photosphere during the
observation time interval, we detected a monotonic increase of the
magnetic helicity accumulated in the corona. We found that both the
shear and the dip angles have high values along the main polarity
inversion line (PIL) before and after all the events. We also note
that before the main flare of X2.1 GOES class, the shearing motions
seem to inject a more significant energy than the energy injected
by the emergence of the magnetic field. <BR /> Conclusions: We
conclude that the very long duration (about 4 days) of the horizontal
displacement of the main photospheric magnetic structures along the
PIL has a primary role in the energy release during the recurrent
flares. This peculiar horizontal velocity field also contributes to
the monotonic injection of magnetic helicity into the corona. This
process, coupled with the high shear and dip angles along the main
PIL, appears to be responsible for the consecutive events of loss
of equilibrium leading to the recurrent flares and CMEs. <P />A
movie associated to Fig. 4 is available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201525887/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: The Pierre Auger Observatory: Contributions to the 34th
International Cosmic Ray Conference (ICRC 2015)
Authors: The Pierre Auger Collaboration; Aab, A.; Abreu, P.; Aglietta,
M.; Ahn, E. J.; Samarai, I. Al; Albuquerque, I. F. M.; Allekotte,
I.; Allison, P.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muñiz,
J.; Alves Batista, R.; Ambrosio, M.; Aminaei, A.; Anastasi, G. A.;
Anchordoqui, L.; Andringa, S.; Aramo, C.; Arqueros, F.; Arsene, N.;
Asorey, H.; Assis, P.; Aublin, J.; Avila, G.; Awal, N.; Badescu, A. M.;
Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.; Berat, C.;
Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Billoir, P.; Blaess,
S. G.; Blanco, A.; Blanco, M.; Blazek, J.; Bleve, C.; Blümer, H.;
Boháčová, M.; Boncioli, D.; Bonifazi, C.; Borodai, N.; Brack, J.;
Brancus, I.; Bretz, T.; Bridgeman, A.; Brogueira, P.; Buchholz, P.;
Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga,
B.; Caccianiga, L.; Candusso, M.; Caramete, L.; Caruso, R.; Castellina,
A.; Cataldi, G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.;
Chinellato, J. A.; Chudoba, J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.;
Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição,
R.; Contreras, F.; Cooper, M. J.; Cordier, A.; Coutu, S.; Covault,
C. E.; Cronin, J.; Dallier, R.; Daniel, B.; Dasso, S.; Daumiller,
K.; Dawson, B. R.; de Almeida, R. M.; de Jong, S. J.; De Mauro, G.;
de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza, V.;
del Peral, L.; Deligny, O.; Dhital, N.; Di Giulio, C.; Di Matteo, A.;
Diaz, J. C.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; Docters,
W.; D'Olivo, J. C.; Dorofeev, A.; Dorosti Hasankiadeh, Q.; dos Anjos,
R. C.; Dova, M. T.; Ebr, J.; Engel, R.; Erdmann, M.; Erfani, M.;
Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Falcke, H.; Fang, K.;
Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Fick, B.;
Figueira, J. M.; Filevich, A.; Filipčič, A.; Fratu, O.; Freire,
M. M.; Fujii, T.; García, B.; García-Gámez, D.; Garcia-Pinto, D.;
Gate, F.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.; Giaccari, U.;
Giammarchi, M.; Giller, M.; Głas, D.; Glaser, C.; Glass, H.; Golup,
G.; Gómez Berisso, M.; Gómez Vitale, P. F.; González, N.; Gookin,
B.; Gordon, J.; Gorgi, A.; Gorham, P.; Gouffon, P.; Griffith, N.;
Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel, M. R.;
Hansen, P.; Harari, D.; Harrison, T. A.; Hartmann, S.; Harton, J. L.;
Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Hérve, A. E.; Hill,
G. C.; Hojvat, C.; Hollon, N.; Holt, E.; Homola, P.; Hörandel, J. R.;
Horvath, P.; Hrabovský, M.; Huber, D.; Huege, T.; Insolia, A.; Isar,
P. G.; Jandt, I.; Jansen, S.; Jarne, C.; Johnsen, J. A.; Josebachuili,
M.; Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.;
Keilhauer, B.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges,
M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Kuempel, D.; Kukec Mezek,
G.; Kunka, N.; Kuotb Awad, A. W.; LaHurd, D.; Latronico, L.; Lauer,
R.; Lauscher, M.; Lautridou, P.; Le Coz, S.; Lebrun, D.; Lebrun, P.;
Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link,
K.; Lopes, L.; López, R.; López Casado, A.; Louedec, K.; Lucero,
A.; Malacari, M.; Mallamaci, M.; Maller, J.; Mandat, D.; Mantsch, P.;
Mariazzi, A. G.; Marin, V.; Mariş, I. C.; Marsella, G.; Martello,
D.; Martinez, H.; Martínez Bravo, O.; Martraire, D.; Masías Meza,
J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews, J. A. J.;
Matthiae, G.; Maurizio, D.; Mayotte, E.; Mazur, P. O.; Medina, C.;
Medina-Tanco, G.; Meissner, R.; Mello, V. B. B.; Melo, D.; Menshikov,
A.; Messina, S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.;
Miramonti, L.; Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Montanet,
F.; Morello, C.; Mostafá, M.; Moura, C. A.; Müller, G.; Muller,
M. A.; Müller, S.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.;
Neuser, J.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol, M.;
Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.; Nožka,
L.; Núñez, L. A.; Ochilo, L.; Oikonomou, F.; Olinto, A.; Pacheco, N.;
Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Papenbreer, P.; Parente,
G.; Parra, A.; Paul, T.; Pech, M.; Pękala, J.; Pelayo, R.; Pepe,
I. M.; Perrone, L.; Petermann, E.; Peters, C.; Petrera, S.; Petrov,
Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.;
Pirronello, V.; Platino, M.; Plum, M.; Porcelli, A.; Porowski, C.;
Prado, R. R.; Privitera, P.; Prouza, M.; Quel, E. J.; Querchfeld,
S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.; Reinert, D.;
Revenu, B.; Ridky, J.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de
Carvalho, W.; Rodriguez Rojo, J.; Rodríguez-Frías, M. D.; Rogozin,
D.; Rosado, J.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sanabria Gomez, J. D.; Sánchez, F.; Sanchez-Lucas, P.;
Santos, E. M.; Santos, E.; Sarazin, F.; Sarkar, B.; Sarmento, R.;
Sarmiento-Cano, C.; Sato, R.; Scarso, C.; Schauer, M.; Scherini, V.;
Schieler, H.; Schmidt, D.; Scholten, O.; Schoorlemmer, H.; Schovánek,
P.; Schröder, F. G.; Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto,
S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sigl,
G.; Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers,
P.; Sonntag, S.; Sorokin, J.; Squartini, R.; Srivastava, Y. N.;
Stanca, D.; Stanič, S.; Stapleton, J.; Stasielak, J.; Stephan, M.;
Stutz, A.; Suarez, F.; Suarez Durán, M.; Suomijärvi, T.; Supanitsky,
A. D.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Taborda, O. A.;
Tapia, A.; Tepe, A.; Theodoro, V. M.; Tibolla, O.; Timmermans, C.;
Todero Peixoto, C. J.; Toma, G.; Tomankova, L.; Tomé, B.; Tonachini,
A.; Torralba Elipe, G.; Torres Machado, D.; Travnicek, P.; Trini, M.;
Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño,
I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.;
van Velzen, S.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.;
Varner, G.; Vasquez, R.; Vázquez, J. R.; Vázquez, R. A.; Veberič,
D.; Verzi, V.; Vicha, J.; Videla, M.; Villaseñor, L.; Vlcek, B.;
Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz, D.; Watson, A. A.;
Weber, M.; Weidenhaupt, K.; Weindl, A.; Welling, C.; Werner, F.;
Widom, A.; Wiencke, L.; Wilczyński, H.; Winchen, T.; Wittkowski,
D.; Wundheiler, B.; Wykes, S.; Yang, L.; Yapici, T.; Yushkov, A.;
Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zepeda, A.; Zimmermann, B.;
Ziolkowski, M.; Zuccarello, F.
2015arXiv150903732T Altcode:
Contributions of the Pierre Auger Collaboration to the 34th
International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague,
The Netherlands
---------------------------------------------------------
Title: Search for patterns by combining cosmic-ray energy and arrival
directions at the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai,
I. Al; Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison,
P.; Almela, A.; Castillo, J. Alvarez; Alvarez-Muñiz, J.; Batista,
R. Alves; Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa,
S.; Aramo, C.; Aranda, V. M.; Arqueros, F.; Asorey, H.; Assis, P.;
Aublin, J.; Ave, M.; Avenier, M.; Avila, G.; Awal, N.; Badescu, A. M.;
Barber, K. B.; Bäuml, J.; Baus, C.; Beatty, J. J.; Becker, K. H.;
Bellido, J. A.; Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann,
P. L.; Billoir, P.; Blaess, S.; Blanco, M.; Bleve, C.; Blümer, H.;
Boháčová, M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.;
Brack, J.; Brancus, I.; Bridgeman, A.; Brogueira, P.; Brown, W. C.;
Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora,
K. S.; Caccianiga, B.; Caccianiga, L.; Candusso, M.; Caramete, L.;
Caruso, R.; Castellina, A.; Cataldi, G.; Cazon, L.; Cester, R.;
Chavez, A. G.; Chiavassa, A.; Chinellato, J. A.; Chudoba, J.; Cilmo,
M.; Clay, R. W.; Cocciolo, G.; Colalillo, R.; Coleman, A.; Collica,
L.; Coluccia, M. R.; Conceição, R.; Contreras, F.; Cooper, M. J.;
Cordier, A.; Coutu, S.; Covault, C. E.; Cronin, J.; Curutiu, A.;
Dallier, R.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.;
Almeida, R. M. de; Domenico, M. De; Jong, S. J. de; Neto, J. R. T. de
Mello; Mitri, I. De; Oliveira, J. de; Souza, V. de; Peral, L. del;
Deligny, O.; Dembinski, H.; Dhital, N.; Giulio, C. Di; Matteo, A. Di;
Diaz, J. C.; Castro, M. L. Díaz; Diogo, F.; Dobrigkeit, C.; Docters,
W.; D'Olivo, J. C.; Dorofeev, A.; Hasankiadeh, Q. Dorosti; Dova,
M. T.; Ebr, J.; Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.;
Espadanal, J.; Etchegoyen, A.; Luis, P. Facal San; Falcke, H.; Fang,
K.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Fernandes,
M.; Fick, B.; Figueira, J. M.; Filevich, A.; Filipčič, A.; Fox,
B. D.; Fratu, O.; Fröhlich, U.; Fuchs, B.; Fujii, T.; Gaior, R.;
García, B.; Roca, S. T. Garcia; Garcia-Gamez, D.; Garcia-Pinto, D.;
Garilli, G.; Bravo, A. Gascon; Gate, F.; Gemmeke, H.; Ghia, P. L.;
Giaccari, U.; Giammarchi, M.; Giller, M.; Glaser, C.; Glass, H.;
Berisso, M. Gómez; Vitale, P. F. Gómez; Gonçalves, P.; Gonzalez,
J. G.; González, N.; Gookin, B.; Gordon, J.; Gorgi, A.; Gorham, P.;
Gouffon, P.; Grebe, S.; Griffith, N.; Grillo, A. F.; Grubb, T. D.;
Guarino, F.; Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.;
Harrison, T. A.; Hartmann, S.; Harton, J. L.; Haungs, A.; Hebbeker,
T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.;
Hollon, N.; Holt, E.; Homola, P.; Hörandel, J. R.; Horvath, P.;
Hrabovský, M.; Huber, D.; Huege, T.; Insolia, A.; Isar, P. G.; Jandt,
I.; Jansen, S.; Jarne, C.; Josebachuili, M.; Kääpä, A.; Kambeitz,
O.; Kampert, K. H.; Kasper, P.; Katkov, I.; Kégl, B.; Keilhauer, B.;
Keivani, A.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.;
Kleinfeller, J.; Krause, R.; Krohm, N.; Krömer, O.; Kruppke-Hansen,
D.; Kuempel, D.; Kunka, N.; LaHurd, D.; Latronico, L.; Lauer, R.;
Lauscher, M.; Lautridou, P.; Coz, S. Le; Leão, M. S. A. B.; Lebrun,
D.; Lebrun, P.; Oliveira, M. A. Leigui de; Letessier-Selvon, A.;
Lhenry-Yvon, I.; Link, K.; López, R.; Agüera, A. Lopez; Louedec,
K.; Bahilo, J. Lozano; Lu, L.; Lucero, A.; Ludwig, M.; Malacari,
M.; Maldera, S.; Mallamaci, M.; Maller, J.; Mandat, D.; Mantsch, P.;
Mariazzi, A. G.; Marin, V.; Mariş, I. C.; Marsella, G.; Martello, D.;
Martin, L.; Martinez, H.; Bravo, O. Martínez; Martraire, D.; Meza,
J. J. Masías; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews,
J. A. J.; Matthiae, G.; Maurel, D.; Maurizio, D.; Mayotte, E.; Mazur,
P. O.; Medina, C.; Medina-Tanco, G.; Meissner, R.; Melissas, M.;
Melo, D.; Menshikov, A.; Messina, S.; Meyhandan, R.; Mićanović,
S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.; Miramonti, L.;
Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Monasor, M.; Ragaigne,
D. Monnier; Montanet, F.; Morello, C.; Mostafá, M.; Moura, C. A.;
Muller, M. A.; Müller, G.; Müller, S.; Münchmeyer, M.; Mussa,
R.; Navarra, G.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.;
Neuser, J.; Nguyen, P.; Niechciol, M.; Niemietz, L.; Niggemann, T.;
Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.; Ochilo, L.; Olinto,
A.; Oliveira, M.; Pacheco, N.; Selmi-Dei, D. Pakk; Palatka, M.;
Pallotta, J.; Palmieri, N.; Papenbreer, P.; Parente, G.; Parra, A.;
Paul, T.; Pech, M.; Pȩkala, J.; Pelayo, R.; Pepe, I. M.; Perrone,
L.; Petermann, E.; Peters, C.; Petrera, S.; Petrov, Y.; Phuntsok,
J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello,
V.; Platino, M.; Plum, M.; Porcelli, A.; Porowski, C.; Prado, R. R.;
Privitera, P.; Prouza, M.; Purrello, V.; Quel, E. J.; Querchfeld,
S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani, D.; Revenu, B.;
Ridky, J.; Riggi, S.; Risse, M.; Ristori, P.; Rizi, V.; Carvalho,
W. Rodrigues de; Cabo, I. Rodriguez; Fernandez, G. Rodriguez; Rojo,
J. Rodriguez; Rodríguez-Frías, M. D.; Rogozin, D.; Ros, G.; Rosado,
J.; Rossler, T.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.; Greus, F. Salesa;
Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santo, C. E.; Santos,
E.; Santos, E. M.; Sarazin, F.; Sarkar, B.; Sarmento, R.; Sato, R.;
Scharf, N.; Scherini, V.; Schieler, H.; Schiffer, P.; Schmidt, D.;
Schröder, F. G.; Scholten, O.; Schoorlemmer, H.; Schovánek, P.;
Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto, S. J.; Segreto, A.;
Settimo, M.; Shadkam, A.; Shellard, R. C.; Sidelnik, I.; Sigl, G.;
Sima, O.; kowski, A. Śmiał; Šmída, R.; Snow, G. R.; Sommers, P.;
Sorokin, J.; Squartini, R.; Srivastava, Y. N.; Stanič, S.; Stapleton,
J.; Stasielak, J.; Stephan, M.; Stutz, A.; Suarez, F.; Suomijärvi,
T.; Supanitsky, A. D.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.;
Szuba, M.; Taborda, O. A.; Tapia, A.; Tartare, M.; Tepe, A.; Theodoro,
V. M.; Timmermans, C.; Peixoto, C. J. Todero; Toma, G.; Tomankova,
L.; Tomé, B.; Tonachini, A.; Elipe, G. Torralba; Machado, D. Torres;
Travnicek, P.; Trovato, E.; Tueros, M.; Ulrich, R.; Unger, M.; Urban,
M.; Galicia, J. F. Valdés; Valiño, I.; Valore, L.; Aar, G. van;
Bodegom, P. van; Berg, A. M. van den; Velzen, S. van; Vliet, A. van;
Varela, E.; Vargas Cárdenas, B.; Varner, G.; Vázquez, J. R.;
Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha, J.; Videla, M.;
Villaseñor, L.; Vlcek, B.; Vorobiov, S.; Wahlberg, H.; Wainberg,
O.; Walz, D.; Watson, A. A.; Weber, M.; Weidenhaupt, K.; Weindl, A.;
Werner, F.; Widom, A.; Wiencke, L.; Wilczyńska, B.; Wilczyński, H.;
Will, M.; Williams, C.; Winchen, T.; Wittkowski, D.; Wundheiler, B.;
Wykes, S.; Yamamoto, T.; Yapici, T.; Yuan, G.; Yushkov, A.; Zamorano,
B.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zaw, I.; Zepeda, A.; Zhou,
J.; Zhu, Y.; Silva, M. Zimbres; Ziolkowski, M.; Zuccarello, F.
2015EPJC...75..269A Altcode: 2014arXiv1410.0515T
Energy-dependent patterns in the arrival directions of cosmic rays
are searched for using data of the Pierre Auger Observatory. We
investigate local regions around the highest-energy cosmic rays with
eV by analyzing cosmic rays with energies above eV arriving within an
angular separation of approximately 15. We characterize the energy
distributions inside these regions by two independent methods, one
searching for angular dependence of energy-energy correlations and one
searching for collimation of energy along the local system of principal
axes of the energy distribution. No significant patterns are found with
this analysis. The comparison of these measurements with astrophysical
scenarios can therefore be used to obtain constraints on related model
parameters such as strength of cosmic-ray deflection and density of
point sources.
---------------------------------------------------------
Title: Improved limit to the diffuse flux of ultrahigh energy
neutrinos from the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Al Samarai, I.;
Albuquerque, I. F. M.; Allekotte, I.; Allison, P.; Almela, A.; Alvarez
Castillo, J.; Alvarez-Muñiz, J.; Alves Batista, R.; Ambrosio, M.;
Aminaei, A.; Anchordoqui, L.; Andringa, S.; Aramo, C.; Aranda, V. M.;
Arqueros, F.; Arsene, N.; Asorey, H.; Assis, P.; Aublin, J.; Ave,
M.; Avenier, M.; Avila, G.; Awal, N.; Badescu, A. M.; Barber, K. B.;
Bäuml, J.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.;
Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Billoir,
P.; Blaess, S. G.; Blanco, A.; Blanco, M.; Bleve, C.; Blümer, H.;
Boháčová, M.; Boncioli, D.; Bonifazi, C.; Borodai, N.; Brack, J.;
Brancus, I.; Bridgeman, A.; Brogueira, P.; Brown, W. C.; Buchholz,
P.; Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.;
Caccianiga, B.; Caccianiga, L.; Candusso, M.; Caramete, L.; Caruso,
R.; Castellina, A.; Cataldi, G.; Cazon, L.; Cester, R.; Chavez, A. G.;
Chiavassa, A.; Chinellato, J. A.; Chudoba, J.; Cilmo, M.; Clay, R. W.;
Cocciolo, G.; Colalillo, R.; Coleman, A.; Collica, L.; Coluccia,
M. R.; Conceição, R.; Contreras, F.; Cooper, M. J.; Cordier, A.;
Coutu, S.; Covault, C. E.; Cronin, J.; Dallier, R.; Daniel, B.; Dasso,
S.; Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; de Jong, S. J.;
De Mauro, G.; de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira,
J.; de Souza, V.; del Peral, L.; Deligny, O.; Dembinski, H.; Dhital,
N.; Di Giulio, C.; Di Matteo, A.; Diaz, J. C.; Díaz Castro, M. L.;
Diogo, F.; Dobrigkeit, C.; Docters, W.; D'Olivo, J. C.; Dorofeev, A.;
Dorosti Hasankiadeh, Q.; Dova, M. T.; Ebr, J.; Engel, R.; Erdmann,
M.; Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Falcke,
H.; Fang, K.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.;
Fernandes, M.; Fick, B.; Figueira, J. M.; Filevich, A.; Filipčič, A.;
Fox, B. D.; Fratu, O.; Freire, M. M.; Fuchs, B.; Fujii, T.; García,
B.; Garcia-Pinto, D.; Gate, F.; Gemmeke, H.; Gherghel-Lascu, A.;
Ghia, P. L.; Giaccari, U.; Giammarchi, M.; Giller, M.; Głas, D.;
Glaser, C.; Glass, H.; Golup, G.; Gómez Berisso, M.; Gómez Vitale,
P. F.; González, N.; Gookin, B.; Gordon, J.; Gorgi, A.; Gorham, P.;
Gouffon, P.; Griffith, N.; Grillo, A. F.; Grubb, T. D.; Guardincerri,
Y.; Guarino, F.; Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.;
Harrison, T. A.; Hartmann, S.; Harton, J. L.; Haungs, A.; Hebbeker,
T.; Heck, D.; Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.;
Hollon, N.; Holt, E.; Homola, P.; Hörandel, J. R.; Horvath, P.;
Hrabovský, M.; Huber, D.; Huege, T.; Insolia, A.; Isar, P. G.;
Jandt, I.; Jansen, S.; Jarne, C.; Johnsen, J. A.; Josebachuili, M.;
Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.;
Kégl, B.; Keilhauer, B.; Keivani, A.; Kemp, E.; Kieckhafer, R. M.;
Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.;
Krömer, O.; Kuempel, D.; Kunka, N.; LaHurd, D.; Latronico, L.; Lauer,
R.; Lauscher, M.; Lautridou, P.; Le Coz, S.; Lebrun, D.; Lebrun, P.;
Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.;
Link, K.; Lopes, L.; López, R.; López Casado, A.; Louedec, K.; Lu,
L.; Lucero, A.; Malacari, M.; Maldera, S.; Mallamaci, M.; Maller, J.;
Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, V.; Mariş, I. C.;
Marsella, G.; Martello, D.; Martin, L.; Martinez, H.; Martínez Bravo,
O.; Martraire, D.; Masías Meza, J. J.; Mathes, H. J.; Mathys, S.;
Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Maurel, D.; Maurizio,
D.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Meissner,
R.; Mello, V. B. B.; Melo, D.; Menshikov, A.; Messina, S.; Meyhandan,
R.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.; Miramonti, L.;
Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Montanet, F.; Morello,
C.; Mostafá, M.; Moura, C. A.; Muller, M. A.; Müller, G.; Müller,
S.; Mussa, R.; Navarra, G.; Navarro, J. L.; Navas, S.; Necesal, P.;
Nellen, L.; Nelles, A.; Neuser, J.; Nguyen, P. H.; Niculescu-Oglinzanu,
M.; Niechciol, M.; Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek,
D.; Novotny, V.; Nožka, L.; Ochilo, L.; Oikonomou, F.; Olinto, A.;
Pacheco, N.; Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Papenbreer,
P.; Parente, G.; Parra, A.; Paul, T.; Pech, M.; Pękala, J.; Pelayo,
R.; Pepe, I. M.; Perrone, L.; Petermann, E.; Peters, C.; Petrera,
S.; Petrov, Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.;
Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.; Porcelli, A.;
Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Purrello, V.;
Quel, E. J.; Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.;
Ravignani, D.; Revenu, B.; Ridky, J.; Riggi, S.; Risse, M.; Ristori,
P.; Rizi, V.; Rodrigues de Carvalho, W.; Rodriguez Fernandez, G.;
Rodriguez Rojo, J.; Rodríguez-Frías, M. D.; Rogozin, D.; Rosado,
J.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.; Saftoiu, A.;
Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.; Salina, G.;
Sánchez, F.; Sanchez-Lucas, P.; Santos, E.; Santos, E. M.; Sarazin,
F.; Sarkar, B.; Sarmento, R.; Sato, R.; Scarso, C.; Schauer, M.;
Scherini, V.; Schieler, H.; Schiffer, P.; Schmidt, D.; Scholten, O.;
Schoorlemmer, H.; Schovánek, P.; Schröder, F. G.; Schulz, A.; Schulz,
J.; Schumacher, J.; Sciutto, S. J.; Segreto, A.; Settimo, M.; Shadkam,
A.; Shellard, R. C.; Sidelnik, I.; Sigl, G.; Sima, O.; Śmiałkowski,
A.; Šmída, R.; Snow, G. R.; Sommers, P.; Sorokin, J.; Squartini, R.;
Srivastava, Y. N.; Stanca, D.; Stanič, S.; Stapleton, J.; Stasielak,
J.; Stephan, M.; Stutz, A.; Suarez, F.; Suomijärvi, T.; Supanitsky,
A. D.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Taborda, O. A.;
Tapia, A.; Tepe, A.; Theodoro, V. M.; Tiffenberg, J.; Timmermans, C.;
Todero Peixoto, C. J.; Toma, G.; Tomankova, L.; Tomé, B.; Tonachini,
A.; Torralba Elipe, G.; Torres Machado, D.; Travnicek, P.; Ulrich, R.;
Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.;
van Aar, G.; van Bodegom, P.; van den Berg, A. M.; van Velzen, S.;
van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner, G.; Vasquez,
R.; Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha,
J.; Videla, M.; Villaseñor, L.; Vlcek, B.; Vorobiov, S.; Wahlberg,
H.; Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weidenhaupt,
K.; Weindl, A.; Werner, F.; Widom, A.; Wiencke, L.; Wilczyński,
H.; Winchen, T.; Wittkowski, D.; Wundheiler, B.; Wykes, S.; Yang,
L.; Yapici, T.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zepeda, A.; Zhu, Y.; Zimmermann, B.; Ziolkowski, M.; Zuccarello, F.;
Pierre Auger Collaboration
2015PhRvD..91i2008A Altcode: 2015arXiv150405397T
Neutrinos in the cosmic ray flux with energies near 1 EeV and above
are detectable with the Surface Detector array (SD) of the Pierre
Auger Observatory. We report here on searches through Auger data from
1 January 2004 until 20 June 2013. No neutrino candidates were found,
yielding a limit to the diffuse flux of ultrahigh energy neutrinos that
challenges the Waxman-Bahcall bound predictions. Neutrino identification
is attempted using the broad time structure of the signals expected in
the SD stations, and is efficiently done for neutrinos of all flavors
interacting in the atmosphere at large zenith angles, as well as for
"Earth-skimming" neutrino interactions in the case of tau neutrinos. In
this paper the searches for downward-going neutrinos in the zenith angle
bins 60°-75° and 75°-90° as well as for upward-going neutrinos, are
combined to give a single limit. The 90% C.L. single-flavor limit to
the diffuse flux of ultrahigh energy neutrinos with an E<SUP>-2</SUP>
spectrum in the energy range 1.0 ×1 0<SUP>17</SUP> eV - 2.5 ×1
0<SUP>19</SUP> eV is E<SUB>ν</SUB><SUP>2</SUP>d N<SUB>ν</SUB>/d
E<SUB>ν</SUB><6.4 ×10<SUP>-9</SUP> GeV cm<SUP>-2</SUP>
s<SUP>-1</SUP> sr<SUP>-1</SUP> .
---------------------------------------------------------
Title: Searches for Anisotropies in the Arrival Directions of the
Highest Energy Cosmic Rays Detected by the Pierre Auger Observatory
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai, I. Al;
Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela,
A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves Batista, R.;
Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Aramo, C.;
Aranda, V. M.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave,
M.; Avenier, M.; Avila, G.; Awal, N.; Badescu, A. M.; Barber, K. B.;
Bäuml, J.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.;
Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Billoir,
P.; Blaess, S. G.; Blanco, M.; Bleve, C.; Blümer, H.; Boháčová,
M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.; Brack, J.;
Brancus, I.; Bridgeman, A.; Brogueira, P.; Brown, W. C.; Buchholz, P.;
Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga,
B.; Caccianiga, L.; Candusso, M.; Caramete, L.; Caruso, R.; Castellina,
A.; Cataldi, G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.;
Chinellato, J. A.; Chudoba, J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.;
Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição,
R.; Contreras, F.; Cooper, M. J.; Cordier, A.; Coutu, S.; Covault,
C. E.; Cronin, J.; Curutiu, A.; Dallier, R.; Daniel, B.; Dasso, S.;
Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; De Domenico, M.;
de Jong, S. J.; de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira,
J.; de Souza, V.; del Peral, L.; Deligny, O.; Dembinski, H.; Dhital,
N.; Di Giulio, C.; Di Matteo, A.; Diaz, J. C.; Díaz Castro, M. L.;
Diogo, F.; Dobrigkeit, C.; Docters, W.; D'Olivo, J. C.; Dorofeev, A.;
Dorosti Hasankiadeh, Q.; Dova, M. T.; Ebr, J.; Engel, R.; Erdmann,
M.; Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.;
Facal San Luis, P.; Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.;
Fazzini, N.; Ferguson, A. P.; Fernandes, M.; Fick, B.; Figueira,
J. M.; Filevich, A.; Filipčič, A.; Fox, B. D.; Fratu, O.; Freire,
M. M.; Fröhlich, U.; Fuchs, B.; Fujii, T.; Gaior, R.; García, B.;
Garcia-Gamez, D.; Garcia-Pinto, D.; Garilli, G.; Gascon Bravo, A.;
Gate, F.; Gemmeke, H.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.;
Giller, M.; Glaser, C.; Glass, H.; Gómez Berisso, M.; Gómez Vitale,
P. F.; Gonçalves, P.; Gonzalez, J. G.; González, N.; Gookin, B.;
Gordon, J.; Gorgi, A.; Gorham, P.; Gouffon, P.; Grebe, S.; Griffith,
N.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel,
M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Hartmann, S.; Harton,
J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Herve, A. E.;
Hill, G. C.; Hojvat, C.; Hollon, N.; Holt, E.; Homola, P.; Hörandel,
J. R.; Horvath, P.; Hrabovský, M.; Huber, D.; Huege, T.; Insolia,
A.; Isar, P. G.; Jandt, I.; Jansen, S.; Jarne, C.; Josebachuili, M.;
Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.;
Kégl, B.; Keilhauer, B.; Keivani, A.; Kemp, E.; Kieckhafer, R. M.;
Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.;
Krömer, O.; Kruppke-Hansen, D.; Kuempel, D.; Kunka, N.; LaHurd, D.;
Latronico, L.; Lauer, R.; Lauscher, M.; Lautridou, P.; Le Coz, S.;
Leão, M. S. A. B.; Lebrun, D.; Lebrun, P.; Leigui de Oliveira, M. A.;
Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; López, R.; Louedec,
K.; Lozano Bahilo, J.; Lu, L.; Lucero, A.; Ludwig, M.; Malacari,
M.; Maldera, S.; Mallamaci, M.; Maller, J.; Mandat, D.; Mantsch, P.;
Mariazzi, A. G.; Marin, V.; Mariş, I. C.; Marsella, G.; Martello,
D.; Martin, L.; Martinez, H.; Martínez Bravo, O.; Martraire, D.;
Masías Meza, J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews,
J. A. J.; Matthiae, G.; Maurel, D.; Maurizio, D.; Mayotte, E.; Mazur,
P. O.; Medina, C.; Medina-Tanco, G.; Meissner, R.; Melissas, M.;
Melo, D.; Menshikov, A.; Messina, S.; Meyhandan, R.; Mićanović,
S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.; Miramonti, L.;
Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Monasor, M.; Monnier
Ragaigne, D.; Montanet, F.; Morello, C.; Mostafá, M.; Moura, C. A.;
Muller, M. A.; Müller, G.; Müller, S.; Münchmeyer, M.; Mussa, R.;
Navarra, G.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.; Neuser,
J.; Nguyen, P. H.; Niechciol, M.; Niemietz, L.; Niggemann, T.; Nitz,
D.; Nosek, D.; Novotny, V.; Nožka, L.; Ochilo, L.; Oikonomou,
F.; Olinto, A.; Oliveira, M.; Pacheco, N.; Pakk Selmi-Dei, D.;
Palatka, M.; Pallotta, J.; Palmieri, N.; Papenbreer, P.; Parente,
G.; Parra, A.; Paul, T.; Pech, M.; Pȩkala, J.; Pelayo, R.; Pepe,
I. M.; Perrone, L.; Petermann, E.; Peters, C.; Petrera, S.; Petrov,
Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.;
Pirronello, V.; Platino, M.; Plum, M.; Porcelli, A.; Porowski, C.;
Prado, R. R.; Privitera, P.; Prouza, M.; Purrello, V.; Quel, E. J.;
Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani,
D.; Revenu, B.; Ridky, J.; Riggi, S.; Risse, M.; Ristori, P.; Rizi,
V.; Rodrigues de Carvalho, W.; Rodriguez Fernandez, G.; Rodriguez
Rojo, J.; Rodríguez-Frías, M. D.; Rogozin, D.; Ros, G.; Rosado,
J.; Rossler, T.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santo, C. E.; Santos,
E.; Santos, E. M.; Sarazin, F.; Sarkar, B.; Sarmento, R.; Sato, R.;
Scharf, N.; Scherini, V.; Schieler, H.; Schiffer, P.; Schmidt, D.;
Scholten, O.; Schoorlemmer, H.; Schovánek, P.; Schröder, F. G.;
Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto, S. J.; Segreto, A.;
Settimo, M.; Shadkam, A.; Shellard, R. C.; Sidelnik, I.; Sigl, G.;
Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers, P.;
Sorokin, J.; Squartini, R.; Srivastava, Y. N.; Stanič, S.; Stapleton,
J.; Stasielak, J.; Stephan, M.; Stutz, A.; Suarez, F.; Suomijärvi,
T.; Supanitsky, A. D.; Sutherland, M. S.; Swain, J.; Szadkowski,
Z.; Szuba, M.; Taborda, O. A.; Tapia, A.; Tepe, A.; Theodoro, V. M.;
Timmermans, C.; Todero Peixoto, C. J.; Toma, G.; Tomankova, L.; Tomé,
B.; Tonachini, A.; Torralba Elipe, G.; Torres Machado, D.; Travnicek,
P.; Trovato, E.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia,
J. F.; Valiño, I.; Valore, L.; van Aar, G.; van Bodegom, P.;
van den Berg, A. M.; van Velzen, S.; van Vliet, A.; Varela, E.;
Vargas Cárdenas, B.; Varner, G.; Vázquez, J. R.; Vázquez, R. A.;
Veberič, D.; Verzi, V.; Vicha, J.; Videla, M.; Villase ñor, L.;
Vlcek, B.; Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz, D.; Watson,
A. A.; Weber, M.; Weidenhaupt, K.; Weindl, A.; Werner, F.; Widom,
A.; Wiencke, L.; Wilczyńska, B.; Wilczyński, H.; Williams, C.;
Winchen, T.; Wittkowski, D.; Wundheiler, B.; Wykes, S.; Yamamoto, T.;
Yapici, T.; Yuan, G.; Yushkov, A.; Zamorano, B.; Zas, E.; Zavrtanik,
D.; Zavrtanik, M.; Zepeda, A.; Zhou, J.; Zhu, Y.; Zimbres Silva, M.;
Ziolkowski, M.; Zuccarello, F.; Pierre Auger Collaboration
2015ApJ...804...15A Altcode: 2014arXiv1411.6111P
We analyze the distribution of arrival directions of ultra-high-energy
cosmic rays recorded at the Pierre Auger Observatory in 10 years
of operation. The data set, about three times larger than that
used in earlier studies, includes arrival directions with zenith
angles up to 80°, thus covering from -90{}^\circ to +45{}^\circ in
declination. After updating the fraction of events correlating with
the active galactic nuclei (AGNs) in the Véron-Cetty and Véron
catalog, we subject the arrival directions of the data with energies
in excess of 40 EeV to different tests for anisotropy. We search for
localized excess fluxes, self-clustering of event directions at angular
scales up to 30°, and different threshold energies between 40 and
80 EeV. We then look for correlations of cosmic rays with celestial
structures both in the Galaxy (the Galactic Center and Galactic Plane)
and in the local universe (the Super-Galactic Plane). We also examine
their correlation with different populations of nearby extragalactic
objects: galaxies in the 2MRS catalog, AGNs detected by Swift-BAT,
radio galaxies with jets, and the Centaurus A (Cen A) galaxy. None of
the tests show statistically significant evidence of anisotropy. The
strongest departures from isotropy (post-trial probability ∼ 1.4%)
are obtained for cosmic rays with E\gt 58 EeV in rather large windows
around Swift AGNs closer than 130 Mpc and brighter than 10<SUP>44</SUP>
erg s<SUP>-1</SUP> (18° radius), and around the direction of Cen A
(15° radius).
---------------------------------------------------------
Title: Large Scale Distribution of Ultra High Energy Cosmic Rays
Detected at the Pierre Auger Observatory with Zenith Angles up to 80°
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Samarai, I. Al;
Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela,
A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves Batista, R.;
Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Aramo, C.;
Aranda, V. M.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave,
M.; Avenier, M.; Avila, G.; Awal, N.; Badescu, A. M.; Barber, K. B.;
Bäuml, J.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.;
Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Billoir,
P.; Blaess, S. G.; Blanco, M.; Bleve, C.; Blümer, H.; Boháčová,
M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.; Brack, J.;
Brancus, I.; Bridgeman, A.; Brogueira, P.; Brown, W. C.; Buchholz, P.;
Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga,
B.; Caccianiga, L.; Candusso, M.; Caramete, L.; Caruso, R.; Castellina,
A.; Cataldi, G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.;
Chinellato, J. A.; Chudoba, J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.;
Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição,
R.; Contreras, F.; Cooper, M. J.; Cordier, A.; Coutu, S.; Covault,
C. E.; Cronin, J.; Curutiu, A.; Dallier, R.; Daniel, B.; Dasso, S.;
Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; De Domenico, M.;
de Jong, S. J.; de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira,
J.; de Souza, V.; del Peral, L.; Deligny, O.; Dembinski, H.; Dhital,
N.; Di Giulio, C.; Di Matteo, A.; Diaz, J. C.; Díaz Castro, M. L.;
Diogo, F.; Dobrigkeit, C.; Docters, W.; D'Olivo, J. C.; Dorofeev, A.;
Dorosti Hasankiadeh, Q.; Dova, M. T.; Ebr, J.; Engel, R.; Erdmann,
M.; Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.;
Facal San Luis, P.; Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.;
Fazzini, N.; Ferguson, A. P.; Fernandes, M.; Fick, B.; Figueira,
J. M.; Filevich, A.; Filipčič, A.; Fox, B. D.; Fratu, O.; Freire,
M. M.; Fröhlich, U.; Fuchs, B.; Fujii, T.; Gaior, R.; García, B.;
Garcia-Gamez, D.; Garcia-Pinto, D.; Garilli, G.; Gascon Bravo, A.;
Gate, F.; Gemmeke, H.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.;
Giller, M.; Glaser, C.; Glass, H.; Gómez Berisso, M.; Gómez Vitale,
P. F.; Gonçalves, P.; Gonzalez, J. G.; González, N.; Gookin, B.;
Gordon, J.; Gorgi, A.; Gorham, P.; Gouffon, P.; Grebe, S.; Griffith,
N.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel,
M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Hartmann, S.; Harton,
J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Herve, A. E.;
Hill, G. C.; Hojvat, C.; Hollon, N.; Holt, E.; Homola, P.; Hörandel,
J. R.; Horvath, P.; Hrabovský, M.; Huber, D.; Huege, T.; Insolia,
A.; Isar, P. G.; Jandt, I.; Jansen, S.; Jarne, C.; Josebachuili, M.;
Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.;
Kégl, B.; Keilhauer, B.; Keivani, A.; Kemp, E.; Kieckhafer, R. M.;
Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.;
Krömer, O.; Kruppke-Hansen, D.; Kuempel, D.; Kunka, N.; LaHurd, D.;
Latronico, L.; Lauer, R.; Lauscher, M.; Lautridou, P.; Le Coz, S.;
Leão, M. S. A. B.; Lebrun, D.; Lebrun, P.; Leigui de Oliveira, M. A.;
Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; López, R.; Louedec,
K.; Lozano Bahilo, J.; Lu, L.; Lucero, A.; Ludwig, M.; Malacari,
M.; Maldera, S.; Mallamaci, M.; Maller, J.; Mandat, D.; Mantsch, P.;
Mariazzi, A. G.; Marin, V.; Mariş, I. C.; Marsella, G.; Martello,
D.; Martin, L.; Martinez, H.; Martínez Bravo, O.; Martraire, D.;
Masías Meza, J. J.; Mathes, H. J.; Mathys, S.; Matthews, J.; Matthews,
J. A. J.; Matthiae, G.; Maurel, D.; Maurizio, D.; Mayotte, E.; Mazur,
P. O.; Medina, C.; Medina-Tanco, G.; Meissner, R.; Melissas, M.;
Melo, D.; Menshikov, A.; Messina, S.; Meyhandan, R.; Mićanović,
S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.; Miramonti, L.;
Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Monasor, M.; Monnier
Ragaigne, D.; Montanet, F.; Morello, C.; Mostafá, M.; Moura, C. A.;
Muller, M. A.; Müller, G.; Müller, S.; Münchmeyer, M.; Mussa, R.;
Navarra, G.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.; Neuser,
J.; Nguyen, P. H.; Niechciol, M.; Niemietz, L.; Niggemann, T.; Nitz,
D.; Nosek, D.; Novotny, V.; Nožka, L.; Ochilo, L.; Oikonomou,
F.; Olinto, A.; Oliveira, M.; Pacheco, N.; Pakk Selmi-Dei, D.;
Palatka, M.; Pallotta, J.; Palmieri, N.; Papenbreer, P.; Parente,
G.; Parra, A.; Paul, T.; Pech, M.; Pȩkala, J.; Pelayo, R.; Pepe,
I. M.; Perrone, L.; Petermann, E.; Peters, C.; Petrera, S.; Petrov,
Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.;
Pirronello, V.; Platino, M.; Plum, M.; Porcelli, A.; Porowski, C.;
Prado, R. R.; Privitera, P.; Prouza, M.; Purrello, V.; Quel, E. J.;
Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani,
D.; Revenu, B.; Ridky, J.; Riggi, S.; Risse, M.; Ristori, P.; Rizi,
V.; Rodrigues de Carvalho, W.; Rodriguez Fernandez, G.; Rodriguez
Rojo, J.; Rodríguez-Frías, M. D.; Rogozin, D.; Ros, G.; Rosado,
J.; Rossler, T.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santo, C. E.; Santos,
E.; Santos, E. M.; Sarazin, F.; Sarkar, B.; Sarmento, R.; Sato, R.;
Scharf, N.; Scherini, V.; Schieler, H.; Schiffer, P.; Schmidt, D.;
Scholten, O.; Schoorlemmer, H.; Schovánek, P.; Schröder, F. G.;
Schulz, A.; Schulz, J.; Schumacher, J.; Sciutto, S. J.; Segreto, A.;
Settimo, M.; Shadkam, A.; Shellard, R. C.; Sidelnik, I.; Sigl, G.;
Sima, O.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers, P.;
Sorokin, J.; Squartini, R.; Srivastava, Y. N.; Stanič, S.; Stapleton,
J.; Stasielak, J.; Stephan, M.; Stutz, A.; Suarez, F.; Suomijärvi,
T.; Supanitsky, A. D.; Sutherland, M. S.; Swain, J.; Szadkowski,
Z.; Szuba, M.; Taborda, O. A.; Tapia, A.; Tepe, A.; Theodoro, V. M.;
Timmermans, C.; Todero Peixoto, C. J.; Toma, G.; Tomankova, L.; Tomé,
B.; Tonachini, A.; Torralba Elipe, G.; Torres Machado, D.; Travnicek,
P.; Trovato, E.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia,
J. F.; Valiño, I.; Valore, L.; van Aar, G.; van Bodegom, P.;
van den Berg, A. M.; van Velzen, S.; van Vliet, A.; Varela, E.;
Vargas Cárdenas, B.; Varner, G.; Vázquez, J. R.; Vázquez, R. A.;
Veberič, D.; Verzi, V.; Vicha, J.; Videla, M.; Villaseñor, L.;
Vlcek, B.; Vorobiov, S.; Wahlberg, H.; Wainberg, O.; Walz, D.; Watson,
A. A.; Weber, M.; Weidenhaupt, K.; Weindl, A.; Werner, F.; Widom,
A.; Wiencke, L.; Wilczyńska, B.; Wilczyński, H.; Williams, C.;
Winchen, T.; Wittkowski, D.; Wundheiler, B.; Wykes, S.; Yamamoto, T.;
Yapici, T.; Yuan, G.; Yushkov, A.; Zamorano, B.; Zas, E.; Zavrtanik,
D.; Zavrtanik, M.; Zepeda, A.; Zhou, J.; Zhu, Y.; Zimbres Silva, M.;
Ziolkowski, M.; Zuccarello, F.
2015ApJ...802..111A Altcode: 2014arXiv1411.6953T
We present the results of an analysis of the large angular scale
distribution of the arrival directions of cosmic rays with energy above
4 EeV detected at the Pierre Auger Observatory including for the first
time events with zenith angle between 60° and 80°. We perform two
Rayleigh analyses, one in the right ascension and one in the azimuth
angle distributions, that are sensitive to modulations in right
ascension and declination, respectively. The largest departure from
isotropy appears in the E\gt 8 EeV energy bin, with an amplitude for the
first harmonic in right ascension r<SUB>1</SUB><SUP>α </SUP>=(4.4+/-
1.0)× {{10}<SUP>-2</SUP>}, that has a chance probability P(≥slant
r<SUB>1</SUB><SUP>α </SUP>)=6.4× {{10}<SUP>-5</SUP>}, reinforcing
the hint previously reported with vertical events alone.
---------------------------------------------------------
Title: The magnetic structure of surges in small-scale emerging
flux regions
Authors: MacTaggart, D.; Guglielmino, S. L.; Haynes, A. L.; Simitev,
R.; Zuccarello, F.
2015A&A...576A...4M Altcode: 2015arXiv150201842M
<BR /> Aims: We investigate the relationship between surges and
magnetic reconnection during the emergence of small-scale active
regions. In particular, to examine how the large-scale geometry
of the magnetic field, shaped by different phases of reconnection,
guides the flowing of surges. <BR /> Methods: We present three flux
emergence models. The first model, and the simplest, consists of a
region emerging into a horizontal ambient field that is initially
parallel to the top of the emerging region. The second model is the
same as the first but with an extra smaller emerging region which
perturbs the main region. This is added to create a more complex
magnetic topology and to test how this complicates the development of
surges compared to the first model. The last model has a non-uniform
ambient magnetic field to model the effects of emergence near a sunspot
field and impose asymmetry on the system through the ambient magnetic
field. At each stage, we trace the magnetic topology to identify the
locations of reconnection. This allows for field lines to be plotted
from different topological regions, highlighting how their geometry
affects the development of surges. <BR /> Results: In the first model,
we identify distinct phases of reconnection. Each phase is associated
with a particular geometry for the magnetic field and this determines
the paths of the surges. The second model follows a similar pattern
to the first but with a more complex magnetic topology and extra
eruptions. The third model highlights how an asymmetric ambient field
can result in preferred locations for reconnection, subsequently
guiding the direction of surges. <BR /> Conclusions: Each of the
identified phases highlights the close connection between magnetic
field geometry, reconnection and the flow of surges. These phases can
now be detected observationally and may prove to be key signatures in
determining whether or not an emerging region will produce a large-scale
(CME-type) eruption. <P />Appendix is available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201424646/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: Muons in air showers at the Pierre Auger Observatory: Mean
number in highly inclined events
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Al Samarai, I.;
Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela,
A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves Batista, R.;
Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Aramo, C.;
Aranda, V. M.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave,
M.; Avenier, M.; Avila, G.; Badescu, A. M.; Barber, K. B.; Bäuml,
J.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.; Berat,
C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Billoir, P.; Blanco,
M.; Bleve, C.; Blümer, H.; Boháčová, M.; Boncioli, D.; Bonifazi,
C.; Bonino, R.; Borodai, N.; Brack, J.; Brancus, I.; Brogueira, P.;
Brown, W. C.; Buchholz, P.; Bueno, A.; Buitink, S.; Buscemi, M.;
Caballero-Mora, K. S.; Caccianiga, B.; Caccianiga, L.; Candusso, M.;
Caramete, L.; Caruso, R.; Castellina, A.; Cataldi, G.; Cazon, L.;
Cester, R.; Chavez, A. G.; Chiavassa, A.; Chinellato, J. A.; Chudoba,
J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.; Colalillo, R.; Coleman, A.;
Collica, L.; Coluccia, M. R.; Conceição, R.; Contreras, F.; Cooper,
M. J.; Cordier, A.; Coutu, S.; Covault, C. E.; Cronin, J.; Curutiu,
A.; Dallier, R.; Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.;
de Almeida, R. M.; De Domenico, M.; de Jong, S. J.; de Mello Neto,
J. R. T.; De Mitri, I.; de Oliveira, J.; de Souza, V.; del Peral, L.;
Deligny, O.; Dembinski, H.; Dhital, N.; Di Giulio, C.; Di Matteo, A.;
Diaz, J. C.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; Docters,
W.; D'Olivo, J. C.; Dorofeev, A.; Dorosti Hasankiadeh, Q.; Dova, M. T.;
Ebr, J.; Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal,
J.; Etchegoyen, A.; Facal San Luis, P.; Falcke, H.; Fang, K.; Farrar,
G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Fernandes, M.; Fick,
B.; Figueira, J. M.; Filevich, A.; Filipčič, A.; Fox, B. D.; Fratu,
O.; Fröhlich, U.; Fuchs, B.; Fujii, T.; Gaior, R.; García, B.;
Garcia Roca, S. T.; Garcia-Gamez, D.; Garcia-Pinto, D.; Garilli, G.;
Gascon Bravo, A.; Gate, F.; Gemmeke, H.; Ghia, P. L.; Giaccari, U.;
Giammarchi, M.; Giller, M.; Glaser, C.; Glass, H.; Gómez Berisso, M.;
Gómez Vitale, P. F.; Gonçalves, P.; Gonzalez, J. G.; González, N.;
Gookin, B.; Gordon, J.; Gorgi, A.; Gorham, P.; Gouffon, P.; Grebe, S.;
Griffith, N.; Grillo, A. F.; Grubb, T. D.; Guardincerri, Y.; Guarino,
F.; Guedes, G. P.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison,
T. A.; Hartmann, S.; Harton, J. L.; Haungs, A.; Hebbeker, T.; Heck, D.;
Heimann, P.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Hollon, N.; Holt,
E.; Homola, P.; Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huber,
D.; Huege, T.; Insolia, A.; Isar, P. G.; Islo, K.; Jandt, I.; Jansen,
S.; Jarne, C.; Josebachuili, M.; Kääpä, A.; Kambeitz, O.; Kampert,
K. H.; Kasper, P.; Katkov, I.; Kégl, B.; Keilhauer, B.; Keivani, A.;
Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller,
J.; Krause, R.; Krohm, N.; Krömer, O.; Kruppke-Hansen, D.; Kuempel,
D.; Kunka, N.; LaHurd, D.; Latronico, L.; Lauer, R.; Lauscher, M.;
Lautridou, P.; Le Coz, S.; Leão, M. S. A. B.; Lebrun, D.; Lebrun,
P.; Leigui de Oliveira, M. A.; Letessier-Selvon, A.; Lhenry-Yvon,
I.; Link, K.; López, R.; Louedec, K.; Lozano Bahilo, J.; Lu, L.;
Lucero, A.; Ludwig, M.; Malacari, M.; Maldera, S.; Mallamaci, M.;
Maller, J.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, V.;
Mariş, I. C.; Marsella, G.; Martello, D.; Martin, L.; Martinez, H.;
Martínez Bravo, O.; Martraire, D.; Masías Meza, J. J.; Mathes, H. J.;
Mathys, S.; Matthews, J. A. J.; Matthews, J.; Matthiae, G.; Maurel,
D.; Maurizio, D.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco,
G.; Melissas, M.; Melo, D.; Menshikov, A.; Messina, S.; Meyhandan,
R.; Mićanović, S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.;
Miramonti, L.; Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Monasor,
M.; Monnier Ragaigne, D.; Montanet, F.; Morello, C.; Mostafá, M.;
Moura, C. A.; Muller, M. A.; Müller, G.; Münchmeyer, M.; Mussa,
R.; Navarra, G.; Navas, S.; Necesal, P.; Nellen, L.; Nelles, A.;
Neuser, J.; Newton, D.; Niechciol, M.; Niemietz, L.; Niggemann, T.;
Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.; Ochilo, L.; Olinto, A.;
Oliveira, M.; Olmos-Gilbaja, V. M.; Pacheco, N.; Pakk Selmi-Dei, D.;
Palatka, M.; Pallotta, J.; Palmieri, N.; Papenbreer, P.; Parente,
G.; Parra, A.; Paul, T.; Pech, M.; Pekala, J.; Pelayo, R.; Pepe,
I. M.; Perrone, L.; Petermann, E.; Peters, C.; Petrera, S.; Petrov,
Y.; Phuntsok, J.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.;
Pirronello, V.; Platino, M.; Plum, M.; Porcelli, A.; Porowski, C.;
Prado, R. R.; Privitera, P.; Prouza, M.; Purrello, V.; Quel, E. J.;
Querchfeld, S.; Quinn, S.; Rautenberg, J.; Ravel, O.; Ravignani,
D.; Revenu, B.; Ridky, J.; Riggi, S.; Risse, M.; Ristori, P.; Rizi,
V.; Roberts, J.; Rodrigues de Carvalho, W.; Rodriguez Fernandez,
G.; Rodriguez Rojo, J.; Rodríguez-Frías, M. D.; Ros, G.; Rosado,
J.; Rossler, T.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.;
Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.;
Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santo, C. E.; Santos,
E.; Santos, E. M.; Sarazin, F.; Sarkar, B.; Sarmento, R.; Sato,
R.; Scharf, N.; Scherini, V.; Schieler, H.; Schiffer, P.; Scholten,
O.; Schoorlemmer, H.; Schovánek, P.; Schröder, F. G.; Schulz, A.;
Schulz, J.; Schumacher, J.; Sciutto, S. J.; Segreto, A.; Settimo,
M.; Shadkam, A.; Shellard, R. C.; Sidelnik, I.; Sigl, G.; Sima, O.;
Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers, P.; Sorokin,
J.; Squartini, R.; Srivastava, Y. N.; Stanič, S.; Stapleton, J.;
Stasielak, J.; Stephan, M.; Stutz, A.; Suarez, F.; Suomijärvi, T.;
Supanitsky, A. D.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Szuba,
M.; Taborda, O. A.; Tapia, A.; Tartare, M.; Tepe, A.; Theodoro, V. M.;
Timmermans, C.; Todero Peixoto, C. J.; Toma, G.; Tomankova, L.; Tomé,
B.; Tonachini, A.; Torralba Elipe, G.; Torres Machado, D.; Travnicek,
P.; Trovato, E.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia,
J. F.; Valiño, I.; Valore, L.; van Aar, G.; van den Berg, A. M.; van
Velzen, S.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner,
G.; Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha,
J.; Videla, M.; Villaseñor, L.; Vlcek, B.; Vorobiov, S.; Wahlberg,
H.; Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weidenhaupt,
K.; Weindl, A.; Werner, F.; Widom, A.; Wiencke, L.; Wilczyńska, B.;
Wilczyński, H.; Will, M.; Williams, C.; Winchen, T.; Wittkowski, D.;
Wundheiler, B.; Wykes, S.; Yamamoto, T.; Yapici, T.; Younk, P.; Yuan,
G.; Yushkov, A.; Zamorano, B.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zaw, I.; Zepeda, A.; Zhou, J.; Zhu, Y.; Zimbres Silva, M.; Ziolkowski,
M.; Zuccarello, F.; Pierre Auger Collaboration
2015PhRvD..91c2003A Altcode: 2014arXiv1408.1421P
We present the first hybrid measurement of the average muon number in
air showers at ultrahigh energies, initiated by cosmic rays with zenith
angles between 62° and 80°. The measurement is based on 174 hybrid
events recorded simultaneously with the surface detector array and
the fluorescence detector of the Pierre Auger Observatory. The muon
number for each shower is derived by scaling a simulated reference
profile of the lateral muon density distribution at the ground until
it fits the data. A 10<SUP>19</SUP> eV shower with a zenith angle
of 67°, which arrives at the surface detector array at an altitude
of 1450 m above sea level, contains on average (2.68 ±0.04 ±0.48
(sys))×10<SUP>7</SUP> muons with energies larger than 0.3 GeV. The
logarithmic gain d ln N<SUB>μ</SUB>/d ln E of muons with increasing
energy between 4 ×10<SUP>18</SUP> eV and 5 ×10<SUP>19</SUP> eV is
measured to be (1.029 ±0.024 ±0.030 (sys)) .
---------------------------------------------------------
Title: The Signature of Flare Activity in Multifractal Measurements
of Active Regions Observed by SDO/HMI
Authors: Giorgi, F.; Ermolli, I.; Romano, P.; Stangalini, M.;
Zuccarello, F.; Criscuoli, S.
2015SoPh..290..507G Altcode: 2017arXiv170506708G; 2014SoPh..tmp..132G
Recent studies indicate that measurements of fractal and multifractal
parameters of active regions (ARs) are inefficient tools for
distinguishing ARs on the basis of the flare activity or to predict
flare events. In an attempt to validate this result on a large
observation data set of higher spatial and temporal resolution and
higher flux sensitivity than employed in previous studies, we analyzed
high-cadence time series of line-of-sight magnetograms of 43 ARs
characterized by different flare activity, which were observed with
SDO/HMI from May 2010 to December 2013. On these data, we estimated
four parameters, the generalized fractal dimensions D<SUB>0</SUB> and
D<SUB>8</SUB>, and the multifractal parameters C<SUB>div</SUB> and
D<SUB>div</SUB>. We found distinct average values of the parameters
measured on ARs that have hosted flares of different class. However,
the dispersion of values measured on ARs that have produced the same
class of events is such that the parameters deduced from distinct
classes of flaring regions can also largely overlap. Based on the
results of our measurements, C- and M-class flaring ARs are practically
indistinguishable, and the same is true for M- and X-class flaring
ARs. We only found consistent changes on the time series of the
measured parameters on ≈ 50 % of the ARs and ≈ 50 % of the M-
and X-class events. We show that these results hold for fractal and
multifractal parameter estimates based on total unsigned and signed
flux data of the ARs.
---------------------------------------------------------
Title: Time Evolution of Force-Free Parameter and Free Magnetic
Energy in Active Region NOAA 10365
Authors: Valori, G.; Romano, P.; Malanushenko, A.; Ermolli, I.;
Giorgi, F.; Steed, K.; van Driel-Gesztelyi, L.; Zuccarello, F.;
Malherbe, J. -M.
2015SoPh..290..491V Altcode:
We describe the variation of the accumulated coronal helicity derived
from the magnetic helicity flux through the photosphere in active region
(AR) NOAA 10365, where several large flares and coronal mass ejections
(CMEs) occurred. We used SOHO/MDI full-disk line-of-sight magnetograms
to measure the helicity flux, and the integral of GOES X-ray flux as a
proxy of the coronal energy variations due to flares or CMEs. Using the
linear force-free field model, we transformed the accumulated helicity
flux into a time sequence of the force-free parameter α accounting for
flares or CMEs via the proxy derived from GOES observations. This method
can be used to derive the value of α at different times during the
AR evolution, and is a partial alternative to the commonly used match
of field lines with EUV loops. By combining the accumulated helicity
obtained from the observations with the linear force-free theory, we
describe the main phases of the emergence process of the AR, and relate
them temporally with the occurrence of flares or CMEs. Additionally,
a comparison with the loop-matching method of fixing alpha at each time
independently shows that the proposed method may be helpful in avoiding
unrealistic or undetermined values of alpha that may originate from
an insufficient quality of the image used to identify coronal loops
at a given time. For the relative intensity of the considered events,
the linear force-free field theory implies that there is a direct
correlation between the released energy on the one hand and the product
of the coronal helicity with the variation of α due to the event on
the other. Therefore, the higher the value of the accumulated coronal
helicity, the smaller the force-free parameter variation required to
produce the same decrease in the free energy during the CMEs.
---------------------------------------------------------
Title: Depth of maximum of air-shower profiles at the Pierre Auger
Observatory. II. Composition implications
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Al Samarai, I.;
Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela,
A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves Batista, R.;
Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Aramo, C.;
Aranda, V. M.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave,
M.; Avenier, M.; Avila, G.; Awal, N.; Badescu, A. M.; Barber, K. B.;
Bäuml, J.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.;
Berat, C.; Bertania, M. E.; Bertou, X.; Biermann, P. L.; Billoir,
P.; Blaess, S.; Blanco, M.; Bleve, C.; Blümer, H.; Boháčová,
M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.; Brack, J.;
Brancus, I.; Bridgeman, A.; Brogueira, P.; Brown, W. C.; Buchholz, P.;
Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga,
B.; Caccianiga, L.; Candusso, M.; Caramete, L.; Caruso, R.; Castellina,
A.; Cataldi, G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.;
Chinellato, J. A.; Chudoba, J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.;
Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição,
R.; Contreras, F.; Cooper, M. J.; Cordier, A.; Coutu, S.; Covault,
C. E.; Cronin, J.; Curutiu, A.; Dallier, R.; Daniel, B.; Dasso, S.;
Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; De Domenico, M.;
de Jong, S. J.; de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira,
J.; de Souza, V.; del Peral, L.; Deligny, O.; Dembinski, H.; Dhital,
N.; Di Giulio, C.; Di Matteo, A.; Diaz, J. C.; Díaz Castro, M. L.;
Diogo, F.; Dobrigkeit, C.; Docters, W.; D'Olivo, J. C.; Dorofeev, A.;
Dorosti Hasankiadeh, Q.; Dova, M. T.; Ebr, J.; Engel, R.; Erdmann, M.;
Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Facal San
Luis, P.; Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.; Fazzini,
N.; Ferguson, A. P.; Fernandes, M.; Fick, B.; Figueira, J. M.;
Filevich, A.; Filipčič, A.; Fox, B. D.; Fratu, O.; Fröhlich, U.;
Fuchs, B.; Fuji, T.; Gaior, R.; García, B.; Garcia Roca, S. T.;
Garcia-Gamez, D.; Garcia-Pinto, D.; Garilli, G.; Gascon Bravo, A.;
Gate, F.; Gemmeke, H.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.;
Giller, M.; Glaser, C.; Glass, H.; Gómez Berisso, M.; Gómez Vitale,
P. F.; Gonçalves, P.; Gonzalez, J. G.; González, N.; Gookin, B.;
Gordon, J.; Gorgi, A.; Gorham, P.; Gouffon, P.; Grebe, S.; Griffith,
N.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel,
M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Hartmann, S.; Harton,
J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Herve, A. E.;
Hill, G. C.; Hojvat, C.; Hollon, N.; Holt, E.; Homola, P.; Hörandel,
J. R.; Horvath, P.; Hrabovský, M.; Huber, D.; Huege, T.; Insolia,
A.; Isar, P. G.; Jandt, I.; Jansen, S.; Jarne, C.; Josebachuili, M.;
Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.;
Kégl, B.; Keilhauer, B.; Keivani, A.; Kemp, E.; Kieckhafer, R. M.;
Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm,
N.; Krömer, O.; Kruppke-Hansen, D.; Kuempel, D.; Kunka, N.; LaHurd,
D.; Latronico, L.; Lauer, R.; Lauscher, M.; Lautridou, P.; Le Coz,
S.; Leão, M. S. A. B.; Lebrun, D.; Lebrun, P.; Leigui de Oliveira,
M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; López, R.;
Lopez Agüera, A.; Louedec, K.; Lozano Bahilo, J.; Lu, L.; Lucero,
A.; Ludwig, M.; Malacari, M.; Maldera, S.; Mallamaci, M.; Maller, J.;
Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, V.; Mariş, I. C.;
Marsella, G.; Martello, D.; Martin, L.; Martinez, H.; Martínez Bravo,
O.; Martraire, D.; Masías Meza, J. J.; Mathes, H. J.; Mathys, S.;
Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Maurel, D.; Maurizio,
D.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Meissner,
R.; Melissas, M.; Melo, D.; Menshikov, A.; Messina, S.; Meyhandan,
R.; Mićanović, S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.;
Miramonti, L.; Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Monasor,
M.; Monnier Ragaigne, D.; Montanet, F.; Morello, C.; Mostafá, M.;
Moura, C. A.; Muller, M. A.; Müller, G.; Müller, S.; Münchmeyer,
M.; Mussa, R.; Navarra, G.; Navas, S.; Necesal, P.; Nellen, L.; Nelles,
A.; Neuser, J.; Nguyen, P.; Niechciol, M.; Niemietz, L.; Niggemann, T.;
Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.; Ochilo, L.; Olinto, A.;
Oliveira, M.; Pacheco, N.; Pakk Selmi-Dei, D.; Palatka, M.; Pallotta,
J.; Palmieri, N.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.;
Pech, M.; Pękala, J.; Pelayo, R.; Pepe, I. M.; Perrone, L.; Petermann,
E.; Peters, C.; Petrera, S.; Petrov, Y.; Phuntsok, J.; Piegaia, R.;
Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello, V.; Platino, M.;
Plum, M.; Porcelli, A.; Porowski, C.; Prado, R. R.; Privitera, P.;
Prouza, M.; Purrello, V.; Quel, E. J.; Querchfeld, S.; Quinn, S.;
Rautenberg, J.; Ravel, O.; Ravignani, D.; Revenu, B.; Ridky, J.;
Riggi, S.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho,
W.; Rodriguez Cabo, I.; Rodriguez Fernandez, G.; Rodriguez Rojo, J.;
Rodríguez-Frías, M. D.; Rogozin, D.; Ros, G.; Rosado, J.; Rossler,
T.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.; Saftoiu, A.;
Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.; Salina, G.;
Sánchez, F.; Sanchez-Lucas, P.; Santo, C. E.; Santos, E.; Santos,
E. M.; Sarazin, F.; Sarkar, B.; Sarmento, R.; Sato, R.; Scharf, N.;
Scherini, V.; Schieler, H.; Schiffer, P.; Schmidt, D.; Scholten, O.;
Schoorlemmer, H.; Schovánek, P.; Schulz, A.; Schulz, J.; Schumacher,
J.; Sciutto, S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard,
R. C.; Sidelnik, I.; Sigl, G.; Sima, O.; Śmiałkowski, A.; Šmída,
R.; Snow, G. R.; Sommers, P.; Sorokin, J.; Squartini, R.; Srivastava,
Y. N.; Stanič, S.; Stapleton, J.; Stasielak, J.; Stephan, M.; Stutz,
A.; Suarez, F.; Suomijärvi, T.; Supanitsky, A. D.; Sutherland, M. S.;
Swain, J.; Szadkowski, Z.; Szuba, M.; Taborda, O. A.; Tapia, A.;
Tartare, M.; Tepe, A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Toma, G.; Tomankova, L.; Tomé, B.; Tonachini, A.; Torralba
Elipe, G.; Torres Machado, D.; Travnicek, P.; Trovato, E.; Tueros,
M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño,
I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.; van
Velzen, S.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner,
G.; Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha,
J.; Videla, M.; Villaseñor, L.; Vlcek, B.; Vorobiov, S.; Wahlberg,
H.; Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weidenhaupt,
K.; Weindl, A.; Werner, F.; Widom, A.; Wiencke, L.; Wilczyńska, B.;
Wilczyński, H.; Will, M.; Williams, C.; Winchen, T.; Wittkowski,
D.; Wundheiler, B.; Wykes, S.; Yamamoto, T.; Yapici, T.; Yuan, G.;
Yushkov, A.; Zamorano, B.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zaw, I.; Zepeda, A.; Zhou, J.; Zhu, Y.; Zimbres Silva, M.; Ziolkowski,
M.; Zuccarello, F.; Pierre Auger Collaboration
2014PhRvD..90l2006A Altcode: 2014arXiv1409.5083P
Using the data taken at the Pierre Auger Observatory between December
2004 and December 2012, we have examined the implications of the
distributions of depths of atmospheric shower maximum (X<SUB>max</SUB>
), using a hybrid technique, for composition and hadronic interaction
models. We do this by fitting the distributions with predictions
from a variety of hadronic interaction models for variations in the
composition of the primary cosmic rays and examining the quality of
the fit. Regardless of what interaction model is assumed, we find that
our data are not well described by a mix of protons and iron nuclei
over most of the energy range. Acceptable fits can be obtained when
intermediate masses are included, and when this is done consistent
results for the proton and iron-nuclei contributions can be found
using the available models. We observe a strong energy dependence
of the resulting proton fractions, and find no support from any of
the models for a significant contribution from iron nuclei. However,
we also observe a significant disagreement between the models with
respect to the relative contributions of the intermediate components.
---------------------------------------------------------
Title: Dynamical behaviour of photospheric bright points during
merging
Authors: Criscuoli, S.; Stangalini, M.; Ermolli, I.; Zuccarello, F.;
Cristaldi, A.; Falco, M.; Guglielmino, S.; Giorgi, F.
2014AGUFMSH41C4152C Altcode:
We investigate the merging of bright points observed at high spatial
and temporal resolution with CRISP/SST in a quiet region region. We
analyze the MHD perturbations excited during the merging, their role
in the energy budget of the magnetic structure and the potential role
that they can play in heating the upper layers of the Sun's atmosphere.
---------------------------------------------------------
Title: Depth of maximum of air-shower profiles at the Pierre Auger
Observatory. I. Measurements at energies above 1 0<SUP>17.8</SUP> eV
Authors: Aab, A.; Abreu, P.; Aglietta, M.; Ahn, E. J.; Al Samarai, I.;
Albuquerque, I. F. M.; Allekotte, I.; Allen, J.; Allison, P.; Almela,
A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Alves Batista, R.;
Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Aramo, C.;
Aranda, V. M.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave,
M.; Avenier, M.; Avila, G.; Awal, N.; Badescu, A. M.; Barber, K. B.;
Bäuml, J.; Baus, C.; Beatty, J. J.; Becker, K. H.; Bellido, J. A.;
Berat, C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Billoir,
P.; Blaess, S.; Blanco, M.; Bleve, C.; Blümer, H.; Boháčová,
M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.; Brack, J.;
Brancus, I.; Bridgeman, A.; Brogueira, P.; Brown, W. C.; Buchholz, P.;
Bueno, A.; Buitink, S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga,
B.; Caccianiga, L.; Candusso, M.; Caramete, L.; Caruso, R.; Castellina,
A.; Cataldi, G.; Cazon, L.; Cester, R.; Chavez, A. G.; Chiavassa, A.;
Chinellato, J. A.; Chudoba, J.; Cilmo, M.; Clay, R. W.; Cocciolo, G.;
Colalillo, R.; Coleman, A.; Collica, L.; Coluccia, M. R.; Conceição,
R.; Contreras, F.; Cooper, M. J.; Cordier, A.; Coutu, S.; Covault,
C. E.; Cronin, J.; Curutiu, A.; Dallier, R.; Daniel, B.; Dasso, S.;
Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; De Domenico, M.;
de Jong, S. J.; de Mello Neto, J. R. T.; De Mitri, I.; de Oliveira,
J.; de Souza, V.; del Peral, L.; Deligny, O.; Dembinski, H.; Dhital,
N.; Di Giulio, C.; Di Matteo, A.; Diaz, J. C.; Díaz Castro, M. L.;
Diogo, F.; Dobrigkeit, C.; Docters, W.; D'Olivo, J. C.; Dorofeev, A.;
Dorosti Hasankiadeh, Q.; Dova, M. T.; Ebr, J.; Engel, R.; Erdmann, M.;
Erfani, M.; Escobar, C. O.; Espadanal, J.; Etchegoyen, A.; Facal San
Luis, P.; Falcke, H.; Fang, K.; Farrar, G.; Fauth, A. C.; Fazzini,
N.; Ferguson, A. P.; Fernandes, M.; Fick, B.; Figueira, J. M.;
Filevich, A.; Filipčič, A.; Fox, B. D.; Fratu, O.; Fröhlich, U.;
Fuchs, B.; Fujii, T.; Gaior, R.; García, B.; Garcia Roca, S. T.;
Garcia-Gamez, D.; Garcia-Pinto, D.; Garilli, G.; Gascon Bravo, A.;
Gate, F.; Gemmeke, H.; Ghia, P. L.; Giaccari, U.; Giammarchi, M.;
Giller, M.; Glaser, C.; Glass, H.; Gómez Berisso, M.; Gómez Vitale,
P. F.; Gonçalves, P.; Gonzalez, J. G.; González, N.; Gookin, B.;
Gordon, J.; Gorgi, A.; Gorham, P.; Gouffon, P.; Grebe, S.; Griffith,
N.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes, G. P.; Hampel,
M. R.; Hansen, P.; Harari, D.; Harrison, T. A.; Hartmann, S.; Harton,
J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann, P.; Herve, A. E.;
Hill, G. C.; Hojvat, C.; Hollon, N.; Holt, E.; Homola, P.; Hörandel,
J. R.; Horvath, P.; Hrabovský, M.; Huber, D.; Huege, T.; Insolia,
A.; Isar, P. G.; Jandt, I.; Jansen, S.; Jarne, C.; Josebachuili, M.;
Kääpä, A.; Kambeitz, O.; Kampert, K. H.; Kasper, P.; Katkov, I.;
Kégl, B.; Keilhauer, B.; Keivani, A.; Kemp, E.; Kieckhafer, R. M.;
Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm,
N.; Krömer, O.; Kruppke-Hansen, D.; Kuempel, D.; Kunka, N.; LaHurd,
D.; Latronico, L.; Lauer, R.; Lauscher, M.; Lautridou, P.; Le Coz,
S.; Leão, M. S. A. B.; Lebrun, D.; Lebrun, P.; Leigui de Oliveira,
M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; López, R.;
Lopez Agüera, A.; Louedec, K.; Lozano Bahilo, J.; Lu, L.; Lucero,
A.; Ludwig, M.; Malacari, M.; Maldera, S.; Mallamaci, M.; Maller, J.;
Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, V.; Mariş, I. C.;
Marsella, G.; Martello, D.; Martin, L.; Martinez, H.; Martínez Bravo,
O.; Martraire, D.; Masías Meza, J. J.; Mathes, H. J.; Mathys, S.;
Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Maurel, D.; Maurizio,
D.; Mayotte, E.; Mazur, P. O.; Medina, C.; Medina-Tanco, G.; Meissner,
R.; Melissas, M.; Melo, D.; Menshikov, A.; Messina, S.; Meyhandan,
R.; Mićanović, S.; Micheletti, M. I.; Middendorf, L.; Minaya, I. A.;
Miramonti, L.; Mitrica, B.; Molina-Bueno, L.; Mollerach, S.; Monasor,
M.; Monnier Ragaigne, D.; Montanet, F.; Morello, C.; Mostafá, M.;
Moura, C. A.; Muller, M. A.; Müller, G.; Müller, S.; Münchmeyer,
M.; Mussa, R.; Navarra, G.; Navas, S.; Necesal, P.; Nellen, L.; Nelles,
A.; Neuser, J.; Nguyen, P.; Niechciol, M.; Niemietz, L.; Niggemann, T.;
Nitz, D.; Nosek, D.; Novotny, V.; Nožka, L.; Ochilo, L.; Olinto, A.;
Oliveira, M.; Pacheco, N.; Pakk Selmi-Dei, D.; Palatka, M.; Pallotta,
J.; Palmieri, N.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.;
Pech, M.; Pękala, J.; Pelayo, R.; Pepe, I. M.; Perrone, L.; Petermann,
E.; Peters, C.; Petrera, S.; Petrov, Y.; Phuntsok, J.; Piegaia, R.;
Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello, V.; Platino, M.;
Plum, M.; Porcelli, A.; Porowski, C.; Prado, R. R.; Privitera, P.;
Prouza, M.; Purrello, V.; Quel, E. J.; Querchfeld, S.; Quinn, S.;
Rautenberg, J.; Ravel, O.; Ravignani, D.; Revenu, B.; Ridky, J.;
Riggi, S.; Risse, M.; Ristori, P.; Rizi, V.; Rodrigues de Carvalho,
W.; Rodriguez Cabo, I.; Rodriguez Fernandez, G.; Rodriguez Rojo, J.;
Rodríguez-Frías, M. D.; Rogozin, D.; Ros, G.; Rosado, J.; Rossler,
T.; Roth, M.; Roulet, E.; Rovero, A. C.; Saffi, S. J.; Saftoiu, A.;
Salamida, F.; Salazar, H.; Saleh, A.; Salesa Greus, F.; Salina, G.;
Sánchez, F.; Sanchez-Lucas, P.; Santo, C. E.; Santos, E.; Santos,
E. M.; Sarazin, F.; Sarkar, B.; Sarmento, R.; Sato, R.; Scharf, N.;
Scherini, V.; Schieler, H.; Schiffer, P.; Schmidt, D.; Scholten, O.;
Schoorlemmer, H.; Schovánek, P.; Schulz, A.; Schulz, J.; Schumacher,
J.; Sciutto, S. J.; Segreto, A.; Settimo, M.; Shadkam, A.; Shellard,
R. C.; Sidelnik, I.; Sigl, G.; Sima, O.; Śmiałkowski, A.; Šmída,
R.; Snow, G. R.; Sommers, P.; Sorokin, J.; Squartini, R.; Srivastava,
Y. N.; Stanič, S.; Stapleton, J.; Stasielak, J.; Stephan, M.; Stutz,
A.; Suarez, F.; Suomijärvi, T.; Supanitsky, A. D.; Sutherland, M. S.;
Swain, J.; Szadkowski, Z.; Szuba, M.; Taborda, O. A.; Tapia, A.;
Tartare, M.; Tepe, A.; Theodoro, V. M.; Timmermans, C.; Todero Peixoto,
C. J.; Toma, G.; Tomankova, L.; Tomé, B.; Tonachini, A.; Torralba
Elipe, G.; Torres Machado, D.; Travnicek, P.; Trovato, E.; Tueros,
M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño,
I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.; van
Velzen, S.; van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Varner,
G.; Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Verzi, V.; Vicha,
J.; Videla, M.; Villaseñor, L.; Vlcek, B.; Vorobiov, S.; Wahlberg,
H.; Wainberg, O.; Walz, D.; Watson, A. A.; Weber, M.; Weidenhaupt,
K.; Weindl, A.; Werner, F.; Widom, A.; Wiencke, L.; Wilczyńska, B.;
Wilczyński, H.; Will, M.; Williams, C.; Winchen, T.; Wittkowski,
D.; Wundheiler, B.; Wykes, S.; Yamamoto, T.; Yapici, T.; Yuan, G.;
Yushkov, A.; Zamorano, B.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zaw, I.; Zepeda, A.; Zhou, J.; Zhu, Y.; Zimbres Silva, M.; Ziolkowski,
M.; Zuccarello, F.; Pierre Auger Collaboration
2014PhRvD..90l2005A Altcode: 2014arXiv1409.4809P
We report a study of the distributions of the depth of maximum,
X<SUB>max</SUB>, of extensive air-shower profiles with energies
above 1 0<SUP>17.8</SUP> eV as observed with the fluorescence
telescopes of the Pierre Auger Observatory. The analysis method
for selecting a data sample with minimal sampling bias is described
in detail as well as the experimental cross-checks and systematic
uncertainties. Furthermore, we discuss the detector acceptance
and the resolution of the X<SUB>max</SUB> measurement and provide
parametrizations thereof as a function of energy. The energy dependence
of the mean and standard deviation of the X<SUB>max</SUB> distributions
are compared to air-shower simulations for different nuclear primaries
and interpreted in terms of the mean and variance of the logarithmic
mass distribution at the top of the atmosphere.
---------------------------------------------------------
Title: Erratum: "Observational Evidence of Torus Instability as
Trigger Mechanism for Coronal Mass Ejections: The 2011 August 4
Filament Eruption" <A href="/abs/2014ApJ...785...88Z">(2014, ApJ,
785, 88)</A>
Authors: Zuccarello, F. P.; Seaton, D. B.; Filippov, B.; Mierla, M.;
Poedts, S.; Rachmeler, L. A.; Romano, P.; Zuccarello, F.
2014ApJ...795..175Z Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Evolution of the Magnetic Helicity Flux during the Formation
and Eruption of Flux Ropes
Authors: Romano, P.; Zuccarello, F. P.; Guglielmino, S. L.;
Zuccarello, F.
2014ApJ...794..118R Altcode:
We describe the evolution and the magnetic helicity flux for two active
regions (ARs) since their appearance on the solar disk: NOAA 11318
and NOAA 11675. Both ARs hosted the formation and destabilization
of magnetic flux ropes. In the former AR, the formation of the flux
rope culminated in a flare of C2.3 GOES class and a coronal mass
ejection (CME) observed by Large Angle and Spectrometric Coronagraph
Experiment. In the latter AR, the region hosting the flux rope was
involved in several flares, but only a partial eruption with signatures
of a minor plasma outflow was observed. We found a different behavior in
the accumulation of the magnetic helicity flux in the corona, depending
on the magnetic configuration and on the location of the flux ropes
in the ARs. Our results suggest that the complexity and strength of
the photospheric magnetic field is only a partial indicator of the
real likelihood of an AR producing the eruption of a flux rope and a
subsequent CME.
---------------------------------------------------------
Title: Fractal and Multifractal Properties of Active Regions as Flare
Precursors: A Case Study Based on SOHO/MDI and SDO/HMI Observations
Authors: Ermolli, I.; Giorgi, F.; Romano, P.; Zuccarello, F.;
Criscuoli, S.; Stangalini, M.
2014SoPh..289.2525E Altcode: 2014SoPh..tmp...38E
Several studies indicate that fractal and multifractal parameters
inferred from solar photospheric magnetic field measurements may
help assessing the eruptive potential of Active Regions (ARs) and
also predicting their flare activity. We further investigate this
topic, by exploring the sensitivity of some parameters already
used in the literature on data and methods employed for their
estimation. In particular, we measured the generalized fractal
dimensions D<SUB>0</SUB> and D<SUB>8</SUB>, and the multifractal
parameters C<SUB>div</SUB> and D<SUB>div</SUB>, on the time series of
photospheric magnetograms of the flaring AR NOAA 11158 obtained with
the SOHO/MDI and SDO/HMI. The observations by the latter instrument are
characterized by a higher spatial and temporal resolution, as well as
higher flux sensitivity, than the ones obtained from SOHO/MDI, which
were widely employed in earlier studies. We found that the average
and peak values of complexity parameters measured on the two data sets
agree within measurement uncertainties. The temporal evolution of the
parameters measured on the two data sets show rather similar trends,
but the ones derived from the SOHO/MDI observations show larger and
spurious variations over time than those deduced from analysis of
the corresponding SDO/HMI data. We also found a larger sensitivity
of these measurements to characteristics of the data analyzed than
reported by earlier studies. In particular, analysis of the higher
resolution and higher cadence SDO/HMI data allows us also to detect
slight variations of the complexity indicators that cannot be derived
from the analysis of the SOHO/MDI data. These variations occur right
after the major events in the analyzed AR. They may be the signature
of photospheric effects of coronal magnetic field re-arrangement.
---------------------------------------------------------
Title: Dynamic Properties along the Neutral Line of a Delta Spot
Inferred from High-resolution Observations
Authors: Cristaldi, A.; Guglielmino, S. L.; Zuccarello, F.; Romano,
P.; Falco, M.; Rouppe van der Voort, L.; de la Cruz Rodríguez, J.;
Ermolli, I.; Criscuoli, S.
2014ApJ...789..162C Altcode:
Delta (δ) spots are complex magnetic configurations of sunspots
characterized by umbrae of opposite polarity sharing a common
penumbra. In order to investigate the fine structure of the region
separating the two magnetic polarities of a δ spot, we studied the
morphology, the magnetic configuration, and the velocity field in
such a region using observations of active region (AR) NOAA 11267
obtained with the CRisp Imaging SpectroPolarimeter (CRISP) at the
Swedish Solar Telescope on 2011 August 6. The analysis of CRISP data
shows upflows and downflows of ~ ± 3 km s<SUP>-1</SUP> in proximity
of the δ spot polarity inversion line (PIL), and horizontal motions
along the PIL of the order of ~1 km s<SUP>-1</SUP>. The results
obtained from the SIR inversion of CRISP data also indicate that the
transverse magnetic field in the brighter region separating the two
opposite magnetic polarities of the δ spot is tilted about ~45°
with respect to the PIL. Solar Dynamics Observatory/Helioseismic and
Magnetic Imager observations confirm the presence of motions of ~
± 3 km s<SUP>-1</SUP> in proximity of the PIL, which were observed
to last 15 hr. From the data analyzed, we conclude that the steady,
persistent, and subsonic motions observed along the δ spot PIL can be
interpreted as being due to Evershed flows occurring in the penumbral
filaments that show a curved, wrapped configuration. The fluting of
the penumbral filaments and their bending, continuously increased by
the approaching motion of the negative umbra toward the positive one,
give rise to the complex line-of-sight velocity maps that we observed.
---------------------------------------------------------
Title: F-CHROMA.Flare Chromospheres: Observations, Models and Archives
Authors: Cauzzi, Gianna; Fletcher, Lyndsay; Mathioudakis, Mihalis;
Carlsson, Mats; Heinzel, Petr; Berlicki, Arek; Zuccarello, Francesca
2014AAS...22412339C Altcode:
F-CHROMA is a collaborative project newly funded under the EU-Framework
Programme 7 "FP7-SPACE-2013-1", involving seven different European
research Institutes and Universities. The goal of F-CHROMA is to
substantially advance our understanding of the physics of energy
dissipation and radiation in the flaring solar atmosphere, with a
particular focus on the flares' chromosphere. A major outcome of the
F-CHROMA project will be the creation of an archive of chromospheric
flare observations and models to be made available to the community
for further research.In this poster we describe the structure and
milestones of the project, the different activities planned, as well
as early results. Emphasis will be given to the dissemination efforts
of the project to make results of these activities available to and
usable by the community.
---------------------------------------------------------
Title: Evolution and Dynamics of Orphan Penumbrae in the Solar
Photosphere: Analysis from Multi-instrument Observations
Authors: Zuccarello, Francesca; Guglielmino, Salvo L.; Romano, Paolo
2014ApJ...787...57Z Altcode:
We investigate the dynamics and magnetic properties of orphan penumbrae
observed in the solar photosphere to understand the formation process
of such structures. We observed two orphan penumbrae in active region
NOAA 11089 during a coordinated observing campaign carried out in 2010
July, involving the Hinode/Solar Optical Telescope (SOT) and Dutch
Open Telescope (DOT), benefiting also from continuous observations
acquired by the SDO satellite. We follow their evolution during about
three days. The two structures form in different ways: one seems to
break off the penumbra of a nearby sunspot, the other is formed through
the emergence of new flux. Then they fragment while evolving. The SDO
Helioseismic and Magnetic Imager measurements indicate the presence of
strong line-of-sight motions in the regions occupied by these orphan
penumbrae, lasting for several hours and decreasing with time. This
is confirmed by SOT spectro-polarimetric measurements of the Fe I
630.2 nm pair. The latter also show that Stokes parameters exhibit
significant asymmetries in the orphan penumbral regions, typical
of an uncombed filamentary structure. The orphan penumbrae lie above
polarity inversion lines, where peculiar plasma motions take place with
velocities larger than ±3 km s<SUP>-1</SUP>. The vector magnetic field
in these regions is highly inclined, with the average magnetic field
strength decreasing with time. The DOT observations in the Hα line
and SDO Atmospheric Imaging Assembly measurements in the He II 30.4
nm line indicate that there is no counterpart for the orphan penumbrae
at midchromospheric heights or above. Our findings suggest that in at
least one of the features investigated the emerging flux may be trapped
in the low atmospheric layers by the overlying pre-existing fields,
forming these filamentary structures.
---------------------------------------------------------
Title: Penumbral-like Filaments in the Solar Photosphere as a
Manifestation of Flux Emergence
Authors: Guglielmino, Salvo L.; Zuccarello, Francesca; Romano, Paolo
2014ApJ...786L..22G Altcode:
Rare observations of the solar photosphere show the appearance of orphan
penumbrae, filamentary structures very similar to a bundle of sunspot
penumbral filaments not connected to any umbra. Lim et al. found an
orphan penumbra in active region NOAA 11391 near a mature sunspot. We
analyze a different data set to study the same structure using the Solar
Optical Telescope on board the Hinode satellite. Spectropolarimetric
measurements along the Fe I 630.2 nm pair, complemented by G-band
and Ca II H filtergrams, show the evolution of this penumbral-like
structure and reveal that an emerging flux region is its ancestor. We
find new evidence for the interaction between the emerging flux and
the pre-existing field that leads to a brightening observed near the
base of the chromosphere. Our analysis suggests that as a result of
the combination of photospheric flux emergence and magneto-convection
in inclined fields the horizontal component of the emerging field
can be trapped in the photosphere by the overlying fields and form a
structure resembling penumbral filaments.
---------------------------------------------------------
Title: Observational Evidence of Torus Instability as Trigger
Mechanism for Coronal Mass Ejections: The 2011 August 4 Filament
Eruption
Authors: Zuccarello, F. P.; Seaton, D. B.; Mierla, M.; Poedts, S.;
Rachmeler, L. A.; Romano, P.; Zuccarello, F.
2014ApJ...785...88Z Altcode: 2014arXiv1401.5936Z
Solar filaments are magnetic structures often observed in the solar
atmosphere and consist of plasma that is cooler and denser than their
surroundings. They are visible for days—even weeks—which suggests
that they are often in equilibrium with their environment before
disappearing or erupting. Several eruption models have been proposed
that aim to reveal what mechanism causes (or triggers) these solar
eruptions. Validating these models through observations represents a
fundamental step in our understanding of solar eruptions. We present
an analysis of the observation of a filament eruption that agrees with
the torus instability model. This model predicts that a magnetic flux
rope embedded in an ambient field undergoes an eruption when the axis of
the flux rope reaches a critical height that depends on the topology of
the ambient field. We use the two vantage points of the Solar Dynamics
Observatory (SDO) and the Solar TErrestrial RElations Observatory to
reconstruct the three-dimensional shape of the filament, to follow
its morphological evolution, and to determine its height just before
eruption. The magnetograms acquired by SDO/Helioseismic and Magnetic
Imager are used to infer the topology of the ambient field and to derive
the critical height for the onset of the torus instability. Our analysis
shows that the torus instability is the trigger of the eruption. We also
find that some pre-eruptive processes, such as magnetic reconnection
during the observed flares and flux cancellation at the neutral line,
facilitated the eruption by bringing the filament to a region where
the magnetic field was more vulnerable to the torus instability.
---------------------------------------------------------
Title: Evolution of the Magnetic Field Inclination in a Forming
Penumbra
Authors: Romano, P.; Guglielmino, S. L.; Cristaldi, A.; Ermolli, I.;
Falco, M.; Zuccarello, F.
2014ApJ...784...10R Altcode:
We describe the evolution of the magnetic and velocity fields in the
annular zone around a pore a few hours before the formation of its
penumbra. We detected the presence of several patches at the edge of
the annular zone, with a typical size of about 1”. These patches are
characterized by a rather vertical magnetic field with polarity opposite
to that of the pore. They correspond to regions of plasma upflow up
to 2.5 km s<SUP>-1</SUP> and are characterized by radially outward
displacements with horizontal velocities up to 2 km s<SUP>-1</SUP>. We
interpret these features as portions of the pore magnetic field lines
returning beneath the photosphere being progressively stretched and
pushed down by the overlying magnetic fields. Our results confirm
that the penumbra formation results from changes in the inclination
of the field lines in the magnetic canopy overlying the pore, until
they reach the photosphere.
---------------------------------------------------------
Title: Penumbral-like Structures in the Solar Photosphere: the Role
of Flux Emergence
Authors: Zuccarello, Francesca; Romano, Paolo; Cristaldi, Alice;
Falco, Mariachiara; Guglielmino, Salvo L.
2014cosp...40E3864Z Altcode:
Observations of the solar photosphere rarely show the appearance of
so-called orphan penumbrae, filamentary structures very similar to
a bundle of sunspot penumbral filaments, but not connected to any
umbra. We report on the plasma flows and on the magnetic properties
of such structures observed in different active regions using the
Solar Optical Telescope on board the Hinode satellite. We also benefit
from continuous observations acquired by the SDO satellite and from
some high-resolution data acquired by the DOT telescope. We find that
these structures can form in different ways: one seems to break off the
penumbra of a nearby sunspot, others are formed through the emergence
of new flux. Our analysis suggests that, for these latter features,
the horizontal component of the emerging field can be trapped in the
photosphere by the overlying fields and form a structure resembling
penumbral filaments due to the combination of photospheric flux
emergence and magneto-convection in inclined fields.
---------------------------------------------------------
Title: Shearing motions and torus instability in the 2010 April 3
filament eruption
Authors: Zuccarello, F. P.; Romano, P.; Zuccarello, F.; Poedts, S.
2014IAUS..300..475Z Altcode:
The magnetic field evolution of active region NOAA 11059 is studied
in order to determine the possible causes and mechanisms that led to
the initiation of the 2010 April 3 coronal mass ejection (CME). <P
/>We find (1) that the magnetic configuration of the active region
is unstable to the torus instability and (2) that persistent shearing
motions characterized the negative polarity, resulting in a southward,
almost parallel to the meridians, drift motion of the negative magnetic
field concentrations. <P />We conclude that these shearing motions
increased the axial field of the filament eventually bringing the
flux rope axis to a height where the onset condition for the torus
instability was satisfied.
---------------------------------------------------------
Title: Velocity and Magnetic Field Distribution in a Forming Penumbra
Authors: Romano, P.; Frasca, D.; Guglielmino, S. L.; Ermolli, I.;
Tritschler, A.; Reardon, K. P.; Zuccarello, F.
2013ApJ...771L...3R Altcode:
We present results from the analysis of high-resolution
spectropolarimetric and spectroscopic observations of the solar
photosphere and chromosphere, obtained shortly before the formation of a
penumbra in one of the leading polarity sunspots of NOAA active region
11490. The observations were performed at the Dunn Solar Telescope of
the National Solar Observatory on 2012 May 28, using the Interferometric
Bidimensional Spectrometer. The data set is comprised of a 1 hr time
sequence of measurements in the Fe I 617.3 nm and Fe I 630.25 nm lines
(full Stokes polarimetry) and in the Ca II 854.2 nm line (Stokes I
only). We perform an inversion of the Fe I 630.25 nm Stokes profiles to
derive magnetic field parameters and the line-of-sight (LOS) velocity
at the photospheric level. We characterize chromospheric LOS velocities
by the Doppler shift of the centroid of the Ca II 854.2 nm line. We
find that, before the formation of the penumbra, an annular zone of
3”-5” width is visible around the sunspot. In the photosphere, we
find that this zone is characterized by an uncombed structure of the
magnetic field although no visible penumbra has formed yet. We also
find that the chromospheric LOS velocity field shows several elongated
structures characterized by downflow and upflow motions in the inner
and outer parts of the annular zone, respectively.
---------------------------------------------------------
Title: A new approach to model particle acceleration and energy
transfer in solar flares
Authors: Rubio Da Costa, Fatima; Zuccarello, F.; Fletcher, L.;
Labrosse, N.; Kasparova, J.; Prosecký, T.; Carlsson, M.; Petrosian,
V.; Liu, W.
2013SPD....4440401R Altcode:
Motivated by available observations of two different flares in Lyα and
Hα, we model the conditions of the solar atmosphere using a radiation
hydrodynamics code (RADYN, Carlsson & Stein, 1992) and analyze the
energy transport carried by a beam of non-thermal electrons injected
at the top of a 1D coronal loop. The numerical Lyα and Hα intensities
match with the observations. The electron energy distribution is assumed
to follow a power law of the form (E/E<SUP>c</SUP> )<SUB>-δ</SUB> for
energies greater than a cutoff value of E<SUP>c</SUP>. Abbett &
Hawley (1999) and Allred et al. (2005) assumed that the non-thermal
electrons flux injected at the top of a flaring loop, the cut-off energy
and the power law index are constant over time. An improvement was
achieved by Allred & Hawley (2006), who modified the RADYN code
in such a way that the input parameters were time dependent. Their
inputs were based on observations of a flare obtained with RHESSI. By
combining RADYN with the “flare” code from Stanford University
which models the acceleration and transport of particles and radiation
of solar flares in non-LTE regime, we can calculate the non-thermal
electrons flux, the cut-off energy and the power law index at every
simulated time step. The atmospheric parameters calculated by RADYN
could in turn be used as updated inputs for "flare", providing several
advantages over the results from Liu et al. (2009), who combined the
particle acceleration code with a 1-D hydrodynamic code, improving
the atmospheric conditions.
---------------------------------------------------------
Title: Solar activity and its evolution across the corona: recent
advances
Authors: Zuccarello, Francesca; Balmaceda, Laura; Cessateur, Gael;
Cremades, Hebe; Guglielmino, Salvatore L.; Lilensten, Jean; Dudok
de Wit, Thierry; Kretzschmar, Matthieu; Lopez, Fernando M.; Mierla,
Marilena; Parenti, Susanna; Pomoell, Jens; Romano, Paolo; Rodriguez,
Luciano; Srivastava, Nandita; Vainio, Rami; West, Matt; Zuccarello,
Francesco P.
2013JSWSC...3A..18Z Altcode:
Solar magnetism is responsible for the several active phenomena that
occur in the solar atmosphere. The consequences of these phenomena on
the solar-terrestrial environment and on Space Weather are nowadays
clearly recognized, even if not yet fully understood. In order to shed
light on the mechanisms that are at the basis of the Space Weather,
it is necessary to investigate the sequence of phenomena starting in
the solar atmosphere and developing across the outer layers of the Sun
and along the path from the Sun to the Earth. This goal can be reached
by a combined multi-disciplinary, multi-instrument, multi-wavelength
study of these phenomena, starting with the very first manifestation
of solar active region formation and evolution, followed by explosive
phenomena (i.e., flares, erupting prominences, coronal mass ejections),
and ending with the interaction of plasma magnetized clouds expelled
from the Sun with the interplanetary magnetic field and medium. This
wide field of research constitutes one of the main aims of COST Action
ES0803: Developing Space Weather products and services in Europe. In
particular, one of the tasks of this COST Action was to investigate
the Progress in Scientific Understanding of Space Weather. In this
paper we review the state of the art of our comprehension of some
phenomena that, in the scenario outlined above, might have a role on
Space Weather, focusing on the researches, thematic reviews, and main
results obtained during the COST Action ES0803.
---------------------------------------------------------
Title: From solar physics to astrophysics: the Sun as Rosetta stone
for understanding astrophysical processes & The Sun: new tools
and ideas in observational solar astrophysics: European week of
Astronomy and Space Science
Authors: Berrilli, F.; Ermolli, I.; Zuccarello, F.
2013MmSAI..84..281B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Small-scale brightenings observed in active regions with SST
and Hinode
Authors: Cristaldi, A.; Guglielmino, S. L.; Zuccarello, F.; Ermolli,
I.; Falco, M.; Criscuoli, S.
2013MmSAI..84..339C Altcode:
Ca II H brightenings are good proxies of transient phenomena occurring
in the solar chromosphere. We analyze temporal series of Ca II H
filtergrams taken with SST at extreme high resolution (0.15 arcsec)
at different line positions, simultaneously with spectropolarimetric
data in the Fe I pair at 630.2 nm and Hinode/SOT data, to study the
interactions between flux systems. Ca II H core brightenings have
been observed in areas surrounding the sunspot penumbra, following
their evolution.
---------------------------------------------------------
Title: Spatial distribution of the magnetic helicity flux measured
with SDO/HMI in active regions hosting flares and CMEs
Authors: Romano, P.; Zuccarello, F.
2013MmSAI..84..363R Altcode:
The study of the accumulation of magnetic helicity via emergence of new
magnetic flux and/or shearing photospheric motions is considered an
important tool for understanding the processes that lead to eruptive
phenomena. In a previous work we measured the amount of magnetic
helicity injected into the corona through the photosphere in a sample of
active regions (ARs) by inferring the apparent motion of photospheric
footpoints of magnetic field lines from a time series of MDI full-disk
line-of-sight magnetograms \citep{Rom11}. The temporal variation
of the maps of magnetic helicity flux was analysed by measuring
the fragmentation of the patches characterized by different flux of
magnetic helicity. The more fragmented were the maps of the magnetic
helicity flux, the higher was the flare and coronal mass ejection (CME)
frequency. In order to further investigate the correlation between the
number of these patches and the flare and the CME occurrence, another
sample of ARs observed with a higher spatial resolution by SDO/HMI has
been analyzed. The new results indicate that not only the accumulation
of magnetic helicity in the corona, but also its positive and negative
fragmentation and distribution should be taken into account to provide
a more confident indication of AR complexity and flare/CME productivity.
---------------------------------------------------------
Title: An orphan penumbra observed with Hinode and DOT
Authors: Zuccarello, F.; Guglielmino, S. L.
2013MmSAI..84..375Z Altcode:
Orphan penumbrae are filamentary structures, very similar to the
penumbral filaments, but that are not adjacent to any sunspot
umbra. We observed an orphan penumbra in NOAA 11089 during a
coordinated observational campaign, involving the Hinode/SOT and
DOT telescopes. The spectropolarimetric measurements indicate the
presence of both significant upflows and downflows in the orphan
penumbra region, that decrease in time. A neutral line is present in
the region, with a strong horizontal component of the vector magnetic
field. We investigate the association of such structure with other
features in the low chromosphere.
---------------------------------------------------------
Title: Sunspot evolution observed with SST.
Authors: Falco, M.; Zuccarello, F.; Criscuoli, S.; Cristaldi, A.;
Guglielmino, S. L.; Ermolli, I.
2013MmSAI..84..345F Altcode:
We report on the evolution of an active region NOAA 11263 observed
with SST at extreme high spatial resolution (0.15 arcsec). We analyzed
spectral and spectropolarimetric data acquired at Fe I 557.6 nm and
630.2 nm spectral ranges, respectively, to study the magnetic field
properties and the dynamics of the plasma in the umbral and penumbral
region of the sunspot. Interestingly, images acquired in photospheric
continuum show twisting motions of the penumbral filaments. Moreover,
we investigate if MMFs are present during the evolution of the
sunspot. Brightenings in Ca II H line are also noticed, indicating
the occurrence of transient phenomena in the chromosphere.
---------------------------------------------------------
Title: Spectro-polarimetric Observations of Moving Magnetic Features
around a Pore
Authors: Zuccarello, F.; Berrilli, F.; Criscuoli, S.; Del Moro, D.;
Ermolli, I.; Giannattasio, F.; Giorgi, F.; Romano, P.; Viticchiè, B.
2012ASPC..463...51Z Altcode:
Moving Magnetic Features (MMFs) are small-size magnetic elements that
are seen to stream-out from sunspots. Although several observations
suggest that MMFs are closely related to the existence and presence
of penumbral filaments, there are some very few observations that
report MMFs streaming from pores and sunspots after the penumbra has
disappeared. Here we report on the first high spectral, spatial and
temporal resolution observations of type II and III MMFs streaming out
from a small pore and compare our results with previous observations of
features streaming out from penumbrae. We analyzed spectro-polarimetric
observations of NOAA 11005 acquired with the IBIS instrument at
the Dunn Solar Telescope in the Fe I 617.3 nm and the Ca II 854.2 nm
spectral lines, and in the G-band. We show that the characteristics of
the investigated MMFs agree with those reported in the literature for
MMFs which stream out from spots with penumbrae. We believe that our
results provide new information that might be helpful in the future
development and upgrade of numerical modeling of the generation of
MMFs in the lack of a penumbra.
---------------------------------------------------------
Title: The role of streamers in the deflection of coronal mass
ejections: comparison between STEREO 3D reconstructions and numerical
simulations
Authors: Zuccarello, F. P.; Bemporad, A.; Jacobs, C.; Mierla, M.;
Poedts, S.; Zuccarello, F.
2012AGUFMSH31A2200Z Altcode:
On 2009 September 21, a filament eruption and the associated Coronal
Mass Ejection (CME) was observed by the %coronographs on board of the
STEREO spacecraft. The CME originated from the southern hemisphere and
showed a deflection of about 15<SUP>o</SUP> towards the heliospheric
current sheet (HCS) during the propagation in the COR1 field-of-view
(FOV). The CME source region was near the central meridian, but no
on-disk CME signatures could be seen from the Earth. The aim of this
paper is to provide a physical explanation for the strong deflection
of the CME observed on 2009 September 21. The two-sided view of the
STEREO spacecraft allows us to reconstruct the three dimensional (3D)
travel path of the CME and the evolution of the CME source region. The
observations are combined with a magnetohydrodynamic (MHD) simulation,
starting from a magnetic field configuration closely resembling the
extrapolated potential field for that date. %The amount of helicity
injected in the coronal volume is similar in both the observation
and the simulation. By applying localized shearing motions, a CME is
initiated in the simulation, showing a similar non-radial evolution,
structure, and velocity as the observed event. The CME gets deflected
towards the current sheet of the larger northern helmet streamer, due
to an imbalance in the magnetic pressure and tension forces and finally
it gets into the streamer. This study shows that during solar minima,
even CMEs originating from high latitude can be easily deflected towards
the heliospheric current sheet, eventually resulting in geoeffective
events. How rapidly they undergo this latitudinal migration depends
on the strength of both the large scale coronal magnetic field and
the magnetic flux of the erupting filament.
---------------------------------------------------------
Title: IBIS: High-Resolution Multi-Height Observations and Magnetic
Field Retrieval
Authors: Del Moro, D. .; Berrilli, F.; Stangalini, M.; Giannattasio,
F.; Piazzesi, R.; Giovannelli, L.; Viticchiè, B.; Vantaggiato, M.;
Sobotka, M.; Jurčák, J.; Criscuoli, S.; Giorgi, F.; Zuccarello, F.
2012ASPC..463...33D Altcode:
IBIS (Interferometric BIdimensional Spectrometer) allows us to measure
the four Stokes parameters in several spectroscopic lines with high
spatial and spectral resolutions. With this information, we can
retrieve both the dynamics and the magnetic field at different layers
of the Photosphere and Chromosphere. The high spectral, spatial and
temporal resolutions and the polarimetric sensitivity of IBIS allows
us to study different phenomena taking place in the solar atmosphere
with new tools. As an example, we highlight some applications of
IBIS observations and analysis: <BR /> · Radiative and dynamical
properties of Photospheric Bright Points versus their magnetic field
concentration. <BR /> · Close up analysis of magnetic, velocity and
temperature field in a solar pore. <BR /> · MHD wave propagation from
the photosphere to the chromosphere in complex magnetic configuration.
---------------------------------------------------------
Title: Numerical modeling of the initiation of coronal mass ejections
in active region NOAA 9415
Authors: Zuccarello, F. P.; Meliani, Z.; Poedts, S.
2012AGUFMSH33E..02Z Altcode:
Coronal mass ejections (CMEs) and solar flares are the main drivers of
the space weather. Understanding how these events can occur and what
conditions might lead to eruptive events is of crucial relevance for up
to date and reliable space weather forecasting. The aim of the present
paper is to present a numerical magnetohydrodynamic (MHD) data-driven
model suitable for the simulation of the CME initiation and their early
evolution. Starting from a potential magnetic field extrapolation of
the active region (AR) NOAA 9415, we solve the full set of ideal MHD
equations in a non-zero plasma-β environment. We investigate the
response of the solar corona when photospheric motions, resembling
the ones observed for AR 9415, are applied at the inner boundary. As
a consequence of the applied twisting motions a force-free magnetic
field configuration, having the same chirality as the investigated
active region, is obtained. As a response to the converging shearing
motions a flux rope is formed that quickly propagates outwards,
carrying away, against the gravitational attraction by the Sun,
the plasma confined inside the flux rope. Moreover, a compressed
leading edge propagating at a speed of about 550 km s<SUP>-1</SUP>
and preceding the CME is formed. The presented simulation shows that
both the initial magnetic field configuration and the plasma-magnetic
field interaction are relevant for a more comprehensive understanding
of the CME initiation and early evolution phenomenon.
---------------------------------------------------------
Title: Study of Multiple Coronal Mass Ejections at Solar Minimum
Conditions
Authors: Bemporad, A.; Zuccarello, F. P.; Jacobs, C.; Mierla, M.;
Poedts, S.
2012SoPh..281..223B Altcode: 2012SoPh..tmp..153B
The aim of this work is to provide a physical explanation for the
genesis of multiple coronal mass ejections (CMEs) in an asymmetric
coronal field configuration. We analyze STEREO observations of a
multiple eruption and compare the results from the data analysis with
predictions provided by magnetohydrodynamic (MHD) simulations. To this
end, the multiple CMEs (MCMEs) observed on 21 - 22 September 2009 were
selected. Both eruptions originated from the same source region and
showed approximately the same latitudinal deflection, by more than
15 degrees, toward the heliospheric current sheet (HCS) during their
propagation in the COR1 field of view. Numerical MHD simulations of
the MCMEs have been performed, starting from an asymmetric coronal
field configuration that mimics the potential field source surface
extrapolation for 21 September 2009. The results demonstrate that,
by shearing the footpoints at the base of the southern arcade,
we were able to reproduce the observed dynamics of the MCMEs. Both
CMEs are deflected toward the HCS due to an imbalance in the magnetic
pressure and tension forces; the global field strength turns out to
be a crucial parameter in order to release two subsequent eruptions,
and hence to reproduce the observed evolution.
---------------------------------------------------------
Title: High cadence spectropolarimetry of moving magnetic features
observed around a pore
Authors: Criscuoli, S.; Del Moro, D.; Giannattasio, F.; Viticchié,
B.; Giorgi, F.; Ermolli, I.; Zuccarello, F.; Berrilli, F.
2012A&A...546A..26C Altcode: 2012arXiv1208.2039C
Context. Moving magnetic features (MMFs) are small-size magnetic
elements that are seen to stream out from sunspots, generally during
their decay phase. Several observational results presented in the
literature suggest them to be closely related to magnetic filaments
that extend from the penumbra of the parent spot. Nevertheless,
few observations of MMFs streaming out from spots without penumbra
have been reported. The literature still lacks analyses of the
physical properties of these features. <BR /> Aims: We investigate
physical properties of monopolar MMFs observed around a small pore
that had developed penumbra in the days preceding our observations
and compare our results with those reported in the literature for
features observed around sunspots. <BR /> Methods: We analyzed NOAA
11005 during its decay phase with data acquired at the Dunn Solar
Telescope in the Fe i 617.3 nm and the Ca ii 854.2 nm spectral lines
with IBIS, and in the G-band. The field of view showed monopolar
MMFs of both polarities streaming out from the leading negative
polarity pore of the observed active region. Combining different
analyses of the data, we investigated the temporal evolution of the
relevant physical quantities associated with the MMFs as well as the
photospheric and chromospheric signatures of these features. <BR />
Results: We show that the characteristics of the investigated MMFs
agree with those reported in the literature for MMFs that stream out
from spots with penumbrae. Moreover, observations of at least two of the
observed features suggest them to be manifestations of emerging magnetic
arches. <P />Appendices A and B, and a movie are available in electronic
form at <A href="http://www.aanda.org">http://www.aanda.org</A>
---------------------------------------------------------
Title: A Comparative Analysis of Photospheric Bright Points in an
Active Region and in the Quiet Sun
Authors: Romano, P.; Berrilli, F.; Criscuoli, S.; Del Moro, D.;
Ermolli, I.; Giorgi, F.; Viticchié, B.; Zuccarello, F.
2012SoPh..280..407R Altcode: 2012SoPh..tmp...26R
We present a comparative study of photometric and dynamic properties
of photospheric bright points (BPs) observed at the disk centre in
the active region (AR) NOAA 10912 and in the quiet Sun. We found that
the average concentration of BPs is 54% larger in the AR than in the
quiet Sun. We also measure a decrease of the BP concentration and an
increase of their size moving away from the AR centre. However, these
variations can be ascribed to the variation of the spatial resolution
and image quality in the field of view of the AR dataset. We also found
that BPs in the quiet Sun are associated with larger downflow motions
than those measured within the AR. Finally, from our measurements of
contrast and velocity along the line of sight, we deduced that BPs
are less bright in high magnetic flux density regions than in quiet
regions, due to a lower efficiency of convection in the former regions.
---------------------------------------------------------
Title: Numerical Modeling of the Initiation of Coronal Mass Ejections
in Active Region NOAA 9415
Authors: Zuccarello, F. P.; Meliani, Z.; Poedts, S.
2012ApJ...758..117Z Altcode:
Coronal mass ejections (CMEs) and solar flares are the main drivers
of weather in space. Understanding how these events occur and what
conditions might lead to eruptive events is of crucial importance
for up to date and reliable space weather forecasting. The aim
of this paper is to present a numerical magnetohydrodynamic (MHD)
data-inspired model suitable for the simulation of the CME initiation
and their early evolution. Starting from a potential magnetic field
extrapolation of the active region (AR) NOAA 9415, we solve the full
set of ideal MHD equations in a non-zero plasma-β environment. As a
consequence of the applied twisting motions, a force-free-magnetic
field configuration is obtained, which has the same chirality as
the investigated AR. We investigate the response of the solar corona
when photospheric motions resembling the ones observed for AR 9415 are
applied at the inner boundary. As a response to the converging shearing
motions, a flux rope is formed that quickly propagates outward, carrying
away the plasma confined inside the flux rope against the gravitational
attraction by the Sun. Moreover, a compressed leading edge propagating
at a speed of about 550 km s<SUP>-1</SUP> and preceding the CME is
formed. The presented simulation shows that both the initial magnetic
field configuration and the plasma-magnetic-field interaction are
relevant for a more comprehensive understanding of the CME initiation
and early evolution phenomenon.
---------------------------------------------------------
Title: The role of streamers in the deflection of coronal mass
ejections
Authors: Zuccarello, F. P.; Bemporad, A.; Jacobs, C.; Mierla, M.;
Poedts, S.; Zuccarello, F.
2012IAUS..286..134Z Altcode:
On 2009 September 21, a filament eruption and the associated Coronal
Mass Ejection (CME) was observed by the STEREO spacecraft. The CME
originated from the southern hemisphere and showed a deflection of about
15° towards the heliospheric current sheet (HCS) during its propagation
in the COR1 field-of-view (FOV). The aim of this paper is to provide a
physical explanation for the strong deflection of the CME. We first use
the STEREO observations in order to reconstruct the three dimensional
(3D) trajectory of the CME. Starting from a magnetic configuration that
closely resembles the potential field extrapolation for that date, we
performed numerical magneto-hydrodynamics (MHD) simulations. By applying
localized shearing motions, a CME is initiated in the simulation,
showing a similar non-radial evolution, structure, and velocity as the
observed event. The CME gets deflected towards the current sheet of the
larger northern helmet streamer, due to an imbalance in the magnetic
pressure and tension forces and finally it gets into the streamer and
propagates along the heliospheric current sheet.
---------------------------------------------------------
Title: Physical properties of Moving Magnetic Features observed
around a pore
Authors: Criscuoli, S.; Del Moro, D.; Giannattasio, F.; Viticchié,
B.; Giorgi, F.; Ermolli, I.; Zuccarello, F.; Berrilli, F.
2012EAS....55...87C Altcode:
Movies of magnetograms of sunspots often show small-size magnetic
patches that move radially away and seem to be expelled from the
field of the spot. These patches are named Moving Magnetic Features
(MMFs). They have been mostly observed around spots and have been
interpreted as manifestations of penumbral filaments. Nevertheless,
few observations of MMFS streaming out from spots without penumbra
have been reported. He we investigate the physical properties of MMFs
observed around the field of a pore derived by the analyses of high
spectral, spatial and temporal resolution data acquired at the Dunn
Solar Telescope with IBIS. We find that the main properties of the
investigated features agree with those reported for MMFs observed
around regular spots. These results indicate that an improvement of
current numerical simulations is required to understand the generation
of MMFs in the lack of penumbrae.
---------------------------------------------------------
Title: The role of filament activation in a solar eruption
Authors: Rubio da Costa, F.; Zuccarello, F.; Fletcher, L.; Romano,
P.; Labrosse, N.
2012A&A...539A..27R Altcode: 2014arXiv1412.1858R
Context. Observations show that the mutual relationship between
filament eruptions and solar flares cannot be described in terms of an
unique scenario. In some cases, the eruption of a filament appears to
trigger a flare, while in others the observations are more consistent
with magnetic reconnection that produces both the flare observational
signatures (e.g., ribbons, plasma jets, post-flare loops, etc.) and
later the destabilization and eruption of a filament. <BR /> Aims:
Contributing to a better comprehension of the role played by filament
eruptions in solar flares, we study an event which occurred in NOAA
8471, where a flare and the activation of (at least) two filaments
were observed on 28 February 1999. <BR /> Methods: By using imaging
data acquired in the 1216, 1600, 171 and 195 Å TRACE channels and by
BBSO in the continnum and in the Hα line, a morphological study of
the event is carried out. Moreover, using TRACE 1216 and 1600 Å data,
an estimate of the "pure" Lyα power is obtained. The extrapolation of
the magnetic field lines is done using the SOHO/MDI magnetograms and
assuming a potential field. <BR /> Results: Initially an area hosting a
filament located over a δ spot becomes brighter than the surroundings,
both in the chromosphere and in the corona. This area increases in
brightness and extension, eventually assuming a two-ribbon morphology,
until it reaches the eastern part of the active region. Here a second
filament becomes activated and the brightening propagates to the south,
passing over a large supergranular cell. The potential magnetic field
extrapolation indicates that the field line connectivity changes
after the flare. <BR /> Conclusions: The event is triggered by the
destabilization of a filament located between the two polarities
of a δ spot. This destabilization involves the magnetic arcades
of the active region and causes the eruption of a second filament,
that gives rise to a CME and to plasma motions over a supergranular
cell. We conclude that in this event the two filaments play an active
and decisive role, albeit in different stages of the phenomenon,
in fact the destabilization of one filament causes brightenings,
reconnection and ribbons, while the second one, whose eruption is caused
by the field reconfiguration resulting from the previous reconnection,
undergoes the greatest changes and causes the CME.
---------------------------------------------------------
Title: A Broad Band Imager for the European Solar Telescope
Authors: Munari, M.; Scuderi, S.; Cecconi, M.; Zuccarello, F.
2012MSAIS..19..101M Altcode:
The European Solar Telescope (EST) is a joint project of several
European research institutes to design and realize a 4-m class solar
telescope. The EST Broad Band Imager is one of the baseline instruments
of EST. It will obtain diffraction limited images over the full field of
view of EST at multiple wavelengths and high frame rate. Its scientific
objectives are the study of fundamental astrophysical processes at
their intrinsic scales in the Sun's atmosphere. Here we report on the
current optical design of the instrument.
---------------------------------------------------------
Title: The European Solar Telescope: project status .
Authors: Zuccarello, F.; EST Team
2012MSAIS..19...67Z Altcode:
The European Solar Telescope (EST) project foresees the realization of
a 4 - meter solar telescope, characterized by an optical design and by a
suite of instruments optimized for spectropolarimetric measurements from
near infrared to near UV. The aperture, the site at the Canary Islands,
the adaptive optics and the multi conjugate adaptive optics for extended
sources integrated along the optical path, the set of instruments and
the post facto image processing techniques, will allow us to study
the interaction between the plasma and the magnetic field in the solar
atmosphere at resolutions comparable to the photon mean free path in
the photosphere. EST will be operational contemporarily to major ESA
and NASA space missions for the study of the Sun and of its activity.
---------------------------------------------------------
Title: The role of photospheric shearing motions in a filament
eruption related to the 2010 April 3 coronal mass ejection
Authors: Zuccarello, F. P.; Romano, P.; Zuccarello, F.; Poedts, S.
2012A&A...537A..28Z Altcode:
Context. Coronal mass ejections (CMEs) are huge expulsion of solar
plasma and magnetic field in the interplanetary medium. Understanding
the physics that lies beyond the CME initiation is one of the most
fascinating research questions. Several models have been proposed
to explain the initiation of CMEs. However, which model better
explains the different aspects of the initiation process and the
early evolution of the CMEs is a subject of ongoing discussion. <BR
/> Aims: We investigate the magnetic field evolution of NOAA 11059
in order to provide a further contribution to our understanding of
the possible causes and mechanisms that lead to the initiation of
the geoeffective CME that occurred on 2010 April 3. <BR /> Methods:
Using KSO Hα images we determine the chirality of the active region
and some properties of the filament that eventually erupted. Using
SOHO/MDI line-of-sight magnetograms we investigate the magnetic
configuration of NOAA 11059 by means of both linear force free and
potential field extrapolations. We also determine the photospheric
velocity maps using the Differential Affine Velocity Estimator
(DAVE). <BR /> Results: We find that the magnetic configuration of
the active region is unstable to the torus instability. Moreover,
we find that persistent shearing motions characterized the negative
polarity, resulting in a southward, almost parallel to the meridians,
drift motion of the negative magnetic field concentrations. <BR />
Conclusions: We conclude that persistent and coherent shearing motions
played a significant role in facilitating the eruption. These shearing
motions increased the axial field of the filament eventually bringing
the fluxrope axis to a height where the onset condition for the torus
instability was satisfied. Our observations show that both the magnetic
configuration of the system and the photopsheric dynamics that preceded
the event, were favourable for the eruption to occur.
---------------------------------------------------------
Title: Relationship between an M6.6 solar flare and subsequent
filament activations.
Authors: Rubio da Costa, F.; Zuccarello, F.; Romano, P.; Fletcher,
L.; Labrosse, N.
2012MSAIS..19..113R Altcode:
We study an event which occurred in NOAA 8471, where an M6.6 flare
and the activation of two filaments were observed on 28 February
1999. A multi-wavelength study allows us to investigate the behavior
of the several features observed at different atmospheric levels, that
might be used to answer to the question whether and in what conditions
the eruption of filaments can play an active or a passive role in the
flare occurrence. Imaging data were acquired by BBSO in the Halpha line
and by TRACE in the 1216, 1600, 171 and 195 Å channels, allowing us
to deduce the morphology and temporal evolution of the event and to
estimate the Ly-alpha power. Moreover, in order to study the magnetic
topology, the extrapolation of the photospheric magnetic field lines
was done assuming potential field and using SOHO/MDI magnetograms.
---------------------------------------------------------
Title: The Role of Streamers in the Deflection of Coronal Mass
Ejections: Comparison between STEREO Three-dimensional Reconstructions
and Numerical Simulations
Authors: Zuccarello, F. P.; Bemporad, A.; Jacobs, C.; Mierla, M.;
Poedts, S.; Zuccarello, F.
2012ApJ...744...66Z Altcode:
On 2009 September 21, a filament eruption and the associated
coronal mass ejection (CME) were observed by the Solar Terrestrial
Relations Observatory (STEREO) spacecraft. The CME originated from the
southern hemisphere and showed a deflection of about 15° toward the
heliospheric current sheet (HCS) during the propagation in the COR1
field of view. The CME source region was near the central meridian,
but no on-disk CME signatures could be seen from the Earth. The aim
of this paper is to provide a physical explanation for the strong
deflection of the CME observed on 2009 September 21. The two-sided view
of the STEREO spacecraft allows us to reconstruct the three-dimensional
travel path of the CME and the evolution of the CME source region. The
observations are combined with a magnetohydrodynamic simulation,
starting from a magnetic field configuration closely resembling the
extrapolated potential field for that date. By applying localized
shearing motions, a CME is initiated in the simulation, showing a
similar non-radial evolution, structure, and velocity as the observed
event. The CME gets deflected toward the current sheet of the larger
northern helmet streamer due to an imbalance in the magnetic pressure
and tension forces and finally gets into the streamer. This study shows
that during solar minima, even CMEs originating from high latitude can
be easily deflected toward the HCS, eventually resulting in geoeffective
events. How rapidly they undergo this latitudinal migration depends
on the strength of both the large-scale coronal magnetic field and
the magnetic flux of the erupting filament.
---------------------------------------------------------
Title: Solar flares in Halpha and Ly-alpha : observations vs
simulations.
Authors: Rubio da Costa, F.; Zuccarello, F.; Fletcher, L.; Labrosse,
N.; Prosecký, T.; Kašparová, J.
2012MSAIS..19..117R Altcode:
In order to study the properties of faint, moderate and bright flares,
we simulate the conditions of the solar atmosphere using a radiative
hydrodynamic model \citep{2005ApJ...630..573A}. A constant beam of
non-thermal electrons is injected at the apex of a 1D coronal loop
and heating from thermal soft X-ray and UV emission is included. We
study the contribution of different processes to the total intensity of
different lines at different atmospheric layers. We obtain the total
integrated intensity of different lines and we compare those of the
Ly-alpha and Halpha lines with the observational values for Ly-alpha
(using TRACE 1216 and 1600 Å data and estimating the “pure” Ly-alpha
emission) and Halpha (using data from the Ondřejov Observatory). We
inferred from the analysis of the values obtained by simulation that
the X-ray energy of the different kind of flares does not strongly
affect the Ly-alpha results; the Halpha results are comparable to the
observed ones, concluding that the simulated solar atmosphere fits
better at lower layers of the chromosphere than at upper layers.
---------------------------------------------------------
Title: Properties of G-band Bright Points derived from IBIS
observations
Authors: Criscuoli, S.; Del Moro, D.; Giorgi, F.; Romano, P.; Berrilli,
F.; Ermolli, I.; Viticchié, B.; Zuccarello, F.
2012MSAIS..19...93C Altcode: 2010arXiv1011.4890C
We have investigated properties of photospheric Bright Points (BPs)
observed in an Active Region during its decay phase and in a quiet Sun
region. We have analyzed two sets of photospheric observations taken
with IBIS (Interferometric Bidimensioal Spectrometer) at the NSO Dunn
Solar Telescope. The first set consists of spectral data acquired in the
Fe I 709.0 nm and Ca I 854.2 nm lines and simultaneous broad-band and
of G-band observations. The second set consists of spectro-polarimetric
observations in the Fe I 630.15 nm - 630.25 nm doublet and simultaneous
white light and G-band observations. <P />The relation between BP
filling factor and RMS image contrast indicates that, on average,
BPs cover up to 3% of the solar surface outside Active Regions. The
relation between area and intensity values of the features identified
on both data sets suggests that they are composed of aggregations of
magnetic flux elements. The horizontal velocity values are as high
as 2 km/s, thus supporting the scenario of BPs motion contributing to
the coronal heating.
---------------------------------------------------------
Title: High-resolution Observations of Siphon Flows in a Solar
Magnetic Pore
Authors: Guglielmino, Salvo L.; Zuccarello, Francesca
2011ApJ...743L...9G Altcode:
We investigate signatures of siphon flows in a region around a solar
magnetic pore, observed in the photosphere at μ = 0.6, during its
decay phase. We analyze high-resolution Stokes spectra acquired by
Hinode/Solar Optical Telescope along the Fe I pair at 630.2 nm. We
determine the vector magnetic field and the line-of-sight velocity
by an inversion of the full Stokes vector using the SIR code. We
also analyze photospheric G-band filtergrams. We find evidence of a
transient siphon (counter)flow at the edge of the pore. An arch-shaped
structure is found to have upflow motions of 4 km s<SUP>-1</SUP> in
the footpoint with a stronger magnetic field and positive polarity,
and downflows of the same order of magnitude in the footpoint with
opposite polarity and a weaker magnetic field. The event is different
from those reported in previous observations of the Sun's atmosphere
and may represent a physical constraint for numerical models.
---------------------------------------------------------
Title: Flare occurrence and the spatial distribution of the magnetic
helicity flux
Authors: Romano, P.; Zuccarello, F.
2011A&A...535A...1R Altcode:
Context. The accumulation of magnetic helicity via emergence of new
magnetic flux and/or shearing photospheric motions is considered an
important tool for understanding the processes that lead to eruptive
phenomena. <BR /> Aims: We highlight a specific aspect of the magnetic
helicity accumulation, providing new observational evidence of the
role played by the interaction of magnetic field systems that are
characterized by opposite signs of the magnetic helicity flux in
triggering solar eruptions. <BR /> Methods: The amount of magnetic
helicity injected into the corona through the photosphere in a sample
of active regions (ARs) during their passage across the solar disk was
measured by inferring the apparent motion of photospheric footpoints of
magnetic field lines from a time series of MDI full-disk line-of-sight
magnetograms. The temporal variation of the maps of magnetic helicity
flux was analysed by measuring the fragmentation of the patches that
are characterized by the flux of magnetic helicity. The temporal
correlation between the number of these patches and the flare and
coronal mass ejection (CME) occurrence has also been studied. <BR />
Results: The fragmentation of the patches singled out in the maps
of the magnetic helicity flux provides a useful indication of the
evolution of the AR complexity. The more fragmented the maps of
the magnetic helicity flux are, the higher is the flare and CME
frequency. Moreover, most of the events occur for low values (~3 ÷
17) of the difference of the number of patches with opposite signs
of magnetic helicity flux. <BR /> Conclusions: These results indicate
that not only the accumulation of magnetic helicity in the corona, but
also its positive and negative fragmentation and distribution should
be taken into account to provide a more confident indication of AR
complexity and flare/CME productivity. In particular, the interaction
of magnetic systems characterized by opposite sign of magnetic helicity
flux may be responsible for many observed eruptions.
---------------------------------------------------------
Title: Solar observations carried out at the INAF - Catania
Astrophysical Observatory
Authors: Zuccarello, F.; Contarino, L.; Romano, P.
2011CoSka..41...85Z Altcode:
Solar observations at the INAF - Catania Astrophysical Observatory
are carried out by means of an equatorial spar, which includes: a
Cook refractor, used to make daily drawings of sunspot groups from
visual observations; a 150-mm refractor with an Hα Lyot filter for
chromospheric observations; a 150-mm refractor feeding an Hα Halle
filter for limb observations of the chromosphere. The photospheric
and chromospheric data are daily distributed to several international
Solar Data Centers. Recently, a program of Flare Warning has been
implemented, with the aim of determining the probability that an active
region yields a flare on the basis of its characteristics deduced
from optical observations. Some science results obtained by means of
solar data acquired at the INAF - Catania Astrophysical Observatory,
as well as by space-instruments data, are briefly described.
---------------------------------------------------------
Title: Filament destabilization and CME release during a long
duration flare
Authors: Zuccarello, F.; Contarino, L.; Farnik, F.; Karlicky, M.;
Romano, P.; Ugarte-Urra, I.
2011A&A...533A.100Z Altcode:
Context. During complex and long duration solar flares, several filament
destabilizations or eruptions can occur that are often related to
coronal mass ejections (CMEs). <BR /> Aims: We describe the study of
an X3.8 long duration event (LDE) that occurred in NOAA 10720 on 17
January 2005 and was characterized by three filament destabilizations
and two CMEs. <BR /> Methods: Using multi-wavelength data provided
by both ground-based instruments and satellites, in addition to MDI
magnetograms, we investigated the morphological and magnetic evolution
of the active region before and during the LDE. <BR /> Results: Our
analysis of H<SUB>α</SUB> and 1600 Å images showed that initially a
two-ribbon structure developed in the central part of the active region,
where a filament was previously observed. At a later time, two bright
ribbons (in the most eastern side) and a strong brightness increase
(at the western outskirt of the active region) were simultaneously
observed. In a subsequent time interval, a new pair of ribbons was
observed in the western side of the active region. Moreover, a linear
force-free field extrapolation helped identify a null point in the
central part of the active region. <BR /> Conclusions: The initial
filament destabilization that occurred in the central part of NOAA
10720 was probably due to magnetic flux emergence and photospheric
shearing motions, which caused a slow tether-cutting process beneath
the filament. The rearrangement of the magnetic field configuration,
occurring in the same area as the location of the null point, changed
the magnetic field connectivity in the active region, triggering two
filament eruptions in the eastern and western part of the active region
and two halo CMEs, in a kind of domino effect.
---------------------------------------------------------
Title: CME evolution and 3D reconstruction with STEREO Data
Authors: Orlando, A.; Zuccarello, F.; Romano, P.; Zuccarello, F. P.;
Mierla, M.; Spadaro, D.; Ventura, R.
2011IAUS..274..165O Altcode:
We describe a CME event, occurred in NOAA 11059 on April 3 2010,
using STEREO and MDI/SOHO data. We analyze the CME evolution using
data provided by SECCHI-EUVI and COR1 onboard STEREO satellites,
and we perform a 3D reconstruction of the CME using the LCT-TP
method. Using MDI/SOHO line-of-sight magnetograms we analyze the
magnetic configuration of NOAA 11059 and we determine the magnetic
helicity trend.
---------------------------------------------------------
Title: Solar flares: observations vs simulations
Authors: Rubio da Costa, Fatima; Zuccarello, Francesca; Labrosse,
Nicolas; Fletcher, Lyndsay; Prosecký, Tomáš; Kašparová, Jana
2011IAUS..274..182R Altcode:
In order to study the properties of faint, moderate and bright flares,
we simulate the conditions of the solar atmosphere using a radiative
hydrodynamic model (Abbett & Hawley, 1999). A constant beam of
non-thermal electrons is injected at the apex of a 1D coronal loop and
heating from thermal soft X-ray emission is included. We compare the
results with some observational data in Ly-α (using TRACE 1216 and
1600 Å data and estimating the “pure” Ly-α emission) and in Hα
(data taken with a Multichannel Flare Spectrograph, at the Ondrejov
Observatory).
---------------------------------------------------------
Title: Small-scale flux emergence events observed by Sunrise/IMaX
Authors: Guglielmino, S. L.; Pillet, V. Martínez; del Toro Iniesta,
J. C.; Rubio, L. R. Bellot; Zuccarello, F.; Solanki, S. K.; Solanki
2011IAUS..274..140G Altcode:
Thanks to the unprecedented combination of high spatial resolution
(0”.2) and high temporal cadence (33 s) spectropolarimetric
measurements, the IMaX magnetograph aboard the Sunrise balloon-borne
telescope is revealing new insights about the plasma dynamics
of the all-pervasive small-scale flux concentrations in the quiet
Sun. We present the result of a case study concerning the appearance
of a bipole, with a size of about 4” and a flux content of 5 ×
10<SUP>17</SUP> Mx, with strong signal of horizontal fields during
the emergence. We analyze the data set using the SIR inversion code
and obtain indications about the three-dimensional shape of the bipole
and its evolution with time.
---------------------------------------------------------
Title: The EST project
Authors: Zuccarello, Francesca; Zuccarello
2011IAUS..274..310Z Altcode:
EST European Solar Telescope is a pan-european project, presently
in its Conceptual Design Study financed by the European Commission
in the framework of FP7, involving 29 partners, from 14 different
countries. The EST project is aimed at the realization of a 4-m class
telescope, characterized by an optical design and a set of instruments
optimized for extremely high resolution imaging and spectropolarimetric
observations from near UV to NIR. EST will be four times larger than
any existing high resolution solar telescope and it is designated with
the highest priority among the ground-based, medium term (2016-2020)
new projects in the ASTRONET Roadmap (Panel C). The EST instruments
will measure fundamental astrophysical processes at their intrinsic
scales in the Sun's atmosphere to establish the mechanism of magnetic
field generation and removal, and of energy transfer from the surface to
the upper solar atmosphere and eventually to the whole heliosphere. The
conceptual Design Study started on February 2008 and will finish during
2011. EST will be operational at the same time as major ESA and NASA
space missions aimed at studying solar activity.
---------------------------------------------------------
Title: Magnetic helicity evolution inside a hexagonal convective cell
Authors: Smyrli, Aimilia; Mackay, Duncan; Zuccarello, Francesca
2011IAUS..274..192S Altcode:
Magnetic helicity has received considerable attention in the area of
fluid dynamics. Recently, this quantity is attracting the interest
of solar physicists and much research has been carried out related
to magnetic helicity generation and transport through different solar
layers, starting from the interior and the convection zone, towards the
photosphere, the corona and finally into the heliosphere. Taking into
account the global importance of supergranular cells in convection
theories, we study the motion of magnetic features into such a
geometrical element simplified as hexagonal cell and we analyse the
results in terms of the accumulated magnetic helicity. We compute the
emergence of a bipole inside the hexagonal cell and its motion from
the centre of the cell towards its sides and its vertices, where the
magnetic elements are considered to be sinking down. Multiple bipoles
are also considered and phenomena such as cancellation, coalescence and
fragmentation are also investigated. We find that the most important
process for the accumulation of magnetic helicity is the shear motion
between the polarities. The magnetic helicity accumulation changes
its trend when one polarity reaches the side of the hexagon, and later
the vertex. It has zero value when there is no shear motion inside the
hexagonal cell, and it is constant when there is no shear between the
two polarities during their motion along the cell sides.
---------------------------------------------------------
Title: Magnetic helicity balance during a filament eruption that
occurred in active region NOAA 9682
Authors: Zuccarello, F. P.; Romano, P.; Zuccarello, F.; Poedts, S.
2011A&A...530A..36Z Altcode:
Context. Photospheric shear plasma flows in active regions may be
responsible for the magnetic helicity injection in the solar corona not
only during the energy storage process before a solar eruption, but also
during and after the release of the free magnetic energy caused by the
eruption. Indeed, after a filament eruption or expansion the magnetic
torque imbalance can induce shear flows that can be responsible for yet
another injection of magnetic helicity into the corona. <BR /> Aims:
We investigated the magnetic helicity balance in an active region
where a confined solar eruption occurred. This was done to verify a
possible relationship between the filament expansion and the helicity
transport at its footpoints. We aimed to verify if this variation in
the helicity transport rate could be interpreted as a consequence of
the magnetic torque imbalance caused by the tube expansion, as proposed
by Chae et al. (2003, J. Kor. Astron. Soc., 36, 33). <BR /> Methods:
We used 171ÅTRACE data to measure some geometrical parameters of
the new magnetic system produced by a filament eruption that occurred
on 2001 November 1 in active region NOAA 9682. We used MDI full disk
line-of-sight magnetogram data to measure the accumulation of magnetic
helicity in the corona before and after the event. <BR /> Results:
From the measured expansion factor in the magnetic arcade, visible
at 171 Åduring the eruption, we estimated that the resulting torque
imbalance at the photosphere ought to lead to the injection of negative
helicity following the eruption. We compared this with measurements
of the helicity injection using photospheric velocity and magnetogram
data. <BR /> Conclusions: In contradiction to the expectations from
the Chae et al. model, the helicity injection after the eruption was
positive. We offer the alternative interpretation that the helicity
injection resulted from torque of the opposite sign, generated as the
filament lost its negative helicity through magnetic reconnection with
its surroundings.
---------------------------------------------------------
Title: Evolution of Small-scale Magnetic Features Streaming-out from
a Pore
Authors: Criscuoli, S.; Del Moro, D.; Romano, P.; Berrilli, F.;
Ermolli, I. : Giorgi, F.; Vitichhié, B.; Zuccarello, F.
2011ASPC..437..493C Altcode:
We present results from observations of Moving Magnetic Features
(MMFs) of different types observed on region NOAA 11005. The analyses
is based on spectro-polarimetric data obtained with the Interferometric
Bidimensional Spectrometer (IBIS) at various spectral ranges. We present
new evidences of bipolar MMFs observed to stream out from pores and
show the temporal evolution of magnetic, dynamic and morphological
properties of these features.
---------------------------------------------------------
Title: Magnetic reconnection signatures in the solar atmosphere:
results from multi-wavelength observations
Authors: Zuccarello, F.; Guglielmino, S. L.; Romano, P.
2011MmSAI..82..149Z Altcode:
In the solar atmosphere magnetic reconnection is invoked as the
main mechanism causing very energetic events (10<SUP>28</SUP>
- 10<SUP>32</SUP> erg), like flares and coronal mass ejections,
as well as other less energetic phenomena, like microflares, X-ray
jets and chromospheric surges. In the last decade, thanks to high
spatial resolution, multi-wavelength observations carried out by
both ground-based telescopes (THEMIS, SST, VTT, DST) and space-born
satellites (SOHO, TRACE, RHESSI, HINODE), it has been possible to study
these phenomena and several signatures of the occurrence of magnetic
reconnection have been singled out. In this paper, we describe some
results obtained from the analysis of multi-wavelength observations
carried out in the last years, with special emphasis on those events
that were characterized by plasma outflows from the reconnection
site. The events here discussed are relevant to some active regions
observed on the Sun, characterized by the interaction of different
bundles of magnetic flux tubes, as a consequence of phenomena of
emergence of new magnetic flux from the subphotospheric layers and/or
of cancellation of magnetic fragments. We report on these phenomena in
order to give a contribution to the possibility to find a similarity
with jets observed in AGNs.
---------------------------------------------------------
Title: A solar eruption triggered by the interaction between two
magnetic flux systems with opposite magnetic helicity
Authors: Romano, P.; Pariat, E.; Sicari, M.; Zuccarello, F.
2011A&A...525A..13R Altcode:
Context. In recent years the accumulation of magnetic helicity via
emergence of new magnetic flux and/or shearing photospheric motions
has been considered to play an important role in the destabilization
processes that lead to eruptive phenomena occurring in the solar
atmosphere. <BR /> Aims: In this paper we want to highlight a specific
aspect of magnetic helicity accumulation, providing new observational
evidence of the role played by the interaction of magnetic fields
characterized by opposite magnetic helicity signs in triggering solar
eruption. <BR /> Methods: We used 171 Å TRACE data to describe a
filament eruption on 2001 Nov. 1 in active region NOAA 9682 and MDI full
disk line-of-sight magnetograms to measure the accumulation of magnetic
helicity in corona before the event. We used the local correlation
tracking (LCT) and the differential affine velocity estimator (DAVE)
techniques to determine the horizontal velocities and two methods for
estimating the magnetic helicity flux. <BR /> Results: The chirality
signatures of the filament involved in the eruption were ambiguous,
and the overlying arcade visible during the main phase of the event
was characterized by a mixing of helicity signs. However, the measures
of the magnetic helicity flux allowed us to deduce that the magnetic
helicity was positive in the whole active region where the event
took place, while it was negative near the magnetic inversion line
where the filament footpoints were located. <BR /> Conclusions: These
results suggest that the filament eruption may be caused by magnetic
reconnection between two magnetic field systems characterized by
opposite signs of magnetic helicity. We also find that only the DAVE
method allowed us to obtain the crucial information on the horizontal
velocity field near the magnetic inversion line.
---------------------------------------------------------
Title: Trend of photospheric magnetic helicity flux in active regions
generating halo CMEs
Authors: Zuccarello, F. P.; Smyrli, A.; Romano, P.; Poedts, S.
2010AGUFMSH43B1817Z Altcode:
Coronal Mass Ejections (CMEs) are very energetic events initiated
in the solar atmosphere, resulting in the expulsion of magnetized
plasma clouds that propagate into interplanetary space. It has been
proposed that CMEs can play an important role in shedding magnetic
helicity, avoiding its endless accumulation in the corona. We therefore
investigated the behavior of magnetic helicity accumulation in sites
where the initiation of CMEs occurred, in order to determine whether and
how changes in magnetic helicity accumulation are temporally correlated
with CME occurrence. After identifying the active regions (AR) where
the CMEs were initiated by means of a double cross-check based on the
flaring-eruptive activity and the use of SOHO/EIT difference images,
we use MDI magnetograms to calculate magnetic flux evolution magnetic,
helicity injection rate and magnetic helicity injection in 10 active
regions that gave rise to 12 halo CMEs observed during the period
February 2000 - June 2003. No unique behavior in magnetic helicity
injection accompanying halo CME occurrence is found. In fact, in
some cases there is an abrupt change in helicity injection timely
correlated with the CME event, while in some others no significant
variation is recorded. However, our analysis show that the most
significant changes in magnetic flux and magnetic helicity injection
are associated with impulsive CMEs rather than gradual CMEs. Moreover,
the most significant changes in magnetic helicity are observed when
X-class flares or eruptive filaments occur, while the occurrence of
flares of class C or M seems not to affect significantly the magnetic
helicity accumulation. Finally, this study shows that magnetic
helicity accumulation in our sample of ARs generating halo CMEs has
sudden and abrupt changes only in 40 % of the cases examined and that
a correlation between the helicity injection changes and the nature
(gradual or impulsive) of the CMEs seems to exist.
---------------------------------------------------------
Title: Multiwavelength Observations of Small-scale Reconnection
Events Triggered by Magnetic Flux Emergence in the Solar Atmosphere
Authors: Guglielmino, S. L.; Bellot Rubio, L. R.; Zuccarello, F.;
Aulanier, G.; Vargas Domínguez, S.; Kamio, S.
2010ApJ...724.1083G Altcode: 2010arXiv1007.4657G
The interaction between emerging magnetic flux and the pre-existing
ambient field has become a "hot" topic for both numerical simulations
and high-resolution observations of the solar atmosphere. The appearance
of brightenings and surges during episodes of flux emergence is believed
to be a signature of magnetic reconnection processes. We present an
analysis of a small-scale flux emergence event in NOAA 10971, observed
simultaneously with the Swedish 1 m Solar Telescope on La Palma and the
Hinode satellite during a joint campaign in 2007 September. Extremely
high-resolution G-band, Hα, and Ca II H filtergrams, Fe I and Na
I magnetograms, EUV raster scans, and X-ray images show that the
emerging region was associated with chromospheric, transition region
and coronal brightenings, as well as with chromospheric surges. We
suggest that these features were caused by magnetic reconnection
at low altitude in the atmosphere. To support this idea, we perform
potential and linear force-free field extrapolations using the FROMAGE
service. The extrapolations show that the emergence site is cospatial
with a three-dimensional null point, from which a spine originates. This
magnetic configuration and the overall orientation of the field lines
above the emerging flux region are compatible with the structures
observed in the different atmospheric layers and remain stable against
variations of the force-free field parameter. Our analysis supports
the predictions of recent three-dimensional numerical simulations that
energetic phenomena may result from the interaction between emerging
flux and the pre-existing chromospheric and coronal field.
---------------------------------------------------------
Title: Trend of photospheric magnetic helicity flux in active regions
generating halo coronal mass ejections
Authors: Smyrli, A.; Zuccarello, F.; Romano, P.; Zuccarello, F. P.;
Guglielmino, S. L.; Spadaro, D.; Hood, A. W.; Mackay, D.
2010A&A...521A..56S Altcode:
Context. Coronal mass ejections (CMEs) are very energetic events (~
10<SUP>32</SUP> erg) initiated in the solar atmosphere, resulting
in the expulsion of magnetized plasma clouds that propagate into
interplanetary space. It has been proposed that CMEs can play an
important role in shedding magnetic helicity, avoiding its endless
accumulation in the corona. <BR /> Aims: The aim of this work is to
investigate the behavior of magnetic helicity accumulation in sites
where the initiation of CMEs occurred to determine whether and how
changes in magnetic helicity accumulation are temporally correlated
with CME occurrence. <BR /> Methods: We used MDI/SOHO line-of-sight
magnetograms to calculate magnetic flux evolution and magnetic
helicity injection in 10 active regions that gave rise to halo CMEs
observed during the period 2000 February to 2003 June. <BR /> Results:
The magnetic helicity injection does not have a unique trend in the
events analyzed: in 40% of the cases it shows a large sudden and abrupt
change that is temporally correlated with a CME occurrence, while in
the other cases it shows a steady monotonic trend, with a slight change
in magnetic helicity at CME occurrence. <BR /> Conclusions: The results
obtained from the sample of events that we have analyzed indicate that
major changes in magnetic helicity flux are observed in active regions
characterized by emergence of new magnetic flux and/or generating halo
CMEs associated with X-class flares or filament eruptions. In some of
the analyzed cases the changes in magnetic helicity flux follow the
CME events and can be attributed to a process of restoring a torque
balance between the subphotospheric and the coronal domain of the
flux tubes. <P />Appendix is only available in electronic form at <A
href="http://www.aanda.org">http://www.aanda.org</A>
---------------------------------------------------------
Title: The X3.8 flare in NOAA 10720 : a new example of the domino
effect
Authors: Farnik, Frantisek; Contarino, L.; Romano, P.; Zuccarello,
F.; Karlicky, M.
2010shin.confE..16F Altcode:
We have studied an X3.8 flare occurred in NOAA 10720 on 17 January 2005
using chromospheric and photospheric images acquired at INAF - Catania
Astrophysical Observatory, TRACE images acquired at 1600 ?, full disk
MDI magnetograms, RHESSI hard X-ray data and Ondrejov radio data, in
order to investigate the morphological and magnetic evolution of the
active region before and during the flare. The analysis of H-alpha and
1600 ? images showed that initially a two-ribbon structure developed
in the central part of the active region, later two bright ribbons
(in the most eastern side) and a strong brightness increase (at the
western boundary of the active region) were observed contemporarily. In
the following time interval a new pair of ribbons was observed in
the central-western side of the region. The analysis of the magnetic
configuration and the location of a null point allowed us to single
out the sites where magnetic reconnection processes were most likely
to occur. Based on this result and on the analysis of H-alpha, TRACE,
RHESSI and Ondrejov data, we interpreted this behavior as due to an
initial filament eruption that occurred in the central part of NOAA
10720, where the null point was located, and later on, as in a domino
effect, other filament destabilization or eruption took place in the
eastern and western part of the active region.
---------------------------------------------------------
Title: The ADAHELI solar mission: Investigating the structure of
Sun's lower atmosphere
Authors: Berrilli, F.; Bigazzi, A.; Roselli, L.; Sabatini, P.; Velli,
M.; Alimenti, F.; Cavallini, F.; Greco, V.; Moretti, P. F.; Orsini,
S.; Romoli, M.; White, S. M.; ADAHELI Team; Ascani, L.; Carbone, V.;
Curti, F.; Consolini, G.; Di Mauro, M. P.; Del Moro, D.; Egidi, A.;
Ermolli, I.; Giordano, S.; Pastena, M.; Pulcino, V.; Pietropaolo, E.;
Romano, P.; Ventura, P.; Cauzzi, G.; Valdettaro, L.; Zuccarello, F.;
ADAHELI Team
2010AdSpR..45.1191B Altcode: 2010AdSpR..45.1191A
ADAHELI (ADvanced Astronomy for HELIophysics) is a small-class
(500 kg) low-budget (50 MEuro) satellite mission for the study of
the solar photosphere and the chromosphere and for monitoring solar
flare emission. ADAHELI's design has completed its Phase-A feasibility
study in December 2008, in the framework of ASI's (Agenzia Spaziale
Italiana) 2007 "Small Missions" Program (calling for two missions at
50 MEeuros each, plus the launch budget). ADAHELI's main purpose is
to explore Sun's lower atmosphere in the near-infrared, a region so
far unexplored by solar observations from space. ADAHELI will carry
out observations of the solar photosphere and of the chromosphere at
high-temporal rate and high spatial and spectral resolutions. ADAHELI
will contribute to the understanding of Space Weather through the
study of particle acceleration during flares. A radiometer operating
in the millimeter radio band will continuously monitor the solar disk,
throughout the spacecraft's life time. ADAHELI's baseline instruments
are a 50-cm high-resolution telescope operating in the visible and
the near-infrared, and a lightweight full-disk radiometer operating at
millimeter wavelengths (90 GHz). The core of the telescope's focal plane
suite is the spectral imager based on two Fabry-Perot interferometers,
flying for the first time on a solar mission. The instrument
will return fast-cadence, full bi-dimensional spectral images at
high-resolution, thus improving on current slit-scan, mono-dimensional
architectures. Moreover, the possibility of working in polarized light
will enable full 3D magnetic field reconstruction on the photosphere
and the chromosphere. An optional instrumental package is also being
proposed to further extend ADAHELI's scope: a full-disk telescope for
helioseismology based on a double Magneto-Optical Filter, a Neutral
Particle Analyzer for magnetospheric research, an Extreme Ultraviolet
imaging and spectro-radiometry instrument. These options fall outside
the prescribed budget. ADAHELI, flying a Sun-Synchronous orbit at 800
km, will perform continuous, long-duration (4-h), daily acquisitions,
with the possibility of extending them up to 24 h. ADAHELI's operating
life is two years, plus one extension year. Launch would be nominally
planned for 2014.
---------------------------------------------------------
Title: The Italian contribution to the design study of the European
Solar Telescope EST: current status and future steps
Authors: Zuccarello, F.; EST Team
2010MSAIS..14..238Z Altcode:
The EST (European Solar Telescope) is a 4-m class telescope, four
times larger than any existing high resolution solar telescope. It is
designated with the highest priority among the ground-based, medium term
(2016-2020) new projects in the ASTRONET Roadmap (Panel C). The EST will
be equipped with a suite of instruments to perform spectropolarimetric
and imaging observations at high spatial and temporal resolution in the
range UV-NIR. The conceptual design study, which has been funded from
EU in the framework of FP7, started on February 2008. We summarize the
Italian participation to the EST project, which includes detailed design
of various subsystems affecting the opto-mechanical structure, the suite
of post-focus instruments, the data handling, and the control system.
---------------------------------------------------------
Title: Trend of photospheric helicity flux in active regions
generating halo CMEs
Authors: Smyrli, Aimilia; Zuccarello, Francesco; Zuccarello, Francesca;
Romano, Paolo; Guglielmino, Salvatore Luigi; Spadaro, Daniele; Hood,
Alan; Mackay, Duncan
2010cosp...38.1860S Altcode: 2010cosp.meet.1860S
Coronal Mass Ejections (CMEs) are very energetic events initiated
in the solar atmosphere, re-sulting in the expulsion of magnetized
plasma clouds that propagate into interplanetary space. It has been
proposed that CMEs can play an important role in shedding magnetic
helicity, avoiding its endless accumulation in the corona. We therefore
investigated the behavior of magnetic helicity accumulation in sites
where the initiation of CMEs occurred, in order to de-termine whether
and how changes in magnetic helicity accumulation are temporally
correlated with CME occurrence. After identifying the active
regions (AR) where the CMEs were ini-tiated by means of a double
cross-check based on the flaring-eruptive activity and the use of
SOHO/EIT difference images, we used MDI magnetograms to calculate
magnetic flux evolu-tion, magnetic helicity injection rate and
magnetic helicity injection in 10 active regions that gave rise to
12 halo CMEs observed during the period February 2000 -June 2003. No
unique behavior in magnetic helicity injection accompanying halo CME
occurrence is found. In fact, in some cases there is an abrupt change
in helicity injection timely correlated with the CME event, while
in some others no significant variation is recorded. However, our
analysis show that the most significant changes in magnetic flux and
magnetic helicity injection are associated with impulsive CMEs rather
than gradual CMEs. Moreover, the most significant changes in mag-netic
helicity are observed when X-class flares or eruptive filaments occur,
while the occurrence of flares of class C or M seems not to affect
significantly the magnetic helicity accumulation.
---------------------------------------------------------
Title: High-resolution observations of interactions during the
emergence of magnetic flux from the photosphere to the corona
Authors: Guglielmino, S. L.; Bellot Rubio, L. R.; Zuccarello, F.;
Romano, P.; Vargas Domínguez, S.
2010MSAIS..14..184G Altcode:
Interactions occurring at sites where new flux emerges and an
old flux system is already present can trigger various phenomena,
such as flux cancellation, reconnection events, and even flaring. We
analyze high-resolution observations of a small-scale flux emergence
event in NOAA 10971, observed simultaneously by the Hinode satellite
and the Swedish Solar Telescope in La Palma Island during a joint
campaign. G-band, Halpha , and Ca II H filtergrams were acquired
together with Fe I and Na I magnetograms. The data show that the
emerging region seen in the photosphere is associated with Ca II H
brightenings and a Halpha chromospheric surge. Moreover, EUV raster
scans and XRT filtergrams show cospatial brightenings. Comparing our
results with recent 3D simulations, we interpret our observations in the
context of the low-altitude magnetic reconnection model, suggesting
that interactions between the emerging flux and the pre-existing
magnetic field can explain the observed coupling.
---------------------------------------------------------
Title: Integrated Ly-alpha intensity emission in ribbon flares
Authors: Rubio da Costa, F.; Fletcher, L.; Labrosse, N.; Zuccarello, F.
2010MSAIS..14..193R Altcode:
We have analyzed two flares observed by TRACE in Ly alpha (on 8th
September 1999 and 28th February 1999) in order to deduce their
morphology, temporal evolution, radiative outputs and compare these
results with data obtained in the X-range (SXT and HXT on Yohkoh) and
with magnetograms (MDI/SOHO). These observational data and the results
obtained by a theoretical study of the intensity of the radiation
emitted by hydrogen lines, contribute to construct semi-empirical and
theoretical models of the chromospheric emission during flares. Future
observations by the planned Extreme Ultraviolet Imager selected for
the Solar Orbiter mission -which will have a Lyman alpha channel-
and this work, can help in designing observational flare studies.
---------------------------------------------------------
Title: Morphological and dynamical properties of small-scale
chromospheric features deduced from IBIS observations
Authors: Contarino, L.; Zuccarello, F.; Romano, P.; Spadaro, D.;
Ermolli, I.
2009A&A...507.1625C Altcode:
Context: In the past, chromospheric features were mostly studied by
analyzing observations performed along the Hα profile, but several
aspects related to their formation and dynamics remained uncertain
and poorly understood. Recently, new investigations have been carried
out using data obtained along the Ca II line at 854.21 nm, providing
new inputs for clarification of some of these aspects.<BR /> Aims:
In order to give a further contribution to the comprehension of the
physical processes occurring in small-scale chromospheric features,
we analyzed high spatial and temporal resolution images, acquired along
the Ca II (λ = 854.21 nm) line with the Interferometric Bidimensional
Spectrometer (IBIS). We studied four chromospheric structures such
as mottles and arches belonging to an arch filament system (AFS)
inside a bipolar region, observed on October 3, 2006.<BR /> Methods:
We evaluated the plasma velocity along the line of sight (LOS) using
two methods: the Doppler shift of the centroid of the line profile and
the cloud model. Also, we deduced the mean temperature, the Doppler
width, the optical thickness and the source function in the structures
to which we could apply the cloud model.<BR /> Results: The pattern
of the LOS velocity in the four mottles showed different behaviors. A
mottle, initially, showed positive and negative velocities in eastern
and western endpoints, respectively, then the plasma motion seems
to reverse over a period of about 4 mn. In another mottle a motion
characterized by alternate upward and downward plasma flow along the
main axis was recorded. Irregular upward and downward motions along
the other two mottles confirm previous results. The LOS velocities
measured in the AFS, observed during the decay phase of the region,
are of the same order of magnitude as those measured in short-lived
active regions during their emergence phase.<BR /> Conclusions:
The observations carried out in the Ca II line allowed us to obtain
information on small-scale magnetic features, like mottles and AFS,
observed in the chromosphere. These results, on one hand, confirm
previous results obtained using data acquired in the Hα line, and on
the other hand, provide new clues to the dynamic similarities between
mottles and dynamic fibrils. Moreover, this study allowed us to single
out the presence of an AFS during a phase characterized by decreasing
magnetic flux and the approach of the opposite polarities.
---------------------------------------------------------
Title: Observations of a solar flare and filament eruption in Lyman
α and X-rays
Authors: Rubio da Costa, F.; Fletcher, L.; Labrosse, N.; Zuccarello, F.
2009A&A...507.1005R Altcode: 2009arXiv0909.4705R
Context: Lα is a strong chromospheric emission line, which has been
relatively rarely observed in flares. The Transition Region and Coronal
Explorer (TRACE) has a broad “Lyman α” channel centered at 1216
Å used primarily at the beginning of the mission. A small number of
flares were observed in this channel. <BR />Aims: We aim to characterise
the appearance and behaviour of a flare and filament ejection which
occurred on 8th September 1999 and was observed by TRACE in Lα, as well
as by the Yohkoh Soft and Hard X-ray telescopes. We explore the flare
energetics and its spatial and temporal evolution. We have in mind the
fact that the Lα line is a target for the Extreme Ultraviolet Imaging
telescope (EUI) which has been selected for the Solar Orbiter mission,
as well as the LYOT telescope on the proposed SMESE mission. <BR
/>Methods: We use imaging data from the TRACE 1216 Å, 1600 Å and
171 Å channels, and the Yohkoh hard and soft X-ray telescopes. A
correction is applied to the TRACE data to obtain a better estimate of
the pure Lα signature. The Lα power is obtained from a knowledge of
the TRACE response function, and the flare electron energy budget is
estimated by interpreting Yohkoh/HXT emission in the context of the
collisional thick target model. <BR />Results: We find that the Lα
flare is characterised by strong, compact footpoints (smaller than the
UV ribbons) which correlate well with HXR footpoints. The Lα power
radiated by the flare footpoints can be estimated, and is found to be
on the order of 10<SUP>26</SUP> erg s<SUP>-1</SUP> at the peak. This is
less than 10% of the power inferred for the electrons which generate
the co-spatial HXR emission, and can thus readily be provided by
them. The early stages of the filament eruption that accompany the
flare are also visible, and show a diffuse, roughly circular spreading
sheet-like morphology, with embedded denser blobs. <BR />Conclusions:
On the basis of this observation, we conclude that flare and filament
observations in the Lα line with the planned EUI and LYOT telescopes
will provide valuable insight into solar flare evolution and energetics,
especially when accompanied by HXR imaging and spectroscopy.
---------------------------------------------------------
Title: Solar Weather Event Modelling and Prediction
Authors: Messerotti, Mauro; Zuccarello, Francesca; Guglielmino,
Salvatore L.; Bothmer, Volker; Lilensten, Jean; Noci, Giancarlo;
Storini, Marisa; Lundstedt, Henrik
2009SSRv..147..121M Altcode:
Key drivers of solar weather and mid-term solar weather are reviewed
by considering a selection of relevant physics- and statistics-based
scientific models as well as a selection of related prediction models,
in order to provide an updated operational scenario for space weather
applications. The characteristics and outcomes of the considered
scientific and prediction models indicate that they only partially cope
with the complex nature of solar activity for the lack of a detailed
knowledge of the underlying physics. This is indicated by the fact that,
on one hand, scientific models based on chaos theory and non-linear
dynamics reproduce better the observed features, and, on the other
hand, that prediction models based on statistics and artificial neural
networks perform better. To date, the solar weather prediction success
at most time and spatial scales is far from being satisfactory, but
the forthcoming ground- and space-based high-resolution observations
can add fundamental tiles to the modelling and predicting frameworks
as well as the application of advanced mathematical approaches in the
analysis of diachronic solar observations, that are a must to provide
comprehensive and homogeneous data sets.
---------------------------------------------------------
Title: Magnetic evolution of superactive regions. Complexity and
potentially unstable magnetic discontinuities
Authors: Criscuoli, S.; Romano, P.; Giorgi, F.; Zuccarello, F.
2009A&A...506.1429C Altcode: 2009arXiv0908.3608C
Context: It is widely accepted that solar flares are manifestations
of magnetic reconnection events taking place in the solar
atmosphere. Several aspects of these events remain unclear, although
many efforts have been devoted to the investigation of magnetic
field configurations at flare occurrence sites. <BR />Aims: In this
work, we have studied the temporal evolution of some properties of
a sample of superactive regions with the aim to single out the most
significant for flare activity forecasting. <BR />Methods: We have
investigated properties of 14 superactive regions, observed between
January 1st 2000 and December 31st 2006 with MDI/SOHO instrument and
characterized by a particularly intense flare activity during their
passage on the solar disk. We have analyzed the temporal evolution of
fractal and multifractal properties of photospheric magnetic fields,
namely the generalized fractal dimension and the contribution and
dimensional diversities, which describe geometrical properties of
the magnetic field, as well as the potential unstable volumes of
magnetic discontinuities above the studied ARs, which may provide
information about the magnetic field configuration in upper layers of
the atmosphere. Correlations of these quantities with the flare index,
which provides information about the flare activity of a region, have
also been estimated. <BR />Results: We found that in 50% of our sample
the generalized fractal dimension is correlated with the flare index
computed over windows of 50 h, while the contribution diversity and the
dimensional diversity are anticorrelated with the same index. A clear
increase of the potential unstable volume of magnetic discontinuities in
the corona is observed before the phases characterized by more frequent
and intense flares. We also found that the free energy distribution
functions of unstable volumes of the analyzed superactive regions can be
fitted with straight lines whose slope is larger than the values found
in previous works for less active magnetic regions. <BR />Conclusions:
The generalized fractal dimension and the potential unstable volume
of magnetic discontinuities are the most suitable for statistical
investigations of relations with flare activity over longer (50 h)
and shorter (few hours) time intervals, respectively. <P />Appendix
A is only available in electronic form at http://www.aanda.org
---------------------------------------------------------
Title: Magnetic helicity and active filament configuration
Authors: Romano, P.; Zuccarello, F.; Poedts, S.; Soenen, A.;
Zuccarello, F. P.
2009A&A...506..895R Altcode:
Context: The role of magnetic helicity in active filament formation
and destabilization is still under debate. <BR />Aims: Although active
filaments usually show a sigmoid shape and a twisted configuration
before and during their eruption, it is unclear which mechanism leads
to these topologies. In order to provide an observational contribution
to clarify these issues, we describe a filament evolution whose
characteristics seem to be directly linked to the magnetic helicity
transport in corona. <BR />Methods: We applied different methods to
determine the helicity sign and the chirality of the filament magnetic
field. We also computed the magnetic helicity transport rate at the
filament footpoints. <BR />Results: All the observational signatures
provided information on the positive helicity and sinistral chirality of
the flux rope containing the filament material: its forward S shape,
the orientation of its barbs, the bright and dark threads at 195
Å. Moreover, the magnetic helicity transport rate at the filament
footpoints showed a clear accumulation of positive helicity. <BR
/>Conclusions: The study of this event showed a correspondence between
several signatures of the sinistral chirality of the filament and
several evidences of the positive magnetic helicity of the filament
magnetic field. We also found that the magnetic helicity transported
along the filament footpoints showed an increase just before the
change of the filament shape observed in Hα images. We argued that
the photospheric regions where the filament was rooted might be the
preferential ways where the magnetic helicity was injected along
the filament itself and where the conditions to trigger the eruption
were yielded.
---------------------------------------------------------
Title: Modelling the initiation of coronal mass ejections: magnetic
flux emergence versus shearing motions
Authors: Zuccarello, F. P.; Jacobs, C.; Soenen, A.; Poedts, S.;
van der Holst, B.; Zuccarello, F.
2009A&A...507..441Z Altcode:
Context: Coronal mass ejections (CMEs) are enormous expulsions of
magnetic flux and plasma from the solar corona into the interplanetary
space. These phenomena release a huge amount of energy. It is generally
accepted that both photospheric motions and the emergence of new
magnetic flux from below the photosphere can put stress on the system
and eventually cause a loss of equilibrium resulting in an eruption. <BR
/>Aims: By means of numerical simulations we investigate both emergence
of magnetic flux and shearing motions along the magnetic inversion
line as possible driver mechanisms for CMEs. The pre-eruptive region
consists of three arcades with alternating magnetic flux polarity,
favouring the breakout mechanism. <BR />Methods: The equations of ideal
magnetohydrodynamics (MHD) were advanced in time by using a finite
volume approach and solved in spherical geometry. The simulation domain
covers a meridional plane and reaches from the lower solar corona
up to 30 R_⊙. When we applied time-dependent boundary conditions
at the inner boundary, the central arcade of the multiflux system
expands, leading to the eventual eruption of the top of the helmet
streamer. We compare the topological and dynamical evolution of the
system when driven by the different boundary conditions. The available
free magnetic energy and the possible role of magnetic helicity in the
onset of the CME are investigated. <BR />Results: In our simulation
setup, both driving mechanisms result in a slow CME. Independent of the
driving mechanism, the overall evolution of the system is the same: the
actual CME is the detatched helmet streamer. However, the evolution of
the central arcade is different in the two cases. The central arcade
eventually becomes a flux rope in the shearing case, whereas in the
flux emergence case there is no formation of a flux rope. Furthermore,
we conclude that magnetic helicity is not crucial to a solar eruption.
---------------------------------------------------------
Title: Numerical simulations of homologous coronal mass ejections
in the solar wind
Authors: Soenen, A.; Zuccarello, F. P.; Jacobs, C.; Poedts, S.;
Keppens, R.; van der Holst, B.
2009A&A...501.1123S Altcode:
Context: Coronal mass ejections (CMEs) are enormous expulsions of
magnetic flux and plasma from the solar corona. Most scientists agree
that a coronal mass ejection is the sudden release of magnetic free
energy stored in a strongly stressed field. However, the exact reason
for this sudden release is still highly debated. <BR />Aims: In an
initial multiflux system in steady state equilibrium, containing
a pre-eruptive region consisting of three arcades with alternating
magnetic flux polarity, we study the initiation and early evolution
properties of a sequence of CMEs by shearing a region slightly
larger than the central arcade. <BR />Methods: We solve the ideal
magnetohydrodynamics (MHD) equations in an axisymmetrical domain
from the solar surface up to 30 R_⊙. The ideal MHD equations are
advanced in time over a non uniform grid using a modified version of
the Versatile Advection Code (VAC). <BR />Results: By applying shearing
motions on the solar surface, the magnetic field is energised and
multiple eruptions are obtained. Magnetic reconnection first opens the
overlying field and two new reconnections sites set in on either side
of the central arcade. After the disconnection of the large helmet top,
the system starts to restore itself but cannot return to its original
configuration as a new arcade has already started to erupt. This process
then repeats itself as we continue shearing. <BR />Conclusions: The
simulations reported in the present paper, demonstrate the ability to
obtain a sequence of CMEs by shearing a large region of the central
arcade or by shearing a region that is only slightly larger than
the central arcade. We show, be it in an axisymmetric configuration,
that the breakout model can not only lead to confined eruptions but
also to actual coronal mass ejections provided the model includes a
realistic solar wind model.
---------------------------------------------------------
Title: Observation of bipolar moving magnetic features streaming
out from a naked spot
Authors: Zuccarello, F.; Romano, P.; Guglielmino, S. L.; Centrone,
M.; Criscuoli, S.; Ermolli, I.; Berrilli, F.; Del Moro, D.
2009A&A...500L...5Z Altcode:
Context: Mechanisms responsible for active-region formation, evolution,
and decay have been investigated by many authors and several common
features have been identified. In particular, a key element in the
dispersal of the magnetic field seems to be the presence of magnetic
elements, called moving magnetic features (MMFs). <BR />Aims: We
analyze the short-lived sunspot group NOAA 10977, which appeared on
the solar disk between 2 and 8 December 2007, to study the details of
its emergence and decay phases. <BR />Methods: We performed a multi
wavelength analysis of the region using images at visible (G band
and Hα) and near-IR (Ca II) wavelengths acquired by both the IBIS
instrument and SOT/HINODE, EUV images (17.1 nm) acquired by TRACE, and
MDI and SOT magnetograms. <BR />Results: The observed region exhibits
some peculiarities. During the emergence phase the formation of the
f-pore was initially observed, while the p-polarity later formed a
naked spot, i.e., a sunspot without a penumbra. We measured a moat
flow around this spot, and observed some MMFs streaming out from it
during the decay phase. The characteristics of these MMFs allowed us
to classify them as type I (U-shaped) MMFs. They were also cospatial
with sites of increased brightness both in the photosphere and the
chromosphere. <BR />Conclusions: The presence of bipolar MMFs in a
naked spot indicates that current interpretation of bipolar MMFs,
as extensions of the penumbral filaments beyond the sunspot outer
boundaries, should be revised, to take into account this observational
evidence. We believe that our results provide new insights into
improving models of sunspot evolution.
---------------------------------------------------------
Title: Evolution of an eruptive flare loop system
Authors: Romano, P.; Zuccarello, F.; Fletcher, L.; Rubio da Costa,
F.; Bain, H. M.; Contarino, L.
2009A&A...498..901R Altcode:
Context: Flares, eruptive prominences and coronal mass ejections are
phenomena where magnetic reconnection plays an important role. However,
the location and the rate of the reconnection, as well as the mechanisms
of particle interaction with ambient and chromospheric plasma are still
unclear. <BR />Aims: In order to contribute to the comprehension of the
above mentioned processes we studied the evolution of the eruptive flare
loop system in an active region where a flare, a prominence eruption
and a CME occurred on August 24, 2002. <BR />Methods: We measured the
rate of expansion of the flare loop arcade using TRACE 195 Å images
and determined the rising velocity and the evolution of the low and high
energy hard X-ray sources using RHESSI data. We also fitted HXR spectra
and considered the radio emission at 17 and 34 GHZ. <BR />Results:
We observed that the top of the eruptive flare loop system initially
rises with a linear behavior and then, after 120 mn from the start of
the event registered by GOES at 1-8 Å, it slows down. We also observed
that the heating source (low energy X-ray) rises faster than the top
of the loops at 195 Å and that the high energy X-ray emission (30-40
keV) changes in time, changing from footpoint emission at the very
onset of the flare to being coincident during the flare peak with the
whole flare loop arcade. <BR />Conclusions: The evolution of the loop
system and of the X-ray sources allowed us to interpret this event in
the framework of the Lin & Forbes model (2000), where the absolute
rate of reconnection decreases when the current sheet is located at an
altitude where the Alfvén speed decreases with height. We estimated
that the lower limit for the altitude of the current sheet is 6 ×
10<SUP>4</SUP> km. Moreover, we interpreted the unusual variation of
the high energy HXR emission as a manifestation of the non thermal
coronal thick-target process which appears during the flare in a manner
consistent with the inferred increase in coronal column density.
---------------------------------------------------------
Title: Magnetic Flux Emergence and Shearing Motions as Trigger
Mechanisms for Coronal Mass Ejections
Authors: Poedts, S.; Soenen, A.; Zuccarello, F. P.; Jacobs, C.;
van der Holst, B.
2009AIPC.1121...99P Altcode:
We study the initiation and early evolution of coronal mass ejections
(CMEs) in the framework of numerical ideal magnetohydrodynamics
(MHD). The magnetic field of the active region possesses a topology in
order for the “breakout” model to work. An initial multi-flux system
in steady equilibrium containing a pre-eruptive region consisting of
three arcades with alternating flux polarity is kept in place by the
magnetic tension of the overlying closed magnetic field of the helmet
streamer. Both foot point shearing and magnetic flux emergence are used
as a triggering mechanism in this model. The boundary conditions cause
the central arcade to expand and lead to the eventual ejection of the
top of the helmet streamer. We compare the topological and dynamical
evolution of the two triggering mechanisms and find that the overall
evolution of the systems are similar.
---------------------------------------------------------
Title: Emergence and evolution of active and ephemeral regions:
Comparison between observations and models
Authors: Zuccarello, Francesca; Guglielmino, Salvatore L.; Battiato,
Viviana; Contarino, Lidia; Spadaro, Daniele; Romano, Pado
2009AcGeo..57...15Z Altcode: 2008AcGeo.tmp...44Z
This work aims to describe some aspects relevant to the emergence
of magnetic structures on the solar surface. Using high resolution
photospheric and chromospheric data, besides than EUV images acquired
by space telescopes, the dynamics of rising flux tubes is studied. It
is shown that, for both long-lived and short-lived magnetic regions, the
flux tubes are initially characterized by a high rising velocity, which
eventually decreases as the region develops. Other results concern the
timeline of the active regions appearance in the atmospheric layers and
the asymmetries in plasma downflows between preceding and following
legs of the flux tubes. These results are briefly discussed in the
light of most recent models.
---------------------------------------------------------
Title: Flare forecasting based on sunspot-groups characteristics
Authors: Contarino, Lidia; Zuccarello, Francesca; Romano, Paolo;
Spadaro, Daniele; Guglielmino, Salvatore L.; Battiato, Viviana
2009AcGeo..57...52C Altcode: 2008AcGeo.tmp...51C
Our comprehension of solar flares is still lacking in many aspects
and the possibility of observing active regions during the first
phases of flare occurrence is limited by our capability of doing
accurate flare forecasting. In order to give a contribution to this
aspect, we focused our attention on the characteristics that must
be fulfilled by sunspot-groups in order to be flare-productive. We
addressed this problem using a statistical approach: first, we analyzed
sunspot-groups parameters (i.e., Zürich class, magnetic configuration,
area, morphology of the penumbra) and evolution; then, we performed
a flare forecasting campaign, based on the results obtained in the
first phase and on real-time observations. The results obtained by
comparing the flare forecasting probability with the number of flares
that have actually occurred are quite encouraging; we plan to improve
this procedure by including a bigger statistical sampling.
---------------------------------------------------------
Title: Multi-wavelength observations of flares and eruptive filaments
Authors: Zuccarello, Francesca; Contarino, Lidia; Romano, Paolo;
Battiato, Viviana; Guglielmino, Salvo L.
2009AcGeo..57...24Z Altcode: 2008AcGeo.tmp...26Z
In this paper we report some results obtained from multi-wavelength
observations carried out to study the mechanisms operating in flares and
filament eruptions. Most of these studies have given indication of the
presence of phenomena that might be considered signatures of magnetic
reconnection, while others have pointed out the important role played
by magnetic helicity transport in corona before the eruptive phase.
---------------------------------------------------------
Title: The X17.2 flare occurred in NOAA 10486: an example of filament
destabilization caused by a domino effect
Authors: Zuccarello, F.; Romano, P.; Farnik, F.; Karlicky, M.;
Contarino, L.; Battiato, V.; Guglielmino, S. L.; Comparato, M.;
Ugarte-Urra, I.
2009A&A...493..629Z Altcode:
Context: It is now possible to distinguish between two main models
describing the mechanisms responsible for eruptive flares : the standard
model, which assumes that most of the energy is released, by magnetic
reconnection, in the region hosting the core of a sheared magnetic
field, and the breakout model, which assumes reconnection occurs
at first in a magnetic arcade overlaying the eruptive features. <BR
/>Aims: We analyze the phenomena observed in NOAA 10486 before and
during an X17.2 flare that occurred on 2003 October 28, to study the
relationship between the pre-flare and flare phases and determine which
model is the most suitable for interpreting this event. <BR />Methods:
We performed an analysis of multiwavelength data set available for
the event using radio data (0.8-4.5 GHz), images in the visible range
(WL and Hα), EUV images (1600 and 195 Å), and X-ray data, as well
as MDI longitudinal magnetograms. We determined the temporal sequence
of events occurring before and during the X17.2 flare and the magnetic
field configuration in the linear force-free field approximation. <BR
/>Results: The active region was characterized by a multiple arcade
configuration and the X17.2 flare was preceded, by ~2 h, by the partial
eruption of one filament. This eruption caused reconnection at null
points located in the low atmosphere and a decrease in magnetic tension
in the coronal field lines overlaying other filaments present in the
active region. As a consequence, these filaments were destabilized and
the X17.2 flare occurred. <BR />Conclusions: The phenomena observed
in NOAA 10486 before and during the X17.2 flare cannot be explained
by a simple scenario such as the standard or breakout model, but
instead in terms of a so-called domino effect, involving a sequence
of destabilizing processes that triggered the flare.
---------------------------------------------------------
Title: EST: the European future of solar ground-based observations
Authors: Zuccarello, F.; EST Team
2009MmSAI..80..243Z Altcode:
EST (European Solar Telescope) is a pan-European project involving 29
partners from 9 different countries (14 scientific institutions and 15
industries). It aims at the realization of a 4-m class solar telescope,
with spectropolarimetric and imaging instruments characterized by
high spatial and temporal resolution and observing in the wavelength
range UV-NIR. EST is aimed at answering to a number of questions made
by the international scientific community: determine the mechanisms
responsible for the interaction between magnetic fields and plasma,
single out the physical processes at the basis of energy transport
in the solar atmospheric layers, acquire the capability of predicting
phenomena that might directly or indirectly affect the Earth, etc. At
present the project is in the Design Phase Study, financed by the
European Union in the framework of FP7 - Research Infrastructures.
---------------------------------------------------------
Title: Observations of small-scale flux evolution with HINODE
Authors: Guglielmino, S. L.; Romano, P.; Zuccarello, F.; Bellot Rubio,
L. R.
2009MmSAI..80..278G Altcode:
We present observations of NOAA 10971 acquired by the Solar
Optical Telescope onboard the HINODE satellite. We have inverted
spectropolarimetric data of SOT/SP along Fe I doublet at 630.15 nm
and 630.25 nm, using the SIR inversion code in order to get magnetic
field strength, inclination, azimuth, Doppler velocity and temperature
from the observed Stokes profiles. We compare these first results with
SOT/FG broad-band observations in the Ca II H line (396.85 ± 0.3 nm)
and G-band (430.5 ±± 0.8 nm), and with magnetograms obtained from the
narrow-band shuttered Stokes I and V in the wings of the Na I D1 line
(589.6 nm). Small-scale events of flux emergence and flux cancellation
have been singled out.
---------------------------------------------------------
Title: Hinode Observations of Chromospheric Brightenings in the Ca
II H Line during Small-Scale Flux Emergence Events
Authors: Guglielmino, S. L.; Zuccarello, F.; Romano, P.; Bellot Rubio,
L. R.
2008ApJ...688L.111G Altcode: 2008arXiv0810.2494G
Ca II H emission is a well-known indicator of magnetic activity in
the Sun and other stars. It is also viewed as an important signature
of chromospheric heating. However, the Ca II H line has not been
used as a diagnostic of magnetic flux emergence from the solar
interior. Here we report on Hinode observations of chromospheric Ca II
H brightenings associated with a repeated, small-scale flux emergence
event. We describe this process and investigate the evolution of
the magnetic flux, G-band brightness, and Ca II H intensity in the
emerging region. Our results suggest that energy is released in the
chromosphere as a consequence of interactions between the emerging
flux and the preexisting magnetic field, in agreement with recent 3D
numerical simulations.
---------------------------------------------------------
Title: Initiation of Coronal Mass Ejections by Magnetic Flux Emergence
in the Framework of the Breakout Model
Authors: Zuccarello, F. P.; Soenen, A.; Poedts, S.; Zuccarello, F.;
Jacobs, C.
2008ApJ...689L.157Z Altcode:
The possible role of magnetic flux emergence in the initiation of
coronal mass ejections (CMEs) is investigated in the framework of the
breakout model. The ideal MHD equations are solved numerically on a
spherical, axisymmetric (2.5-dimensional) domain. An initial multiflux
system in steady equilibrium containing a pre-eruptive region consisting
of three arcades with alternating magnetic flux polarity is kept in
place by the magnetic tension of the overlying closed magnetic field of
a helmet streamer. The emergence of new magnetic flux in the central
arcade is simulated by means of a time-dependent boundary condition
on the vector potential applied at the solar base. Height-time plots
of the ejected material, as well as time evolution of the magnetic,
kinetic and internal energy in the entire domain as functions of flux
emergence rate, are produced. The results show that the emergence of
new magnetic flux in the central arcade triggers a CME. The obtained
eruption corresponds to a slow CME, and conversion of magnetic energy
into kinetic energy is observed.
---------------------------------------------------------
Title: Studying the decay phase of a short-lived active region
with coordinated DST/IBIS, Hinode/EIS+SOT+XRT, SOHO/MDI and TRACE
observations
Authors: Zuccarello, F.; Berrilli, F.; Centrone, M.; Contarino, L.;
Criscuoli, S.; Del Moro, D.; Ermolli, I.; Giorgi, F.; Guglielmino,
L. S.; Salerno, C.; Spadaro, D.; Romano, P.
2008ESPM...12.2.56Z Altcode:
This study concerns the physical processes occurring during the decay
phase of the short-lived active region NOAA 10977, as evaluated from
analysis of data gathered using ground- (DST/IBIS) and space-based
(Hinode/EIS+SOT+XRT, SOHO/MDI and TRACE) facilities. The coordinated
observing campaign was performed from December 1st to 9th, 2007,
covering several spectral ranges, with unprecedented spatial and
spectral resolution. We present preliminary results of the Doppler
analysis of plasma motions evaluated from monochromatic images taken
along the Ca II (8542 Å) and the Fe I (7049 Å) spectral lines with
IBIS. We also report results concerning the horizontal displacements of
photospheric magnetic structures and advection flows as obtained from
application of Local Correlation Tracking (LCT) and Two-Level Structure
Tracking (TST) techniques to both the LoS magnetograms taken by MDI
and to high resolution intensity maps obtained by IBIS at DST/NSO. <P
/>Further contributions to understanding the mechanisms at the base
of the magnetic field diffusion are provided from the inversion of
the Stokes profiles of the photospheric Fe I lines at 6301.5 Å and
6302.5 Å, obtained with SOT/SP, and the analysis of filtergrams in
the core of the Ca II H line (3968.5 ± 3 Å) and images in G-band
(4305 ± 8 Å) taken by SOT/BFI, as well as EIS data and images taken
by the thin Be of XRT, and by TRACE at 171 Å and 1600 Å.
---------------------------------------------------------
Title: The ADAHELI Solar Mission
Authors: Berrilli, F.; Velli, M.; Roselli, L.; Bigazzi, A.; Moretti,
P. F.; Romoli, M.; Orsini, S.; Cavallini, F.; Greco, V.; Carbone,
V.; Consolini, G.; Di Mauro, M. P.; Ermolli, I.; Pietropaolo, E.;
Romano, P.; Ventura, P.; White, S. M.; Zuccarello, F.; Cauzzi, G.;
Valdettaro, L.
2008ESPM...12..6.6B Altcode:
ADAHELI (Advanced Astronomy for HELIOphysics) is an Italian Space
project for the investigation of solar photospheric and chromospheric
dynamics, via high-resolution spectro-polarimetric observations in the
near-infrared spectral range. The mission has been financed for phase
A study in the framework of ASI Italian Space Agency Small Missions
Program call of September 2007. <P />Four fields have been selected
to highlight the specific benefits of ADAHELI scientific payload: 1)
Photospheric and chromospheric dynamics and structure, 2) Emergence and
evolution of solar active regions and solar irradiance, 3) Chromospheric
and corona heating and turbulence, 4) Solar flares in the millimeter
wavelength region. <P />The principal science instrument, ISODY, is
a 50 cm solar telescope equipped with an innovative Focal Plane Suite
composed of a spectro-polarimetric imager, based upon two Fabry-Perot
interferometers operating in the NIR regions around 845nm and 1083nm, a
broad band imager, and a correlation tracker used as image stabilization
system. <P />Designed Mission Profiles for ADAHELI intend to achieve
continuous high-spectral and spatial resolution observations of the
Sun for a routine duration of 4 hours with a goal to be extended to
24 hours. <P />ADAHELI also carries MIOS, a millimeter wavelengths
radiometer operating at around 90 GHz for flare detection. <P />The
ADAHELI payload's instrument suite integrates and complements, without
overlap, the present major objectives of ESA, NASA and the International
Living with a Star program, in particular Solar Dynamics Observatory,
PICARD, Solar Orbiter, and the Solar Probe missions. <P />Proposals
for optional instruments are also under evaluation: DIMMI-2h, a
double channel MOF based full disk imager operating at 589nm and
770nm, allowing high temporal resolution velocity and magnetic field
measurements; EISR a two channel spectrometer operating in the 50-130
nm wavelength range, and NPA, an in-situ Neutral Particle Analyzer
to detect Energetic Neutral Atoms (ENA). Science objectives related
to optional instruments include: solar high and low-degree p modes
oscillations, EUV solar structures and variability, solar gravitational
red-shift measurement, detection of ENA originating from the plasma
region in the Earth's magnetosphere and undergoing reflection from
the Earth's atmosphere.
---------------------------------------------------------
Title: Chromospheric Brightenings during Small-scale Flux Emergence
Events
Authors: Guglielmino, S. L.; Zuccarello, F.; Romano, P.; Bellot Rubio,
L. R.
2008ESPM...12.2.46G Altcode:
We present multi-wavelength high-resolution observations of active
region NOAA 10971, performed by the Solar Optical Telescope aboard
the Hinode satellite. Small-scale events of flux emergence occurring
in this region have been singled out. In particular, we report
observations of chromospheric Ca II H brightenings associated with a
repeated emergence event. We describe this process and investigate
the evolution of the magnetic flux, G-band brightness, and Ca II H
intensity in the emerging region. We compare these observations with
simultaneous spectropolarimetric measurements, using the SIR code to
retrieve the thermal, dynamical, and magnetic properties of the emerging
region. We discuss our results in the context of the chromospheric
heating problem. Magnetic reconnection between the emerging flux
and the pre-existing chromospheric field would be able to explain
the observed chromospheric brightness enhancements. The reconnection
releases energy, and this could be an efficient source of local heating
for the chromosphere, as suggested by recent 3D numerical simulations.
---------------------------------------------------------
Title: Investigation of Lyman <alpha> Emission in a Solar Flare
Authors: Rubio da Costa, F.; Fletcher, L.; Labrosse, N.; Zuccarello, F.
2008ESPM...12.2.64R Altcode:
The TRACE satellite observed a small number of solar flares in the
Lyman alpha channel, which have until now not been analysed. We look at
a well-observed flare on 8th September 1999 to investigate different
topics. We carry out a study of the spatial and temporal evolution of
the flare and associated filament eruption in Lyman alpha, hard X-rays
and soft X-rays, and examine the flare energetics using the hard X-rays
(in the collisional thick target approximation) to estimate the energy
flux carried by electrons, and TRACE Lyman alpha/1600 Å channels to
estimate the temperature and radiative power in UV. We will use these
observations to anticipate what can be observed in the future by the
proposed SMESE satellite mission, and to compare with predictions of
semi-empirical and theoretical models of the flare chromosphere.
---------------------------------------------------------
Title: Temporal Evolution of Magnetic Properties of Super Active
Regions
Authors: Criscuoli, S.; Giorgi, F.; Romano, P.; Zuccarello, F.
2008ESPM...12.2.57C Altcode:
It is widely accepted that solar flares are manifestations of magnetic
reconnection events taking place in the solar atmosphere. Several
aspects of these events remain unclear, although many efforts have
been devoted to the investigation of magnetic field configurations at
flares occurrence. <P />In this work we investigate some properties of
26 super active regions, observed between Jan 1 2000 and Dec 31 2006
with MDI/SOHO instrument and characterized by a particularly intense
flare activity during their passage on the solar disc. We analyzed
the temporal evolution of some fractal and multifractal estimators, as
well as other parameters like the distorsion of the magnetic inversion
line and the number of the singular points in potential fields with
the aim to single out the most significant for flare forecasting.
---------------------------------------------------------
Title: Magnetic flux emergence and shearing motions as CME trigger
mechanisms
Authors: Poedts, S.; Soenen, A.; Zuccarello, F. P.; Jacobs, C.;
van der Hoist, B.
2008AIPC.1043..291P Altcode:
We present recent developments in the mathematical modeling and
numerical simulations of the initiation and interplanetary evolution
of CMEs in the framework of ideal magneto-hydrodynamics (MHD). In
earlier work, we reconstructed simple, axisymmetric (2.5D) solar
wind models for the quiet Sun. Next, we mimicked fast CME events
by superposing high-density plasma blobs on the background wind and
launching them in a given direction at a certain speed, enabling the
study of the evolution of the fast CME shocks, their effects on the
coronal field and background solar wind. Here, more realistic CME onset
models are presented to investigate the possible role of magnetic foot
point shearing and magnetic flux emergence/disppearence as triggering
mechanisms of the instability. In particular, the well-known breakout
model has been superposed on a solar wind model and it is shown that
both foot point shearing and magnetic flux emergence can be used as
a triggering mechanism in this model.
---------------------------------------------------------
Title: Modelling the Initiation of Coronal Mass Ejections by Magnetic
Flux Emergence
Authors: Zuccarello, F. P.; Soenen, A.; Poedts, S.
2008ESPM...12.3.55Z Altcode:
The possible role of magnetic flux emergence as triggering mechanism
for the initiation of Coronal Mass Ejections (CMEs) is studied in the
framework of the ideal magnetohydrodynamics (MHD) model. The full MHD
equations are solved numerically on a spherical, axisymmetric (2.5D)
domain. <P />All simulations are performed with a modified version
of the Versatile Advection Code (VAC) (Toth 1996). The magnetic field
of the solution is maintained divergence-free at machine precision by
exploiting an approach similar to that of Balsara and Spicer (1999):
instead of storing the magnetic field components on a staggered
mesh, we use the vector potential components in the nodes. <P />In
order to get satisfactorily solar wind properties, the Manchester
et al. (2004) source term is implemented in the energy equation and
gravity is taken into account as well in the model. <P />Finally,
a magnetic vector potential is superimposed at the inlet boundary of
the Parker wind solution so that, when the steady state is reached,
the Antiochos et al. (1999) triple arcade 'break out' magnetic
field configuration (symmetric with respect to the equator) of a
helmet streamers is obtained. <P />When the steady state has been
reached, we impose a magnetic flux emergence at the inlet boundary
that is linearly growing in time during a time interval of ? t =
24 hours. After this time the vector potential at the solar base is
again fixed. Due to the magnetic flux emergence at the solar base,
extra radial magnetic field, is built up near the neutral line of the
central arcade that expands outward. This generates an extra upward
magnetic pressure force. As a consequence, the central flux system
expands outward. Also the overlying field expands and, therefore,
the downward magnetic tension increases. As a result, the X-point is
flattened. <P />When the distance between the central expanding arcade
field and the overlying streamer field is of the order of the grid
resolution, the (numerical) reconnection between these fields sets
in. A flux rope is formed and, later, accelerated. <P />Height-time
and velocity-height plots of the ejected material are produced. The
obtained eruption corresponds to a slow CME. The time evolution of
the magnetic energy, kinetic energy and internal energy in the entire
domain shows that magnetic energy is converted into kinetic energy,
as expected. <P />The energy evolution plots show, however, that only a
small amount of magnetic energy is released in the system, so that the
system evolves to a higher energy state. We think that the explanation
of this behavior lies in the role of the magnetic helicity, which we
neglected by only emerging radial magnetic field. <P />In conclusion,
we stress that by imposing a reasonable (Romano et al. (2007)) flux
emergence rate, in a large but realistic active region (with, of course,
model dimensionality limitations), quite realistic velocity profiles
and energetics of slow CMEs are obtained.
---------------------------------------------------------
Title: A C-level flare observed in an arch filament system:
reconnection between pre-existing and emerging field lines?
Authors: Zuccarello, F.; Battiato, V.; Contarino, L.; Guglielmino,
S.; Romano, P.; Spadaro, D.
2008A&A...488.1117Z Altcode:
Context: Observations show that solar flares are often caused by the
emergence of new magnetic flux from subphotospheric layers and by
the interaction of the rising field lines with the ambient magnetic
field. In this framework, recent theoretical models of magnetic
flux emergence have investigated the effectiveness of magnetic
reconnection as a function of the old and new flux system relative
orientations. <BR />Aims: We aim to compare phenomena that occurred in
an active region, before and during a small flare, with the effects of
magnetic reconnection between nearly parallel magnetic field lines,
foreseen by these models. <BR />Methods: We analyzed high resolution
photospheric and chromospheric data acquired during a coordinated
observational campaign performed with the THEMIS telescope in IPM
mode, as well as MDI magnetograms and TRACE 1600 and 171 Å images, to
investigate the dynamics and the magnetic configuration of the active
region hosting the flare. <BR />Results: An emerging arch filament
system (AFS) was observed in the area between the two main sunspots:
it showed typical upward motion at the arch tops and plasma downward
motion at the footpoints. A C-level flare, characterized by a factor
of 3 peak enhancement in the GOES X-ray emission with respect to the
pre-event background, occurred in this zone, where the configuration of
the emerging magnetic field lines showed a small (∼ 12°) relative
inclination with respect to the old flux system. <BR />Conclusions:
In an active region (age ≥6 days) a new magnetic flux bundle emerged
between the two main polarity spots. It gave rise to the formation
of pores in the photosphere and to an AFS in the chromosphere. The
interaction between the new and the pre-existing field lines,
characterized by a small relative inclination, might have caused a
weak reconnection process and given rise to the C-level flare. This
result is in broad agreement with numerical simulations predicting
very limited reconnection when the two flux systems have an almost
parallel orientation.
---------------------------------------------------------
Title: 1967-2007: Forty years of outreach activity at INAF - Catania
Astrophysical Observatory
Authors: Cutispoto, G.; Leto, G.; Strazzulla, G.; Zuccarello, F.
2008ca07.conf..404C Altcode:
Outreach activity at the INAF-Catania Astrophysical Observatory (OACT)
started about forty years ago both at the M.G. Fracastoro station
on Mt. Etna and at the A. Ricco headquarters in Catania. In recent
years the requests for visits, conferences and courses have steadily
increased and about 9500 visitors per year have participated in the
events we have organised. Here we present our activities, as an example
of what can be accomplished in a relatively small institute.
---------------------------------------------------------
Title: Photospheric magnetic evolution of super active regions
Authors: Romano, P.; Zuccarello, F.
2007A&A...474..633R Altcode:
Context: Solar flares are one of the most interesting phenomena of
solar activity. Although many authors agree that their energy release
is related to magnetic reconnection, the phases preceding the magnetic
reconnection process are still unclear in several respects. <BR />Aims:
We studied the magnetic flux evolution in 26 super active regions
observed on the solar disc from Jan. 1, 2000 to Dec. 31, 2006, in order
to determine a physical relationship between flares and some properties
of the photospheric magnetic fields. <BR />Methods: This analysis
is based on full disc line of sight MDI magnetograms. We measured
the total magnetic flux, the magnetic flux imbalance, the horizontal
magnetic gradient and the number of magnetic features characterized by
a collection of pixels lying in the same bins of absolute strength. We
also elaborated an algorithm for the identification and the length
measurement of the magnetic inversion lines. <BR />Results: We found a
correlation between the evolution of the analyzed parameters and the
flare occurrence. The most intense phases of activity are associated
with phases of emergence of a magnetic field in 15 super active regions
and with phases of flux cancellation in 5 super active regions. <BR
/>Conclusions: Super active regions may be characterized by a different
behavior depending on their morphology. Some of them show a continuous
flare activity, while others present an alternation of active and
quiet phases. The deviations from magnetic polarity balance and the
length of the inversion lines characterized by a horizontal magnetic
gradient greater than 0.3 G km<SUP>-1</SUP> seem to have a major role
in producing a magnetic field topology able to trigger flares. <P
/>Tables A.1-A.3 and Figs. B.1-B.9 are only available in electronic
form at http://www.aanda.org
---------------------------------------------------------
Title: Plasma motions in a short-lived filament related to a magnetic
flux cancellation
Authors: Zuccarello, F.; Battiato, V.; Contarino, L.; Romano, P.;
Spadaro, D.
2007A&A...468..299Z Altcode:
Context: In recent years the mechanisms responsible for filament
formation and evolution have been investigated by many authors. In
particular, the role played by the processes of magnetic flux
cancellation in building up or destroying filaments is still a matter
of debate. <BR />Aims: In this paper we analyze the evolution of an
active region filament that formed in NOAA 10 407 on 14 July 2003,
to investigate the phenomena responsible for its destabilization
and short lifetime (~12 h). <BR />Methods: This analysis is based on
high-resolution Hα data acquired by THEMIS operating in IPM mode,
on Hα data acquired at Big Bear Solar Observatory, and on MDI/SOHO
magnetograms. Using these data, we determined the morphological,
dynamical, and magnetic evolution of the filament. <BR />Results: The
chromospheric images show two dark surges occurring sequentially in the
northern part of the filament, besides two bright Hα patches located
in the same area; from analysis of the photospheric magnetograms,
we could infer that a magnetic flux cancellation had occurred in
this area. <BR />Conclusions: The presence of a cancelling magnetic
feature (CMF) in the same area where the dark Hα surges occurred,
the temporal behavior of the velocity fields in the surges, and the
presence of bright Hα patches in the CMF area, suggest a scenario
where the coronal arcade initially sustaining the filament might have
undergone consecutive reconnection processes. From the concurrence of
these events with the filament activation and successive disappearance,
we believe that the arcade field lines, after the reconnection events,
changed such that the plasma filament was no longer confined in the
arcade: this led to its destabilization and disappearance.
---------------------------------------------------------
Title: An M1.5 Flare Triggered by a Multireconnection Process
Authors: Romano, P.; Zuccarello, F.; Contarino, L.
2007SoPh..240...49R Altcode:
We studied the magnetic configuration of active region NOAA 10672,
where two different mechanisms seem to contribute to its instability,
to the subsequent M1.5 flare, and to a halo CME. The analysis of
full-disk SOHO/MDI magnetograms and of WL and 171 Å TRACE images
shows in fact that both flux emergence and horizontal displacements
of photospheric flux concentrations have a key role in triggering
the event. On the basis of these pre-flare mechanisms, we provide a
description of a multireconnection process able to explain the flare
evolution observed by TRACE, as well as the two-step profile in X-ray
emission observed in the 1 - 8 Å band. Moreover, this work highlights
some photospheric signatures that can be considered as flare precursors.
---------------------------------------------------------
Title: Application of the Kopp and Pneuman model to an M2.5 flare
Authors: Contarino, L.; Romano, P.; Zuccarello, F.
2007MmSAI..78..261C Altcode:
We have analyzed X-ray and EUV images relevant to a system of loops
involved in an M2.5 flare that occurred in NOAA 9901 on 16 April,
2002. During the event the EUV and X-ray sources change from an X to
a Y configuration; the formation of a thin, filamentary structure,
compatible with what is expected from the collapse of an X-point
in a current sheet, is observed; moreover the height of the top of
the observed EUV loops and the separation between the footpoints
show an increase with time. The study of this event showed several
observational signatures, expected from theory during the formation
of a current sheet and consequent reconnection, which allowed us to
interpret it in the framework of the Kopp and Pneuman model \citep{KP}.
---------------------------------------------------------
Title: RHESSI and TRACE observations of an M 2.5 flare: a direct
application of the Kopp and Pneuman model
Authors: Contarino, L.; Romano, P.; Zuccarello, F.
2006A&A...458..297C Altcode:
Context: .The processes of current sheet formation and magnetic
reconnection are nowadays believed to be at the basis of several solar
phenomena, including erupting prominences, flares, and CMEs. However,
the possibility of determining clear signatures of the occurrence of
these processes in erupting active regions is still lacking in several
aspects.<BR /> Aims: .In this paper we analyze coronal images relevant
to a system of loops involved in a very energetic flare, to search
for observational signatures of current sheet formation and magnetic
reconnection and compare them with what is expected from theory.<BR
/> Methods: .X-ray and EUV data acquired by the Ramaty High-Energy
Solar Spectroscopic Imager (RHESSI) and the Transition Region and
Coronal Explorer (TRACE) satellites have been used to analyze an M2.5
flare that occurred in NOAA 9901 on 16 April 2002. The evolution of
the flare loops, the EUV footpoints, and the X-ray loop tops have
been studied.<BR /> Results: .The event shows a simple morphology in
which the EUV and X-ray sources change from an X to a Y configuration;
the formation of a thin, filamentary structure, compatible with what
is expected from the collapse of an X-point in a current sheet, is
observed; the height of the top of the observed EUV loops and the
separation between the footpoints show an increase with time.<BR />
Conclusions: .The study of this event provides several observational
signatures, expected from theory during the formation of a current
sheet and consequent reconnection, which allowed us to interpret it
in the framework of the Kopp and Pneuman model.
---------------------------------------------------------
Title: Cancelling magnetic feature and filament activation
Authors: Contarino, L.; Romano, P.; Zuccarello, F.
2006AN....327..674C Altcode:
We report in this paper the analysis of the evolution of a magnetic
fragment observed in NOAA 9445 on 5 May, 2001. This magnetic fragment
emerged laterally to a filament which later split into two parts. The
bifurcation site coincided with the magnetic fragment location and the
part of the filament which split was later destabilized and a flare
occurred. The magnetic flux variations in the magnetic fragment and
in the surrounding area were analyzed and, considering their trends
and other observational signatures (Hα brightenings and associated
plasma motions), we could infer that it was a cancelling magnetic
feature (CMF). We determined some geometrical and physical parameters
of the CMF (area, magnetic flux variation, cancellation speed and flux
cancellation rate) using high resolution magnetograms taken by BBSO. We
compared the observed parameters of the CMF with the parameters of
low-lying reconnection current sheets given in the model proposed
by Litvinenko (1999) and found good agreement between observed and
theoretical values. Therefore, we conclude that a low-lying magnetic
reconnection process might be the cause of the filament activation.
---------------------------------------------------------
Title: Magnetic Helicity Transport in Active Filaments
Authors: Romano, P.; Contarino, L.; Guglielmino, S.; Zuccarello, F.
2006ESASP.617E.143R Altcode: 2006soho...17E.143R
No abstract at ADS
---------------------------------------------------------
Title: Dayside Auroral Activity and Dependence from Solar Wind
Parameters
Authors: Orlando, A.; Massetti, S.; Zuccarello, F.
2006ESASP.617E.136O Altcode: 2006soho...17E.136O
No abstract at ADS
---------------------------------------------------------
Title: High Resolution Observations of Emerging Active Regions
Carried Out at the THEMIS Telescope
Authors: Battiato, V.; Billotta, S.; Contarino, L.; Guglielmino, S.;
Romano, P.; Soadaro, D.; Zuccarello, F.
2006ESASP.617E..51B Altcode: 2006soho...17E..51B
No abstract at ADS
---------------------------------------------------------
Title: A Detailed Analysis of an Ephemeral Region .
Authors: Guglielmino, S. L.; Martínez Pillet, V.; Ruiz Cobo, B.;
Zuccarello, F.; Lites, B. W.
2006MSAIS...9..103G Altcode:
In order to improve the understanding of the process of emergence of
magnetic flux on the solar surface, we studied the temporal evolution of
an ephemeral region using \emph{Advanced Stokes Polarimeter} data. We
adopted two different approaches: first, we used a Milne-Eddington
inversion to obtain mean parameters of the emerging bipole magnetic
configuration. Then, we considered the full radiative transfer
equation, and we studied the trend of all the previous parameters as
a function of the optical depth tau . We pointed out peculiar flows,
such as an initial upflow of 1.5 ;textrm {km s}<SUP>-1</SUP> where the
zenith angle is essentially horizontal, and downflows decreasing in
time in footpoints, characterized by a vertical field. These results
seem to confirm the emerging bipole topology, due to magnetic flux
tube emergence. The results obtained with this inversion confirm the
structure found with Milne-Eddington code. However we found regions
in which the presence of two distinct magnetic components is highly
significant. It also seems very interesting the trend of the temperature
with optical depth: the plasma temperature appears to grow up in the
high photosphere above the emerging bipole.
---------------------------------------------------------
Title: XLIX Congresso della Società Astronomica Italiana
Authors: Leto, G.; Zuccarello, F.
2006MSAIS...9....3L Altcode:
No abstract at ADS
---------------------------------------------------------
Title: SINERGIES (Sun, INterplanetary, EaRth Ground-based InstrumEntS)
or the potential of the Italian Network for Ground-Based Observations
of Sun-Earth Phenomena.
Authors: Amata, E.; Candidi, M.; Centrone, M.; Consolini, G.;
Contarino, L.; Criscuoli, S.; De Lauretis, M.; Diego, P.; Ermolli,
I.; Francia, P.; Giorgi, F.; Laurenza, M.; Magrí, M.; Marcucci, F.;
Massetti, S.; Messerotti, M.; Oliviero, M.; Penza, V.; Perna, C.;
Pietropaolo, E.; Romano, P.; Severino, G.; Spadaro, D.; Storini, M.;
Vellante, M.; Villante, U.; Zlobec, P.; Zuccarello, F.
2006MSAIS...9...82A Altcode:
The Italian Network for Ground-Based Observations of Sun-Earth
Phenomena, whose instruments monitor the Sun, the Interplanetary
Space, and the Earth's Magnetosphere, has recently started to operate
in a coordinated scheme. In this paper, we describe few significant
examples of this coordination effort. 1) During the year 2003, several
coordinated observational campaigns were carried out in order to study
the solar photospheric dynamics. 2) Reconstruction of TSI in time, for
periods spanning from a solar rotation up to the whole current solar
cycle. 3) Extreme solar events occurring during the late October -
early November 2003.
---------------------------------------------------------
Title: COST Action 724: the Italian contribution .
Authors: Messerotti, M.; Candidi, M.; Storini, M.; Zuccarello, F.
2006MSAIS...9..117M Altcode:
COST Action 724, devoted to developing the scientific basis for
monitoring, modelling and predicting Space Weather, is briefly outlined
with emphasis to the contribution by Italian researchers of the solar
and solar-terrestrial communities.
---------------------------------------------------------
Title: Dynamics and evolution of emerging active regions .
Authors: Battiato, V.; Billotta, S.; Contarino, L.; Romano, P.;
Spadaro, D.; Zuccarello, F.
2006MSAIS...9...85B Altcode:
In the framework of the study on active region emergence, we report
the results obtained from the analysis of two ARs (NOAA 10050 and NOAA
10407), characterized by different lifetimes: recurrent the former and
short-lived (7 days) the latter. The data used were acquired during
two observational campaigns carried out at THEMIS telescope in IPM
mode, coordinated with other instruments (IOACT, DOT, BBSO, MDI/SOHO,
EIT/SOHO, TRACE). The results obtained have provided indications on the
atmospheric layers where the first manifestations of the emerging AR
are evidenced, on the rate of emergence of magnetic flux, on the upward
velocity of AFS, on asymmetries in downward motions in the AFS legs.
---------------------------------------------------------
Title: SINERGIES, the Italian Network for Ground-Based Observations
of Sun-Earth Phenomena .
Authors: Amata, E.; Berrilli, F.; Candidi, M.; Cantarano, S.; Centrone,
M.; Consolini, G.; Contarino, L.; Criscuoli, S.; De Lauretis, M.;
Del Moro, D.; Egidi, A.; Ermolli, I.; Francia, P.; Giordano, S.;
Giorgi, F.; Oliviero, M.; Magrí, M.; Marcucci, F.; Massetti, S.;
Messerotti, M.; Parisi, M.; Perna, C.; Pietropaolo, E.; Romano, P.;
Severino, G.; Spadaro, D.; Storini, M.; Vellante, M.; Villante, U.;
Zlobec, P.; Zuccarello, F.
2006MSAIS...9...79A Altcode:
Since many years, the complex phenomena occurring on the Sun have
been continuously monitored by different and complementary ground
based instruments managed by groups of the Italian Astrophysics
Community. Recently some of these instruments have started to operate in
a coordinated scheme, the Italian Network for Ground-Based Observations
of Sun-Earth Phenomena. In this paper, we describe the characteristics
of the nodes belonging to the Network, called SINERGIES, the scientific
objectives, the facilities and the data storage system of the Network
itself. Due to its capabilities, the Network allows the Italian Solar
Terrestrial Physics Community to monitor solar activity and its effect
on the Earth.
---------------------------------------------------------
Title: SOLARNET-Italian Solar Archive Federation. The First Italian
Virtual Observatory Application
Authors: Volpicelli, C. A.; Antonucci, E.; Cora, A.; Giordano, S.;
Messerotti, M.; Santin, A.; Zlobec, P.; Severino, G.; Oliviero, M.;
DeMarino, I.; Alvino, R.; Straus, T.; Ermolli, I.; Centrone, C.;
Perna, C.; Zuccarello, F.; Romano, P.; Spadaro, D.; Contarino, L.
2006MSAIS...9..129V Altcode:
We describe the implementation of the national project SOLARNET (SOLar
ARchive NETwork) aimed at federating the heterogeneous Italian solar
data archives into a VO (Virtual Observatory) framework as a single
integrated database, and providing users with tools to search and
retrieve specific data sets. It interoperates using the SOAP/XML
Web Services exposed by each single node and managed via a unified
Portal.This project is the first real Italian Virtual Observatory
application using the standard defined by the IVOA (International
Virtual Observatory Alliance) working groups.
---------------------------------------------------------
Title: A statistical analysis of sunspot groups hosting M and X flares
Authors: Ternullo, M.; Contarino, L.; Romano, P.; Zuccarello, F.
2006AN....327...36T Altcode:
In this paper we present the results obtained from a statistical
analysis carried out by correlating sunspot-group data collected at the
INAF-Catania Astrophysical Observatory and in the NOAA reports with
data on M and X flares obtained by the GOES-8 satellite in the soft
X-ray range during the period January 1996-June 2003. These results
allow us to provide a quantitative estimate of the parameters typical
for an active region with very energetic flares. Moreover, the analysis
of the flare productivity as a function of the group evolutionary stage
indicates that the flaring probability of sunspots slightly increases
with the spot age during the first passage across the solar disk,
and that flaring groups are characterized by longer lifetimes than
non-flaring ones.
---------------------------------------------------------
Title: An IDL procedure to determine the inclination of loops in a
solar image .
Authors: Contarino, L.; Romano, P.; Zuccarello, F.
2006MSAIS...9...94C Altcode:
The physics of solar loops is quite complex: there are several
aspects, like their stability, heating and interaction, which have
been deeply analyzed, but that still deserve further investigation. In
this framework, the determination of loops geometric parameters in
a coronal image can be very important. Therefore, in order to give a
contribution to this question, we have elaborated an IDL procedure,
based on a method developed by \cite{Lough}, which allows us to
determine in a TRACE image the loop orientation and inclination on the
solar surface. The procedure is based on the following assumptions:
1) both loop footpoints can be determined; 2) the loop central axis
lies in a plane; 3) the loop is symmetrical about its central axis.
---------------------------------------------------------
Title: Atmospheric Pressure Anomalies Recorded on Italian Volcanoes:
Possible Relationships With Solar Activity
Authors: Madonia, P.; Gurrieri, S.; Inguaggiato, S.; Giugliano, P.;
Romano, P.; Spadaro, D.; Zuccarello, F.
2005AGUFM.A43C0118M Altcode:
Hourly data of atmospheric pressure are normally recorded in Italian
active volcanoes (Etna, Vesuvius, Stromboli), for environmental and
volcanic hazard monitoring purposes, in ground station networks managed
by the Italian National Institute for Geophysics and Volcanology
(INGV) and Vesuvius National Park. The common characteristic of the
three networks is the presence of two stations, located the lower
in the altitude range 0-300, the higher in the range 1000-1300 m,
that in the cases of Vesuvius and Stromboli coincide with the top of
the volcanoes. Data recorded during the years 2003-2004 have been
first analyzed in order to looking for anomalies due to volcanic
activities. The main result of the preliminary data analysis was
the identification of two main anomalies, not directly linked to
volcanic activity, occurred at the same time on the three volcanoes
at least in two different episodes in the periods September-October,
2003 and July-August, 2004. The main characteristics of the anomalies
was a decoupling of the signal recorded at sea level respect that
one recorded at higher altitudes, evidenced by a dramatic lowering of
the correlation coefficients calculated, on weekly basis, between the
hourly values of atmospheric pressure. These anomalies appear to be
strongly correlated with the level of solar activity, as determined
by the values of the electromagnetic index Kp and of the Wolf number,
the latter one calculated from the sunspot data daily acquired at the
Catania Astrophysical Observatory of the Italian National Institute
for Astrophysics.
---------------------------------------------------------
Title: AFS dynamics in a short-lived active region
Authors: Zuccarello, F.; Battiato, V.; Contarino, L.; Romano, P.;
Spadaro, D.; Vlahos, L.
2005A&A...442..661Z Altcode:
In the framework of the study on active region emergence, we report the
results obtained from the analysis of the short-lived (7 days) active
region NOAA 10407. The data used were acquired during an observational
campaign carried out with the THEMIS telescope in IPM mode in July 2003,
coordinated with other ground- and space-based instruments (INAF-OACT,
DOT, BBSO, MDI/SOHO, EIT/SOHO, TRACE). We determined the morphological
and magnetic evolution of NOAA 10407, as well as the velocity fields
associated with its magnetic structures. Within the limits imposed by
the spatial and temporal resolution of the images analyzed, the first
evidence of the active region formation is initially observed in the
transition region and lower corona, and later on (i.e. after about 7
h) in the inner layers, as found in a previous analysis concerning a
long-lived, recurrent active region. The results also indicate that
the AFS formed in the active region shows typical upward motion at
the AFS's tops and downward motion at the footpoints. The velocity
values relevant to the upward motions decrease over the evolution
of the region, similarly to the case of the recurrent active region,
while we notice an increasing trend in the downflow velocity during
the early phases of the time interval analyzed by THEMIS. On the other
hand, the AFS preceding legs show a higher downflow than the following
ones, a result in contrast with that found in the long-lived active
region. The chromospheric area overhanging the sunspot umbra shows an
upward motion of ∼ 2 km s<SUP>-1</SUP>, while that above the pores
shows a downward motion of ~4 km s<SUP>-1</SUP>.
---------------------------------------------------------
Title: Observational evidence of the primary role played by
photospheric motions in magnetic helicity transport before a filament
eruption
Authors: Romano, P.; Contarino, L.; Zuccarello, F.
2005A&A...433..683R Altcode:
Many filament eruptions can be suitably described in the framework
of the kink instability model, although it is not always easy to
discriminate whether the helical flux rope writhes due to new emerging
flux or to photospheric horizontal motions. In this paper we provide
observational evidence of the important role which can be played by
horizontal motions in filament instability and eruption. More precisely,
we describe the analysis of the eruption of a reverse-S-shaped filament
associated with a flare of class M6.3, that occurred on 15 June, 2001
in the active region NOAA 9502. Using TRACE 195 Åimages we studied
the morphological evolution of the EUV filament channel. Using 1 minute
cadence MDI full-disc longitudinal magnetograms we analyzed the magnetic
evolution of the entire active region. The geometrical parameters of
the EUV filament channel and the horizontal velocities in the areas
corresponding to the filament footpoints were determined and agreed
with the kink instability. Moreover, the analysis of MDI magnetograms
showed that a sudden and strong increase in the magnetic helicity
transport rate to the corona preceded and accompanied the filament
eruption. During the same time interval, on the one hand the emergence
of magnetic flux in both polarities became negligible, but on the
other hand the velocity pattern at the filament ends showed horizontal,
counterclockwise motions, which could make a significant contribution
to the transformation, from twist to writhe, of the magnetic helicity
accumulated along the filament before its eruption. This result seems to
indicate that in this event the transport of magnetic helicity exceeding
the limit for the kink instability is primarily due to photospheric
motions, while the contribution from the emerging flux is negligible.
---------------------------------------------------------
Title: Global warming: solar variability and energy consumption
Authors: Nigro, A.; Pagano, A.; Zuccarello, F.
2005MmSAI..76.1015N Altcode:
Recent measurements support evidence for short-term global warming of
the earth's surface. The average trend of the earth's surface anomaly
as a function of the time was fitted by a simple thermodynamical
model including short-term variation of the solar irradiance as well
as anthropogenic forcing.
---------------------------------------------------------
Title: AFS dynamic evolution during the emergence of an active region
Authors: Spadaro, D.; Billotta, S.; Contarino, L.; Romano, P.;
Zuccarello, F.
2004A&A...425..309S Altcode:
Using data acquired during an observational campaign carried out at
the THEMIS telescope in IPM mode, coordinated with other ground- and
space-based instruments (IOACT, TRACE, EIT/SOHO, MDI/SOHO), we have
analyzed the first evolutionary phases of a recurrent active region
(NOAA 10050), in order to study the morphology and dynamics of its
magnetic structures during their emergence and early development. The
main result obtained from this analysis concerns the dynamic evolution
of the arch filament system (AFS) crossing the polarity inversion line:
the line of sight velocities determined from Doppler measurements
confirm that the loops forming the AFS show an upward motion at their
tops and a downward motion at their extremities, but also indicate that
the upward motion decreases while the active region develops. Moreover,
it has been found that, within the limits of the temporal cadence
and spatial resolution of the instruments used, the first evidence of
the active region formation is initially observed in the transition
region and lower corona, and later on (i.e. after about 6 h) in the
inner layers (chromosphere and photosphere). Another interesting
result concerns the analysis of the magnetograms, indicating that the
initial increase in the magnetic flux seems to be synchronous with the
appearance od the active region appearance in the transition region
and lower corona, and that the rate of increase of the magnetic flux
during the formation of the active region is not constant, but is
steeper at the beginning (i.e. during the first 150 h) than in the
following period. All these results may indicate the presence of some
mechanism that decelerates the magnetic flux emergence as more and
more flux tubes rise towards higher atmospheric layers. Finally, we
would like to stress the observed asymmetries between the preceding
and the following sides of NOAA 10050: the p-side is more extented
than the f-side, the p-side moves forward from the initial outbreak
position much faster than the f-side recedes; the AFS f-side exhibits
higher downflows than the p-side.
---------------------------------------------------------
Title: Magnetic helicity transport in corona and filament eruptions
Authors: Romano, P.; Contarino, L.; Zuccarello, F.
2003SoPh..218..137R Altcode:
Using a 28-hour time series of line-of-sight magnetograms taken
by the Michelson Doppler Imager (MDI), we determined the magnetic
flux variations and the rate of magnetic helicity transport at the
footpoints of a filament in active region NOAA 8375. The filament was
characterized by a positive helicity change due to shearing motions
in both footpoints and showed several partial eruptions during the
observing time. In particular, we considered 4 events registered in
the Hα daily reports of Solar Geophysical Data. We found a strong
temporal correlation between filament eruptions and helicity transport
from the photospheric magnetic structures at the filament footpoints
into the corona: in at least one footpoint, all of the events were
preceded by an evident increase and followed by a small decrease of
the emerging magnetic flux and of the magnetic helicity change due to
shearing motions. We compared these two mechanisms of helicity transport
and found that the predominant role to drive filament instability is
played by emergence of new magnetic flux from the convection zone.
---------------------------------------------------------
Title: Themis, BBSO, MDI and trace observations of a filament eruption
Authors: Contarino, L.; Romano, P.; Yurchyshyn, V. B.; Zuccarello, F.
2003SoPh..216..173C Altcode:
We describe a filament destabilization which occurred on 5 May 2001 in
NOAA AR 9445, before a flare event. The analysis is based on Hα data
acquired by THEMIS operating in IPM mode, Hα data and magnetograms
obtained at the Big Bear Solar Observatory, MDI magnetograms and 171 Å
images taken by TRACE. Observations at 171 Å show that ∼ 2.5 hours
before the flare peak, the western part of the EUV filament channel
seems to split into two parts. The bifurcation of the filament in the
Hα line is observed to take place ∼ 1.5 hours before the flare peak,
while one thread of the filament erupts ∼10 min before the peak of
the flare. Our analysis of longitudinal magnetograms shows the presence
of a knot of positive flux inside a region of negative polarity, which
coincides with the site of filament bifurcation. We interpret this
event as occurring in two steps: the first step, characterized by the
appearance of a new magnetic feature and the successive reconnection
in the lower atmosphere between its field lines and the field lines
of the old arcade sustaining the filament, leads to a new filament
channel and to the observed filament bifurcation; the second step,
characterized by the eruption of part of the filament lying on the
old PIL, leads to a second reconnection, occurring higher in the corona.
---------------------------------------------------------
Title: Angular velocity during the cycle deduced using the sunspot
group age selection methodology
Authors: Zuccarello, F.; Zappalá, R. A.
2003AN....324..464Z Altcode:
We have used the "age selection methodology" (ASM) (Zappalá and
Zuccarello 1991) to study the variability of the sunspot groups angular
velocity during the activity cycle. The ASM allows us to separate the
contribution of Young Sunspot Groups (YSG) from that of Recurrent ones
(RSG) in the Ω (θ) determination and therefore to evaluate whether
the increase in angular velocity during minima (reported in literature
using all sunspot groups as tracers), is due to a greater statistical
weight of YSG on RSG or whether it reflects a global characteristic of
the Sun. The results obtained from the analysis of sunspot groups data
collected during the period 1874-1981 (Greenwich Photoheliographic
Results) indicate that during minima, besides the fact that the
percentage of RSG drops to <= 5%, both YSG and RSG show the same
increase in angular velocity, i.e. 0.16 degrees/day. Comparing our
results with those reported in literature and taking into account
the internal angular velocity as deduced by p-mode oscillations, it
is possible to conclude that the observed higher angular velocity of
the Sun during minima concerns several layers of the Sun.
---------------------------------------------------------
Title: Eruption of a helically twisted prominence
Authors: Romano, P.; Contarino, L.; Zuccarello, F.
2003SoPh..214..313R Altcode:
In this paper we analyze the eruption of a prominence, characterized
by a helical-like structure and by a non-linear rising motion. We
approximated the prominence as a cylindrical curved flux tube and
estimated the behaviour of several geometrical parameters during the
activation and the eruption phases. We determined that, at the onset
of the activation, the number N of turns of a magnetic field line over
the whole length of the prominence was ∼5.0, while the value of the
ratio P/r<SUB>0</SUB> between the pitch of the magnetic field lines and
the prominence width was ∼0.45. These values are in good agreement
with those predicted by the kink-mode instability. Moreover, we found
a decrease of the total twist of one helical thread from Φ∼10π to
Φ∼2π during the prominence eruption, indicating a relaxation of the
magnetic field towards a less twisted configuration. We conclude that
the prominence was initially destabilized by the kink-mode instability
and, not succeeding in finding a new equilibrium configuration,
it erupted.
---------------------------------------------------------
Title: Flare activity in solar active region 8421 observed by the
TRACE satellite
Authors: Zuccarello, F.; Contarino, L.; Romano, P.; Priest, E. R.
2003A&A...402.1085Z Altcode:
Due to the wide range of wavelengths examined and to the high angular
and temporal resolution, TRACE allows one to carry out a spatial and
temporal analysis of active regions during highly transient phenomena
such as flares. This provides new input to the study of the mechanisms
involved in these phenomena. We have studied 3 flares that occurred in
AR 8421 between 29 and 30 December 1998 by comparing white light, 1600
Å, and 171 Å images obtained by TRACE with BBSO H<SUB>alpha </SUB>
images, Mitaka magnetograms and Yohkoh hard X-ray data. The flares,
characterized by sudden intensity enhancements in EUV loops and by
moss brightenings, have been interpreted in the framework of the two
canonical flare models: i.e. simple loop and two ribbon flares. Our
analysis has shown that flare No. 1 may be interpreted as a two-ribbon
flare triggered by reconnection between a sheared arcade and a new
emerging flux tube. The analysis of flare No. 2 strongly supports the
model of two-ribbon flares characterized by reconnection occurring
at higher and higher levels as time proceeds. Finally, the analysis
of flare No. 3 has given the opportunity to relate moss brightening
with a probable process of chromospheric evaporation.
---------------------------------------------------------
Title: A process of low-lying magnetic reconnection observed by
THEMIS, BBSO and TRACE
Authors: Contarino, L.; Romano, P.; Zuccarello, F.; Yurchyshyn, V. B.
2003MmSAI..74..647C Altcode:
We describe the results obtained from the study of a filament eruption
associated to a two-ribbon flare, occurred in NOAA AR 9445 on May 5,
2001. We interpret the event in a two-step reconnection scenario. The
first reconnection takes place in the lower atmosphere and is due to a
slow, but continuous, magnetic flux cancellation near the filament. The
second reconnection, which is explosive and takes place in the corona,
is caused by the eruption of the filament which triggers a two-ribbon
flare. The analysis is based on Hα data acquired by THEMIS operating
in IPM mode, Hα data and magnetograms obtained at the Big Bear Solar
Observatory, and 171 Å images taken by TRACE.
---------------------------------------------------------
Title: The impact of the spotgroup age and lifetime on their
capability of hosting M and X flares
Authors: Ternullo, M.; Contarino, L.; Romano, P.; Zuccarello, F.
2003MmSAI..74..615T Altcode:
The present study originates in the framework of a Flare Warning
Campaign carried on at the INAF Catania Astrophysical Observatory
(OACt) and aimed at getting the capability of predicting the
occurrence of the potentially most dangerous flares. The analysis is
based on sunspot-groups data collected at OACt and on M and X flare
data collected by GOES 8 during the period 1998 - 2002. Evidence is
found that: i) M and X flares tend to replicate in a small sample of
spotgroups (≈ 10% total); ii) the spotgroups hosting flares live
significantly longer than the others. The predictive value of these
findings is stressed.
---------------------------------------------------------
Title: Angular velocity of sunspot-groups during the activity cycle
deduced using the age selection methodology
Authors: Zuccarello, F.; Zappalá, R. A.
2003MmSAI..74..619Z Altcode:
Using Greenwich Photoheliographic Results collected during the period
1874-1981 and the Age Selection Methodology (\citet{Zappa-Zucca}), we
have studied the variability of the sunspot-groups angular velocity in
different phases of the activity cycle. The results indicate that during
minima, all sunspot-groups, independently of their age, show the same
increase in angular velocity, i.e. ~ 0.16 degrees/day. Comparing our
results with those regarding the internal angular velocity as deduced
by p-mode oscillations, it is possible to conclude that the observed
higher angular velocity during minima concerns several layers beneath
the solar photosphere.
---------------------------------------------------------
Title: Instability analysis of an active prominence
Authors: Romano, P.; Contarino, L.; Zuccarello, F.
2003MmSAI..74..651R Altcode:
Using EUV images aquired by TRACE, we analysed the eruption of a
prominence, occurred on July 19, 2000 in the Active Region NOAA
9077. We approximated the prominence to a cylindrical curved flux
tube and estimated the behaviour of several geometrical parameters
during the activation and the eruption phases. We found a decrease
in the total twist of one helical thread from Phi ~ 10 pi to Phi ~
2 pi during the prominence eruption, indicating a relaxation of
the magnetic field towards a more stable configuration. Moreover we
determined that, at the onset of the activation, the number N of turns
of a magnetic field line over the whole length of the prominence was ~
5.0, while the value of the ratio P/r<SUB>0</SUB> between the pitch
of the magnetic field lines and the prominence width was ~ 0.45,
in agreement with the kink mode instability.
---------------------------------------------------------
Title: 3rd national meeting on the Italian solar research : Vulcano,
Isole Eolie, Italy, 30 September-4 October, 2002
Authors: Zuccarello, Francesca; Spandaro, Daniele; Ventura, Rita
2003MmSAI..74.....Z Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Changes in magnetic field topology and current intensity
during a filament eruption
Authors: Romano, P.; Contarino, L.; Zuccarello, F.
2002ESASP.506..733R Altcode: 2002ESPM...10..733R; 2002svco.conf..733R
Using images taken by the BBSO telescope and the TRACE satellite,
we have examined a prominence eruption occurred in AR 9077 at the
west limb of the Sun, on July 19th, 2000. We have followed the
morphological evolution of the prominence several hours before its
activation and during the eruption phase. Assuming that the filament
may be approximated as a cylindrical flux tube initially anchored in the
solar surface and taking into account the different inclinations of the
filament axis compared to the solar surface, we have determined several
geometrical and physical parameters. The results of this analysis
indicate that, after an initial phase of constant velocity eruption,
the filament seems to oscillate and then it starts to rise again towards
higher levels till when the plasma is ejected. Moreover, it has been
possible to determine a decrease in the twist of the prominence magnetic
field and to infer the behaviors of the axial electric current and of
the filament total mass over time. The implications of these results
in the framework of a screw-instability is briefly discussed.
---------------------------------------------------------
Title: Optical and EUV observation of a filament destabilization
and pre-eruption reconnection
Authors: Contarino, L.; Romano, P.; Zuccarello, F.; Yurchyshyn, V. B.
2002ESASP.506..573C Altcode: 2002ESPM...10..573C; 2002svco.conf..573C
Filament eruption occurring prior to solar flares or CME may be
related to changes in the magnetic field structure in and around
the filament. In particular, when the magnetic field topology is
characterized by great complexity, or new magnetic flux emerges in
the surrouding of the main arcade supporting the filament, a so-called
pre-eruption reconnection is likely to take place. In this framework,
using both ground-based (THEMIS and BBSO) and satellite (TRACE)
images and BBSO magnetograms, we have followed a filament eruption
occurred in AR 9445 on May 5, 2001, before a two-ribbon flare. Our
analysis has shown that the event was characterized by the following
steps: a) presence of a knot of positive polarity inside the region of
negative polarity where the arcade loops were anchored; b) appearance
of a bright knot in Hα images at the same location where the positive
polarity knot was observed; c) spread of the filament into two threads
and bifurcation near the Hα bright knot; d) eruption of part of the
filament and two-ribbon flare; e) EUV post-flare loops anchored in a
region near the Hα bright knot. The interpretation of these phenomena
in terms of a pre-eruption, low-lying magnetic reconnection, followed
by a post-eruption, high-lying reconnection, is discussed.
---------------------------------------------------------
Title: A statistical analysis on sunspot-groups correlated to M and
X flares
Authors: Ternullo, M.; Contarino, L.; Romano, P.; Zuccarello, F.
2002ESASP.506.1045T Altcode: 2002svco.conf.1045T; 2002ESPM...10.1045T
Very energetic flares and Coronal Mass Ejections may have important
consequences on Space Weather and Earth magnetosphere. In the last
years, thanks to theoretical modelling, ground based and satellite
observations, the comprehension of flares and CME has greatly
improved. Nevertheless, it is not yet possible to surely forecast
whether and when an active region may give rise to these events. In this
context, we have focussed our attention on the possibility to identify
the most favourable conditions an active region must develop in order
to be flare-productive. We have therefore used data on sunspot-groups
(INAF-Catania Astrophysical Observatory and NOAA reports) during the
period January 1998 - April 2002, and data on very energetic flares
(M and X) obtained in the soft X-ray range by GOES 8, in order to
define the characteristics of several parameters which may indicate
whether an active region is going to produce a flare.
---------------------------------------------------------
Title: A statistical approach to the spot-flare connection
Authors: Ternullo, M.; Zuccarello, F.; Contarino, L.; Romano, P.
2002ESASP.505..591T Altcode: 2002IAUCo.188..591T; 2002solm.conf..591T
Very energetic flares and CME may strongly influence Space Weather and
Earth environment. In the last years, there has been growing interest
in the possibility of forecasting flare occurrence, in order to reduce
damages to spacecraft, satellite positioning systems and effects on
RF communications. In this context, we have carried out a statistical
analysis on a number of parameters characterizing sunspot-groups,
hosting very energetic flares. We have used data on sunspot-groups, a
part collected at INAF-Catania Astrophysical Observatory during 1998 -
2002 and a part deduced by NOAA reports, together with data on M and X
flares obtained by GOES 8 in the soft X-ray range. The results obtained
by this analysis may contribute to a better knowledge of the flare
phenomenon and could improve the capabilities of Flare Warning Services.
---------------------------------------------------------
Title: Development of a filament eruption during a solar flare
Authors: Romano, P.; Contarino, L.; Zuccarello, F.
2002ESASP.505..553R Altcode: 2002IAUCo.188..553R; 2002solm.conf..553R
Using BBSO Hα images and TRACE data, we have studied a prominence
eruption occurred on July 19th, 2000, in active region 9077, at the
west limb of the Sun. We have followed the morphological evolution
of the prominence several hours before its activation and during the
eruption phase, in different atmospheric layers. In particular, TRACE
images showed that the prominence had a helical-like structure and that
its motion towards higher atmospheric layers was characterized by a
non-linear behaviour. We approximated the prominence as a cylindrical
flux tube and estimated the evolution of the twist of the prominence
magnetic field and the behaviour of the rise speed during different
phases. Taking into account the forces acting on the prominence, we
determined the decrease of the axial electric current and the rate of
mass loss of the prominence.
---------------------------------------------------------
Title: Analysis of high resolution and full disk solar images
Authors: Berrilli, F.; Caccin, B.; Cantarano, S.; Egidi, A.; Penza,
V.; Criscuoli, S.; del Moro, D.; Pietropaolo, E.; Consolini, G.;
Ermolli, I.; Lepreti, F.; Mainella, G.; Severino, G.; Zuccarello, F.
2001ESASP.493..173B Altcode: 2001sefs.work..173B
No abstract at ADS
---------------------------------------------------------
Title: Coordinated space and ground-based observations of rapidly
evolving active regions
Authors: Zuccarello, F.; Cacciani, A.; Contarino, L.; Romano, P.
2001ESASP.493..439Z Altcode: 2001sefs.work..439Z
No abstract at ADS
---------------------------------------------------------
Title: Description of a Procedure to Analyze EUV Loops
Authors: Zuccarello, F.; Contarino, L.; Romano, P.
2001SoPh..199...97Z Altcode:
We have developed an IDL procedure to analyze spatial and time evolution
of loops observed in the outer solar atmosphere by EUV instruments. The
use of this procedure, based on the assumption that loop portions
have cylindrical symmetry, allows automatic processing of sequences
of images. Our work mainly aims to describe spatial and temporal
variations of brightness along the loop length and to determine
the following physical parameters: emission measure EM, electron
density N<SUB>e</SUB>, pressure P, thermal energy E<SUB>th</SUB>,
radiative cooling time τ<SUB>rad</SUB>, and conductive cooling time
τ<SUB>cond</SUB>. In this paper we describe an application of this
procedure to a sequence of TRACE images at 171 Å, in order to study
loop interaction during a flare that occurred in AR 8421 on 29 December
1998 at 09:41 UT.
---------------------------------------------------------
Title: Evolution of solar flares observed by TRACE
Authors: Zuccarello, F.; Contarino, L.; Romano, P.
2001MmSAI..72..579Z Altcode:
The study of the mechanisms involved in solar flares has a remarkable
importance not only in the framework of the comprehension of
transient phenomena, but also in the context of the coronal heating
question. Several authors have in fact suggested that the solar corona
might be heated by the same mechanism which causes flares, i.e. the
magnetic reconnection. In this framework we have analyzed several
images obtained by TRACE satellite at 171, 1600 Å and WL in order to
emphasize possible signatures of reconnection in I class loops. The
images analyzed concern 5 flares occurred in active region AR 8421
between 29 and 30 December 1998.
---------------------------------------------------------
Title: Solar Patrol at Catania Astrophysical Observatory
Authors: Contarino, L.; Romano, P.; Ternullo, M.; Zappala, R. A.;
Zuccarello, F.
2000ESASP.463..639C Altcode: 2000sctc.proc..639C
No abstract at ADS
---------------------------------------------------------
Title: TRACE Observation of a Flare Triggered by the Interaction of
Class I Loops
Authors: Zuccarello, F.; Romano, P.
1999ESASP.448..907Z Altcode: 1999ESPM....9..907Z; 1999mfsp.conf..907Z
No abstract at ADS
---------------------------------------------------------
Title: Diverging magnetic arcades and antiparallel currents
Authors: Zuccarello, F.; Vinci, A.; Hofmann, A.
1998MmSAI..69..715Z Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Changes in sunspots angular velocity and phase of the solar
cycle
Authors: Zuccarello, F.; Zappalá, R. A.
1998MmSAI..69..591Z Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Energetics of chromospheric-coronal active regions
Authors: Zuccarello, F.; Zappalá, R. A.
1998MmSAI..69..685Z Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Elemental abundances in the solar network and cell centers
from EUV spectra.
Authors: Spadaro, D.; Zuccarello, F.; Zappala, R. A.
1996A&A...308..970S Altcode:
In order to search for empirical evidences in the transition region
and corona explaining the observed variability of the chemical
composition in the solar wind, we have used a set of EUV average
spectra in the 296-1350A wavelength range (Vernazza & Reeves
1978), to determine the relative abundances of C, N, O, Ne, Mg, Si,
S in the cell centers and the network within a coronal hole and a
quiet region, respectively. Moreover, we have determined the relative
abundances in an active region during two periods characterized by
different activity levels. The analysis has shown that the elemental
abundances appear in broad agreement with the photospheric ones for
all the different regions examined. Moreover, within the coronal hole
and the quiet region, the chemical composition in the cell centers
does not differ appreciably from that in the network. Further, no
differences in the elemental abundances have been found in the active
region during the two considered phases. Nevetherless, we point out
that the data used in this analysis for a given kind of structures,
are composed by spectra taken at various times and positions within
the same region, so that eventual differences may be smoothed out
by temporal and spatial averages. We discuss the implications of the
results concerning the cell centers and the network for the ion-neutral
separation model suggested by Meyer (1991).
---------------------------------------------------------
Title: Coronal loops and their modeling (review)
Authors: van den Oord, G. H. J.; Zuccarello, F.
1996IAUS..176..433V Altcode:
No abstract at ADS
---------------------------------------------------------
Title: On the Role Played by Peculiar Photospheric Motions on
Force-Free Magnetic Arcades
Authors: Zuccarello, F.
1994emsp.conf...39Z Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Rotation Rates of Sunspots with Different Lifetimes
Authors: Zuccarello, F.
1994emsp.conf...43Z Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Influence of the lifetime parameter on the rotation rate
of sunspots
Authors: Zuccarello, F.
1993A&A...272..587Z Altcode:
Recent investigations on the photospheric angular velocity pattern
have shown that young and short- living tracers show rotation rates
higher than those determined both by older tracers and by photospheric
plasma. <P />As a direct relationship between the age of the tracer
and the angular velocity determination has been found (Zappalà &
Zuccarello 1991), it seemed very interesting to investigate whether
also the "lifetime" parameter might have a role on angular velocity
determinations. <P />We have therefore analyzed the sunspot-group data
reported in the Greenwich Photoheliographic Results during the 1874-1976
period. 9000 objects were selected as young sunspot-groups (YSG) and,
using the lifetime parameter as selecting rule, we could catalogue 4463
objects having a lifetime between 2 and 10 d. <P />The rotation rate
of these objects as a function of their lifetime was calculated and
the results obtained may be summarized in the following main points:
<P />1. Independently of their lifetime, sunspots rotate during the
first 2-3 days of life in the photosphere, at a higher rate than
that of recurrent sunspots. <P />2. Sunspots with a lifetime ranging
from 2 to 8 d are more efficiently decelerated than YSG, while 11-day
living sunspots are less efficiently decelerated. <P />3. Sunspots in
the equatorial belt (0-10°) having a lifetime comparable to that of
supergranule cells, rotate slower than the cells themselves. <P />4. The
angular velocity measured during the last day of life is lower both than
that of YSG and than that deduced by sunspots which disappear the day
after. <P />These results have been analyzed in the scenario of the
sunspots cluster model ( 1987). According to the conclusions drawn,
the initial higher angular velocity of young and short-living sunspots
is not a function of the cluster "aggregation capability"; the rate of
rise of the merging level through the convection zone is influenced by
(or influences) the ability of the cluster to keep coalesced; finally,
when the merging level rises too fast, the sunspot dissolves.
---------------------------------------------------------
Title: Peculiar photospheric velocity fields and magnetic energy
build-up
Authors: Zuccarello, F.
1992A&A...257..298Z Altcode:
The in situ storage of magnetic energy was studied in a linear
force-free arcade sheared by a relative velocity between its
footpoints. The photospheric velocity fields used are related to
sunspots proper motions and to the solar differential rotation
pattern. Results indicate that sunspot proper motions are efficient
in magnetic energy build-up and that the values of the stored magnetic
energy in a region characterized by rigidly rotating structures coupled
with new born sunspots may be sufficient to allow flaring activity. It
is concluded that the anomalies in the solar angular velocity pattern
may have an important role in the magnetic energy build-up.
---------------------------------------------------------
Title: Angular momentum transport by Reynolds stresses determined
from the analysis of 100-year sunspot motions and its variations
with solar cycle
Authors: Paterno, L.; Zuccarello, F.; Spadaro, D.; Zappala, R. A.
1991A&A...252..337P Altcode:
Some aspects of the latitudinal momentum transport by Reynolds
stresses, as deduced from the analysis of the Greenwich sunspot data
for the period 1874-1976 by using only very young sunspot groups (age
equal to or less than 3 d), were investigated in order to study the
equatorial acceleration maintenance and its possible correlations with
the equatorial angular velocity time variations and the solar cycle. The
results, which are consistent with those of previous authors, indicate
the presence of a net angular momentum flux toward the equator which
is more vigorous at higher latitudes, and sufficient on average to
maintain the observed equatorial acceleration. The angular momentum
transport time variations show a significant periodicity correlated
with the solar cycle. Also, the equatorial velocity time variations
show significant periodicities, which in turn may depend on the
angular momentum transport time variations. The scenario which emerges
from these results is discussed in the framework of the theories of
differential rotation and activity cycle.
---------------------------------------------------------
Title: Angular velocities of sunspot-groups and solar photospheric
rotation
Authors: Zappala, R. A.; Zuccarello, F.
1991A&A...242..480Z Altcode:
From the analysis of the Greenwich Photoheliographic Results
sunspot-groups data from 1874 to 1976, it has been found that the
sunspot-groups angular velocity is not invariant with time during
the first 2.5 x 10 to the 6th s of their life, showing a nonrandom
negative acceleration. More precisely, 2-day-old sunspot-groups have,
at all the latitude strips, angular velocities which are, on average,
0.3 degrees/day higher than recurrent sunspots. Moreover, the angular
velocity difference between sunspot-groups of age less than 860,000
s and recurrent sunspots decreases with time, and after 2 rotations,
the angular velocity is almost equal to the plasma velocity. On the
basis of these results, the problem of the determination of the solar
photospheric rotation has been reexamined. The implications of a higher
angular velocity of young tracers on the subphotospheric layer rotation
are discussed.
---------------------------------------------------------
Title: Energy storage in solar loops by footpoint motions
Authors: Zappala, R. A.; Zuccarello, F.
1989A&A...214..369Z Altcode:
The amount of stored magnetic energy in an arcade, sheared by
footpoint motions due to the relative velocity of young and recurrent
sunspot groups (RSG), has been evaluated in the force-free-field
approximation. The relative velocity (Delta v) between young and
RSG and the time scales during which this Delta v lasts have been
estimated from the analysis of sunspot data reported in the Greenwich
Photoheliograhic Results for the years 1874-1976. Using shearing times
from 86,000-260,000 sec and Delta v of 2940-3470 cm/sec, it is found
that the stored energy may be (1-1000) x 10 to the 30th ergs. The
consequences of these results, concerning the phase of energy build-up
for loop heating and for transients are discussed.
---------------------------------------------------------
Title: Relative velocity of photospheric magnetic regions and energy
input in the coronal loops
Authors: Zappala, R. A.; Zuccarello, F.
1989MmSAI..60..161Z Altcode:
The differences in the angular velocity between young and recurrent
sunspot groups observed for the years 1874-1976 are used here to
evaluate, in the force-free field approximation, the amount of stored
magnetic energy in an arcade sheared by footpoint motions due to the
relative velocities of the sunspot groups. The range of energy goes
from 10 to the 30th to 10 to the 33rd ergs.
---------------------------------------------------------
Title: Elemental abundances in different solar regions from EUV
observations
Authors: Noci, G.; Spadaro, D.; Zappala, R. A.; Zuccarello, F.
1988A&A...198..311N Altcode:
The relative abundances of C, N, O, Ne, Mg, Si, S in different regions
of the solar transition zone (a coronal hole, a quiet and an active
region) have been determined from the analysis of average EUV spectra
in the range 296-1350 A. The methodology described by Pottasch (1964)
and later on improved (Dupree, 1972; Withbroe, 1981) has been used;
moreover, the role played by the population of the metastable levels
of the emitting ions has been taken into account. The abundances found
in different regions and those found at the photospheric level do not
differ more than the errors, except for oxygen, whose abundances seem
to be lower for values of T less than 10 exp 5.2 K, particularly in
the active region. The comparison between quiet region and coronal
hole shows that their chemical compositions differ by values much
lower than the estimated uncertainty, which suggests that the errors
affecting the abundance determinations are lower than estimated. This
could imply that differences in the chemical composition between active
region and other coronal regions exist.
---------------------------------------------------------
Title: Varying self-inductance and energy storage in a sheared
force-free arcade
Authors: Zuccarello, F.; Burm, H.; Kuperus, M.; Raadu, M.; Spicer,
D. S.
1987A&A...180..218Z Altcode:
The authors utilize an electric circuit analogy to model the build-up
and storage of magnetic energy in the coronal loops known to exist
in the atmosphere of the Sun. The parameterization of magnetic energy
storage in an electric circuit analogue uses a bulk current I flowing
in the circuit and a self-inductance L. Because the self-inductance is
determined by the geometry of the magnetic configuration any change in
its dimensions will change L. If L is increased, the amount of magnetic
energy stored and the rate at which magnetic energy is stored are both
increased. One way of increasing L is to shear the magnetic field lines
and increase their effective geometrical length. Using the force-free
field approximation for a magnetic arcade whose field lines are sheared
by photospheric motions, the authors demonstrate that the increase
of magnetic energy is initially due to the increase of the current
intensity I and later mainly due to the increase of the self-inductance.
---------------------------------------------------------
Title: Footpoint Motions and Energy Storage in the Sun
Authors: Zappala, R. A.; Zuccarello, F.
1986mrt..conf..159Z Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The role of differential rotation in magnetic energy storage.
Authors: Zappala, R. A.; Zuccarello, F.; Kuperus, M.
1984ESASP.220..159Z Altcode: 1984ESPM....4..159Z
The authors investigate a possible mechanism for magnetic energy
storage in coronal loops without making assumptions about dissipative
mechanisms.
---------------------------------------------------------
Title: X-ray emission of late-type stars
Authors: Paterno, L.; Zuccarello, F.
1983ApJ...275L...1P Altcode:
A theoretical estimate of the dependence of the X-ray coronal flux
from late-type stars on stellar parameters is given and compared with
observations. The theoretical approach is based on the assumptions
that magnetic energy in coronal loops is converted into thermal energy
and that the amplitude of the emerging magnetic field generated in
the deepest part of the convection zone by an (alpha)(omega)-dynamo
mechanism is limited by buoyancy. Using simple physics, an approximate
relationship is derived linking the X-ray surface flux to the mass,
the angular velocity of rotation, and the depth of the convection
zone of the star. When this relationship is calibrated with the sun,
the theory predicts a trend in agreement with observations, except
for K stars, within the uncertainties of the measured rotational
velocities. Rotation, convection, and magnetic field appear, therefore,
to be the basic ingredients of the X-ray coronal emission from
late-type stars.
---------------------------------------------------------
Title: Flow in Coronal Loops with a Mass Source
Authors: Noci, G.; Zuccarello, F.
1983SoPh...88..193N Altcode:
This research studies the flow of plasma inside a coronal loop in which
an injection of plasma through the lateral surface is permitted. The
flow is assumed steady and polytropic.
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Title: Basic parameters determining X-ray emission level in stars
of spectral type later than F5
Authors: Paterno, L.; Zuccarello, F.
1983ASSL..102..633P Altcode: 1983ards.proc..633P; 1983IAUCo..71..633P
An attempt is made to estimate the importance of certain stellar
parameters for the X-ray emission from stars possessing outer convective
envelopes. The dependence of the average surface magnetic field strength
on the star's rotation and the depth of the convection zone is obtained,
and the X-ray surface flux is plotted against the rotational velocities
for 41 stars.
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Title: Relationship between Photospheric and Chromospheric Ω(θ)
deduced by Temporarily and Spatially Correlated Tracers
Authors: Zappala, R. A.; Zuccarello, F.
1982ASSL...96...71Z Altcode: 1982spls.meet...71Z
An analysis of the spatially and temporally correlated photospheric
and chromospheric features lasting 2-9 days is used to describe the
kinematic characteristics of a young active region in two levels of the
solar atmosphere. Daily K spectrograms served as a basis for an analysis
of faculae occurring from Jan. 1972-Nov. 1977. Consideration was limited
to phenomena of the same age and geometric center-of-mass overlapping
within 2 deg. Daily averages were calculated of the velocities of
the sunspot groups and of the K faculae, using 5 deg latitude strips
for scale, and weighting the calculations for age. Similar behavior
of spatially and temporally correlated tracers indicated a magnetic
linkage exists between two layers in the same active region. Active
regions of different ages displayed different velocities. Data on the
triggering mechanism of solar transients are suggested to be available
from analysis of twisting and shearing due to the motions of sunspots
in different active regions which are magnetically linked.
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Title: The Age-Dependence of Photospheric Tracer Rotation
Authors: Ternullo, M.; Zappala, R. A.; Zuccarello, F.
1981SoPh...74..111T Altcode:
From the analysis of the motions of sunspot groups recorded at
Catania Astrophysical Observatory over a 7-years period from 1972 to
1978 the mean angular velocity as a function of latitude and age is
calculated. The results suggest that the age of photospheric tracer
(sunspot groups) affects the rotation curve slope. The implications
of this result are discussed.
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Title: Solar observations made at Catania Astrophysical Observatory
during 1980.
Authors: D'Arrigo, C.; Zappalà, R. A.; Zuccarello, F.; Catinoto,
E.; Domina, G.; Sciuto, S.; Celeani, G.; Sapienza, G.; Del Bufalo, A.
1981PCat..166.....D Altcode:
No abstract at ADS
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Title: Associazioni di strutture fotosferiche e cromosferiche nei
primissimi stadi evolutivi come traccianti della rotazione solare.
Authors: Paternò, L.; Zappalà, R. A.; Zuccarello, F.
1979RSAI...22..150P Altcode:
No abstract at ADS
