Author name code: mueller-daniel
ADS astronomy entries on 2022-09-14
author:"Mueller, Daniel A."
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Title: Refractory species in the neutral gas coma of comet
67P/Churyumov-Gerasimenko
Authors: Rubin, Martin; Combi, Michael; Gombosi, Tamas; Wurz, Peter;
De Keyser, Johan; Fuselier, Stephen; Altwegg, Kathrin; Wampfler,
Susanne; Haenni, Nora; Berthelier, Jean-Jacques; Dhooghe, Frederik;
Müller, Daniel; Pestoni, Boris R.
Bibcode: 2022cosp...44..265R
Altcode:
For more than 2 years the European Space Agency's Rosetta mission
carried out a close inspection of comet 67P/Churyumov-Gerasimenko. Among
the payload instruments was ROSINA - DFMS, the Rosetta Orbiter
Spectrometer for Ion and Neutral Analysis - Double Focusing Mass
Spectrometer (Balsiger et al. 2007). DFMS was dedicated to measure the
relative and absolute abundances of the neutral gas species present
in the coma. DFMS had a mass resolution that was sufficiently high
to separate refractory elements from organic molecules. When the
comet was at a heliocentric distance of 3 au before perihelion,
DFMS detected the refractory elements sodium, silicon, potassium,
and calcium, which were most likely sputtered off the comet's surface
by impacting solar wind ions (Wurz et al., 2015). However, recent
analysis of the DFMS data revealed the presence of not only these
elements, but also iron, in atomic form also close to perihelion
(Rubin et al., 2021). During that time, the comet was much more
active, with a substantial atmosphere preventing the solar wind from
reaching both the surface of the comet and the dust grains in the
coma near Rosetta (Behar et al., 2017). Our observations are in line
with recent observations of refractory iron and nickel in the gas
phase around more than 20 comets (Manfroid et al., 2021). ROSINA DFMS
failed to detect suitable parents or fragments for these refractory
elements. Therefore, these refractory elements are released directly
in their atomic form from small coma grains and not from a distributed
source of larger molecules. In this presentation we will summarize
these recent findings in the coma of comet 67P/Churyumov-Gerasimenko and
discuss their implications. \vspace{0.5 cm} References Balsiger et al.,
ROSINA - Rosetta Orbiter Spectrometer for Ion and Neutral Analysis,
Sp. Sci. Rev., 128(1), 745-801, 02/2007 Behar et al., The birth and
growth of a solar wind cavity around a comet - Rosetta Observations,
Mon. Not. R. Astron. Soc., 469, S396-S403, 03/2017 Manfroid et al.,
Iron and nickel atoms in cometary atmospheres even far from the Sun,
Nature, 593, 372-374, 05/2021 Rubin et al., Refractory elements in
the gas phase for comet 67P/Churyumov-Gerasimenko, Astron. Astrophys.,
Astron. Astrophys., 658, A87, 12/2021 Wurz et al., Solar Wind Sputtering
of Dust on the Surface of 67P/Churyumov-Gerasimenko, Astron. &
Astrophys., 583, A22, 10/2015
Title: The Magnetic Origin of Solar Campfires: Observations by Solar
Orbiter and SDO
Authors: Panesar, Navdeep Kaur; Zhukov, Andrei; Berghmans, David;
Auchere, Frederic; Müller, Daniel; Tiwari, Sanjiv Kumar; Cheung, Mark
Bibcode: 2022cosp...44.2564P
Altcode:
Solar campfires are small-scale, short-lived coronal brightenings,
recently observed in 174 Å images by Extreme Ultraviolet Imager (EUI)
on board Solar Orbiter (SolO). Here we investigate the magnetic origin
of 52 campfires, in quiet-Sun, using line-of-sight magnetograms from
Solar Dynamics Observatory (SDO)/Helioseismic and Magnetic Imager
(HMI) together with extreme ultraviolet images from SolO /EUI and
SDO/Atmospheric Imaging Assembly (AIA). We find that the campfires
are rooted at the edges of photospheric magnetic network lanes; (ii)
most of the campfires reside above neutral lines and 77% of them appear
at sites of magnetic flux cancelation between the majority-polarity
magnetic flux patch and a merging minority-polarity flux patch, with
a flux cancelation rate of ∼1018 Mx hr‑1; some of the smallest
campfires come from the sites where magnetic flux elements were barely
discernible in HMI; (iii) some of the campfires occur repeatedly
from the same neutral line; (iv) in the large majority of instances
(79%), campfires are preceded by a cool-plasma structure, analogous to
minifilaments in coronal jets; and (v) although many campfires have
"complex" structure, most campfires resemble small-scale jets, dots,
or loops. Thus, "campfire" is a general term that includes different
types of small-scale solar dynamic features. They contain sufficient
magnetic energy (∼1026-1027 erg) to heat the solar atmosphere
locally to 0.5-2.5 MK. Their lifetimes range from about 1 minute to
over 1 hour, with most of the campfires having a lifetime of <10
minutes. The average lengths and widths of the campfires are 5400 ±
2500 km and 1600 ± 640 km, respectively. Our observations suggest that
(a) the presence of magnetic flux ropes may be ubiquitous in the solar
atmosphere and not limited to coronal jets and larger-scale eruptions
that make CMEs, and (b) magnetic flux cancelation, most likely driven
by magnetic reconnection in the lower atmosphere, is the fundamental
process for the formation and triggering of most campfires.
Title: Forming a band with the Solar Orbiter Earth fly - a
multi-mission perspective from the ESA Heliophysics Orchestra
supported by the NASA Heliophyiscs System Observatory
Authors: Taylor, Matthew; Dunlop, Malcolm; Nakamura, Rumi; Horbury,
Tim; Orr, Astrid; Panov, Evgeny; Escoubet, C. Philippe; Luntama,
Juha-Pekka; Eastwood, Jonathan; Müller, Daniel; Zouganelis, Yannis;
Masson, Arnaud; Jiggens, Piers; Walsh, Andrew; Goetz, Charlotte;
Strømme, Anja
Bibcode: 2022cosp...44.1647T
Altcode:
Heliophysics, the science of understanding the Sun and its
interaction with the Earth and the solar system, has a large and active
international community, with significant expertise and heritage in the
European Space Agency (ESA) and Europe. On 27 November 2021, a premier
explorer of this science, the ESA Solar Orbiter spacecraft, carried out
a gravity assist flyby of the Earth, passing within 460 km at closest
approach. At the same time, a number of other spacecraft were continuing
a more regular trajectory evolution in Geospace, including the ESA
Swarm mission and Cluster mission. This trio of missions come from two
different directorates within ESA, although many more have activities
directly connected with Heliophysics. These include the Directorate
of Science, the Directorate of Earth Observation, the Directorate of
Operations, the Directorate of Human and Robotic Exploration and the
Directorate of Technology, Engineering & Quality whose activities
include ongoing and/or planned missions, instrumentation, and modelling
and simulations. Output and activities from all these entities make up
an "ESA Heliophysics orchestra". This paper will provide an overview
of the Solar Orbiter flyby from the context of combined multi -mission
observations: ranging from Solar Orbiter's inbound bow shock crossing to
near closest approach and comparisons to low altitude measurements from
Swarm. During the outbound leg, across the dawn flank magnetopause, it
joined a collection of spacecraft, including Cluster and the NASA THEMIS
and MMS missions observing potential Kelvin Helmholtz activity. The
talk will include a brief introduction and description to the newly
formed ESA Heliophysics working group, an activity to provide a more
synergetic approach to Heliophysics internally within ESA, with an
aim to benefit the broad European and international science community.
Title: Solar Orbiter: Here comes the Sun
Authors: Müller, Daniel; Nieves-Chinchilla, Teresa; Zouganelis,
Yannis; Lario, David
Bibcode: 2022cosp...44.1044M
Altcode:
The ESA/NASA Solar Orbiter mission started its nominal mission phase
in November 2021 and will have its first close solar encounter at
0.32 au in March 2022. By combining high-resolution imaging and
spectroscopy of the Sun with detailed in-situ measurements of the
surrounding heliosphere, Solar Orbiter will enable us to determine
the linkage between observed solar wind streams and their source
regions on the Sun. Over the course of the 10-year mission, the highly
elliptical orbit will get progressively more inclined to the ecliptic
plane. Thanks to this new perspective, Solar Orbiter will deliver
images and comprehensive data of the unexplored Sun's polar regions
and the side of the Sun not visible from Earth. This talk will provide
a mission status update, summarise the science operations performed
during the first close perihelion as well as the plans for the next
one in October 2022, and show first data.
Title: Probing spatial orientability of a Friedmann-Robertson-Walker
spatially flat spacetime
Authors: Lemos, N. A.; Müller, D.; Rebouças, M. J.
Bibcode: 2022PhRvD.106b3528L
Altcode: 2021arXiv211007675L
One important global topological property of a spacetime manifold
is orientability. It is widely believed that spatial orientability
can only be tested by global journeys around the Universe to check
for orientation-reversing closed paths. Since such global journeys
are not feasible, theoretical arguments that combine universality
of physical experiments with local arrow of time, C P violation
and C P T invariance are usually offered to support the choosing of
time- and space-orientable spacetime manifolds. The nonexistence of
globally defined spinor fields on a nonorientable spacetime is another
theoretical argument for orientability. However, it is conceivable
that orientability can be put to test by local physical effects. In
this paper, we show that it is possible to locally access spatial
orientability of a spatially flat Friedmann-Robertson-Walker spacetime
through quantum vacuum electromagnestic fluctuations. We argue that
a putative nonorientability of the spatial sections of spatially flat
Friedmann-Robertson-Walker spacetime can be ascertained by the study
of the stochastic motions of a charged particle or a point electric
dipole under quantum vacuum electromagnetic fluctuations. In particular,
the stochastic motions of a dipole permit the recognition of a presumed
nonorientability of three space in itself.
Title: Solar Orbiter's first close encounter with the Sun: preparation
of the coordinated science campaigns
Authors: de Groof, Anik; Müller, Daniel; Zouganelis, Yannis; Walsh,
Andrew; Williams, David
Bibcode: 2022cosp...44.1537D
Altcode:
After a Cruise Phase of 21 months, Solar Orbiter entered its first
scientific orbit on 27 November 2021 after a Gravity Assist Manoeuvre
(GAM) by the Earth. The spacecraft entered a highly elliptical orbit
that will bring it up to its first close perihelion on 17 March 2022,
at 0.32AU from the Sun. In the following years, further GAMs by Venus
will lead it even closer to the Sun and also out of the ecliptic
plane. Solar Orbiter's main goal is to study the connection between
the solar activity close to the star's surface and its effects as seen
in the heliosphere, the bubble-like region of space under the Sun's
influence including all solar planets. Therefore, its main scientific
goals can only be achieved by coordinated observations of both the
6 remote-sensing telescopes onboard, observing the dynamic Sun, and
the 4 in-situ instruments measuring the effects in the solar wind
surrounding the spacecraft. This coordination takes careful planning
and optimisation of the mission resources, in order to fully exploit
the capabilities of this exciting mission. In this contribution,
we present the science operations as planned for the first year of
Nominal mission phase, i.e. the first two orbits. By the time of the
COSPAR meeting, Solar Orbiter will have made its first close encounter
and most of the data from the perihelion will have arrived!
Title: Cosmic-ray isotope measurements with HELIX
Authors: Park, N.; Allison, P.; Beatty, J. J.; Beaufore, L.; Chen, Y.;
Coutu, S.; Gebhard, M.; Green, N.; Hanna, D.; Jeon, H. B.; Kunkler, B.;
Lang, M.; Mbarek, R.; McBride, K.; Mognet, I.; Muller, D.; Musser, J.;
Nutter, S.; O'Brien, S.; Siegel, Z.; Tabata, M.; Tarle, G.; Visser,
G.; Wakely, S. P.; Yu, M.; Helix Collaboration
Bibcode: 2022icrc.confE..91P
Altcode: 2022PoS...395E..91P
No abstract at ADS
Title: Refractory elements in the gas phase for comet
67P/Churyumov-Gerasimenko. Possible release of atomic Na, Si, and
Fe from nanograins
Authors: Rubin, Martin; Altwegg, Kathrin; Berthelier, Jean-Jacques;
Combi, Michael R.; De Keyser, Johan; Dhooghe, Frederik; Fuselier,
Stephen; Gombosi, Tamas I.; Hänni, Nora; Müller, Daniel; Pestoni,
Boris; Wampfler, Susanne F.; Wurz, Peter
Bibcode: 2022A&A...658A..87R
Altcode: 2021arXiv211208965R
Context. Gas-phase sodium, silicon, potassium, and calcium were
previously identified in mass spectra recorded in the coma of
comet 67P/Churyumov-Gerasimenko, the target of the European Space
Agency's Rosetta mission. The major release process for these atoms
was identified as sputtering by the solar wind. More recently, remote
observations of numerous comets over a range in heliocentric distances
revealed the presence of metal atoms of iron and nickel that had been
released either from the nucleus or from a distributed source with
a short scale length. Sputtering, however, has been dismissed as a
major release process due to the attenuation of the solar wind in the
comae of some of the observed targets.
Aims: We investigated
the presence of refractory species in the gas phase of the coma of
67P/Churyumov-Gerasimenko. This investigation includes a period close to
perihelion when the solar wind was likely absent from the near-nucleus
region due to the increased cometary activity. Additionally, we extended
our search to iron and nickel.
Methods: We analyzed in situ data
from the Rosetta/ROSINA Double Focusing Mass Spectrometer DFMS.
Results: We found that gas-phase silicon was present throughout the
Rosetta mission. Furthermore, the presence of sodium and iron atoms
near the comet's perihelion confirms that sputtering cannot be the sole
release process for refractory elements into the gas phase. Nickel
was found to be below the detection limit. The search for parent
species of any of the identified gas phase refractories has not been
successful. Upper limits for a suite of possible fragment species
(SiH, SiC, NaH, etc.) of larger parent and daughter species have been
obtained. Furthermore, Si did not exhibit the same drop in signal as
do common cometary gases when the spacecraft is pointed away from
the nucleus. The combined results suggest that a direct release of
elemental species from small grains on the surface of the nucleus or
from small grains in the surrounding coma is a more likely explanation
than the previous assumption of release via the dissociation of gaseous
parent molecules.
Title: Solar Orbiter: Starting the Nominal Mission Phase
Authors: Mueller, Daniel; Zouganelis, Yannis; Nieves-Chinchilla,
Teresa; Lario, David
Bibcode: 2021AGUFMSH21A..01M
Altcode:
The ESA/NASA Solar Orbiter mission will transition from cruise phase
into its nominal mission phase in November 2021 and have its first close
solar encounter at 0.32 au in March 2022. By combining high-resolution
imaging and spectroscopy of the Sun with detailed in-situ measurements
of the surrounding heliosphere, Solar Orbiter will enable us to
determine the linkage between observed solar wind streams and their
source regions on the Sun. Over the course of the 10-year mission,
the highly elliptical orbit will get progressively more inclined to
the ecliptic plane. Thanks to this new perspective, Solar Orbiter will
deliver images and comprehensive data of the unexplored Suns polar
regions and the side of the Sun not visible from Earth. This talk
will provide a mission status update, preview the science operations
scheduled around the first close perihelion passage, and highlight
synergies with other space- and ground-based observatories.
Title: First Solar Orbiter observation of the Alfvénic slow wind
and identification of its solar source
Authors: D'Amicis, R.; Bruno, R.; Panasenco, O.; Telloni, D.; Perrone,
D.; Marcucci, M. F.; Woodham, L.; Velli, M.; De Marco, R.; Jagarlamudi,
V.; Coco, I.; Owen, C.; Louarn, P.; Livi, S.; Horbury, T.; André,
N.; Angelini, V.; Evans, V.; Fedorov, A.; Genot, V.; Lavraud, B.;
Matteini, L.; Müller, D.; O'Brien, H.; Pezzi, O.; Rouillard, A. P.;
Sorriso-Valvo, L.; Tenerani, A.; Verscharen, D.; Zouganelis, I.
Bibcode: 2021A&A...656A..21D
Altcode:
Context. Turbulence dominated by large-amplitude, nonlinear Alfvén-like
fluctuations mainly propagating away from the Sun is ubiquitous
in high-speed solar wind streams. Recent studies have demontrated
that slow wind streams may also show strong Alfvénic signatures,
especially in the inner heliosphere.
Aims: The present study
focuses on the characterisation of an Alfvénic slow solar wind interval
observed by Solar Orbiter between 14 and 18 July 2020 at a heliocentric
distance of 0.64 AU.
Methods: Our analysis is based on plasma
moments and magnetic field measurements from the Solar Wind Analyser
(SWA) and Magnetometer (MAG) instruments, respectively. We compared
the behaviour of different parameters to characterise the stream
in terms of the Alfvénic content and magnetic properties. We also
performed a spectral analysis to highlight spectral features and
waves signature using power spectral density and magnetic helicity
spectrograms, respectively. Moreover, we reconstruct the Solar Orbiter
magnetic connectivity to the solar sources both via a ballistic
and a potential field source surface (PFSS) model.
Results:
The Alfvénic slow wind stream described in this paper resembles, in
many respects, a fast wind stream. Indeed, at large scales, the time
series of the speed profile shows a compression region, a main portion
of the stream, and a rarefaction region, characterised by different
features. Moreover, before the rarefaction region, we pinpoint several
structures at different scales recalling the spaghetti-like flux-tube
texture of the interplanetary magnetic field. Finally, we identify the
connections between Solar Orbiter in situ measurements, tracing them
down to coronal streamer and pseudostreamer configurations.
Conclusions: The characterisation of the Alfvénic slow wind stream
observed by Solar Orbiter and the identification of its solar source
are extremely important aspects for improving the understanding of
future observations of the same solar wind regime, especially as solar
activity is increasing toward a maximum, where a higher incidence of
this solar wind regime is expected.
Title: First Solar Orbiter observation of an Alfvenic slow wind stream
Authors: D'Amicis, Raffaella; Bruno, Roberto; Panasenco, Olga;
Telloni, Daniele; Perrone, Denise; Marcucci, Maria Federica; Woodham,
Lloyd; Velli, Marco; De Marco, Rossana; Jagarlamudi, vamsee Krishna;
Coco, Igino; Owen, Christopher; Louarn, Philippe; Livi, Stefano;
Horbury, Timothy; Andre, Nicolas; Angelini, Virginia; Evans, Vincent;
Fedorov, Andrei; Genot, Vincent; Lavraud, Benoit; Matteini, Lorenzo;
Muller, Daniel; O'Brien, Helen; Pezzi, Oreste; Rouillard, Alexis;
Sorriso-Valvo, Luca; Tenerani, Anna; Verscharen, Daniel; Zouganelis,
Yannis
Bibcode: 2021AGUFMSH21A..10D
Altcode:
Alfvénic turbulence, dominated by large-amplitude Alfvénic
fluctuations mainly propagating away from the Sun, is a feature
characterizing not only the high-speed streams but also some slow
wind intervals. Within this framework, the present study focuses on
an Alfvénic slow solar wind stream observed by Solar Orbiter in July
2020 at a heliocentric distance of 0.64 AU. Using data collected from
the Solar Wind Analyzer (SWA) and the Magnetometer (MAG), we provide
a fully description of this stream from many respects identifying
different regions within the stream characterized by distinct features
using different indicators and including also a spectral analysis
to highlight spectral features and waves signature. In addition,
we pinpoint several structures at different scales recalling the
spaghetti-like flux-tube texture of the interplanetary magnetic field
and we reconstruct the Solar Orbiter magnetic connectivity to the
solar sources both via a ballistic and a potential field source surface
(PFSS) model. The characterization of the Alfvénic slow wind stream
observed by Solar Orbiter and the identification of its solar source
are extremely important for improving the understanding of future
observations of the same solar wind regime and the general problem of
solar wind acceleration. This is particularly relevant for upcoming
Solar Orbiter observations as solar activity is increasing toward a
maximum, where a higher incidence of this solar wind regime has been
observed over previous solar cycles.
Title: Solar Orbiter's encounter with the tail of comet C/2019 Y4
(ATLAS): Magnetic field draping and cometary pick-up ion waves
Authors: Matteini, L.; Laker, R.; Horbury, T.; Woodham, L.; Bale,
S. D.; Stawarz, J. E.; Woolley, T.; Steinvall, K.; Jones, G. H.; Grant,
S. R.; Afghan, Q.; Galand, M.; O'Brien, H.; Evans, V.; Angelini,
V.; Maksimovic, M.; Chust, T.; Khotyaintsev, Y.; Krasnoselskikh,
V.; Kretzschmar, M.; Lorfèvre, E.; Plettemeier, D.; Souček, J.;
Steller, M.; Štverák, Š.; Trávníček, P.; Vaivads, A.; Vecchio,
A.; Wimmer-Schweingruber, R. F.; Ho, G. C.; Gómez-Herrero, R.;
Rodríguez-Pacheco, J.; Louarn, P.; Fedorov, A.; Owen, C. J.; Bruno,
R.; Livi, S.; Zouganelis, I.; Müller, D.
Bibcode: 2021A&A...656A..39M
Altcode:
Context. Solar Orbiter is expected to have flown close to the tail of
comet C/2019 Y4 (ATLAS) during the spacecraft's first perihelion in
June 2020. Models predict a possible crossing of the comet tails by the
spacecraft at a distance from the Sun of approximately 0.5 AU.
Aims: This study is aimed at identifying possible signatures of the
interaction of the solar wind plasma with material released by comet
ATLAS, including the detection of draped magnetic field as well as the
presence of cometary pick-up ions and of ion-scale waves excited by
associated instabilities. This encounter provides us with the first
opportunity of addressing such dynamics in the inner Heliosphere and
improving our understanding of the plasma interaction between comets
and the solar wind.
Methods: We analysed data from all in situ
instruments on board Solar Orbiter and compared their independent
measurements in order to identify and characterize the nature of
structures and waves observed in the plasma when the encounter was
predicted.
Results: We identified a magnetic field structure
observed at the start of 4 June, associated with a full magnetic
reversal, a local deceleration of the flow and large plasma density,
and enhanced dust and energetic ions events. The cross-comparison
of all these observations support a possible cometary origin for
this structure and suggests the presence of magnetic field draping
around some low-field and high-density object. Inside and around this
large scale structure, several ion-scale wave-forms are detected that
are consistent with small-scale waves and structures generated by
cometary pick-up ion instabilities.
Conclusions: Solar Orbiter
measurements are consistent with the crossing through a magnetic
and plasma structure of cometary origin embedded in the ambient solar
wind. We suggest that this corresponds to the magnetotail of one of the
fragments of comet ATLAS or to a portion of the tail that was previously
disconnected and advected past the spacecraft by the solar wind.
Title: Study of two interacting interplanetary coronal mass
ejections encountered by Solar Orbiter during its first perihelion
passage. Observations and modeling
Authors: Telloni, D.; Scolini, C.; Möstl, C.; Zank, G. P.;
Zhao, L. -L.; Weiss, A. J.; Reiss, M. A.; Laker, R.; Perrone, D.;
Khotyaintsev, Y.; Steinvall, K.; Sorriso-Valvo, L.; Horbury, T. S.;
Wimmer-Schweingruber, R. F.; Bruno, R.; D'Amicis, R.; De Marco,
R.; Jagarlamudi, V. K.; Carbone, F.; Marino, R.; Stangalini, M.;
Nakanotani, M.; Adhikari, L.; Liang, H.; Woodham, L. D.; Davies, E. E.;
Hietala, H.; Perri, S.; Gómez-Herrero, R.; Rodríguez-Pacheco, J.;
Antonucci, E.; Romoli, M.; Fineschi, S.; Maksimovic, M.; Souček,
J.; Chust, T.; Kretzschmar, M.; Vecchio, A.; Müller, D.; Zouganelis,
I.; Winslow, R. M.; Giordano, S.; Mancuso, S.; Susino, R.; Ivanovski,
S. L.; Messerotti, M.; O'Brien, H.; Evans, V.; Angelini, V.
Bibcode: 2021A&A...656A...5T
Altcode:
Context. Solar Orbiter, the new-generation mission dedicated to solar
and heliospheric exploration, was successfully launched on February
10, 2020, 04:03 UTC from Cape Canaveral. During its first perihelion
passage in June 2020, two successive interplanetary coronal mass
ejections (ICMEs), propagating along the heliospheric current sheet
(HCS), impacted the spacecraft.
Aims: This paper addresses the
investigation of the ICMEs encountered by Solar Orbiter on June 7−8,
2020, from both an observational and a modeling perspective. The aim is
to provide a full description of those events, their mutual interaction,
and their coupling with the ambient solar wind and the HCS.
Methods: Data acquired by the MAG magnetometer, the Energetic Particle
Detector suite, and the Radio and Plasma Waves instrument are used to
provide information on the ICMEs' magnetic topology configuration,
their magnetic connectivity to the Sun, and insights into the
heliospheric plasma environment where they travel, respectively. On
the modeling side, the Heliospheric Upwind eXtrapolation model, the
3D COronal Rope Ejection technique, and the EUropean Heliospheric
FORecasting Information Asset (EUHFORIA) tool are used to complement
Solar Orbiter observations of the ambient solar wind and ICMEs,
and to simulate the evolution and interaction of the ejecta in the
inner heliosphere, respectively.
Results: Both data analysis
and numerical simulations indicate that the passage of two distinct,
dynamically and magnetically interacting (via magnetic reconnection
processes) ICMEs at Solar Orbiter is a possible scenario, supported by
the numerous similarities between EUHFORIA time series at Solar Orbiter
and Solar Orbiter data.
Conclusions: The combination of in situ
measurements and numerical simulations (together with remote sensing
observations of the corona and inner heliosphere) will significantly
lead to a deeper understanding of the physical processes occurring
during the CME-CME interaction. Movies are available at https://www.aanda.org
Title: First observations from the SPICE EUV spectrometer on Solar
Orbiter
Authors: Fludra, A.; Caldwell, M.; Giunta, A.; Grundy, T.; Guest,
S.; Leeks, S.; Sidher, S.; Auchère, F.; Carlsson, M.; Hassler, D.;
Peter, H.; Aznar Cuadrado, R.; Buchlin, É.; Caminade, S.; DeForest,
C.; Fredvik, T.; Haberreiter, M.; Harra, L.; Janvier, M.; Kucera, T.;
Müller, D.; Parenti, S.; Schmutz, W.; Schühle, U.; Solanki, S. K.;
Teriaca, L.; Thompson, W. T.; Tustain, S.; Williams, D.; Young, P. R.;
Chitta, L. P.
Bibcode: 2021A&A...656A..38F
Altcode: 2021arXiv211011252F
Aims: We present first science observations taken during the
commissioning activities of the Spectral Imaging of the Coronal
Environment (SPICE) instrument on the ESA/NASA Solar Orbiter
mission. SPICE is a high-resolution imaging spectrometer operating at
extreme ultraviolet (EUV) wavelengths. In this paper we illustrate
the possible types of observations to give prospective users a
better understanding of the science capabilities of SPICE.
Methods: We have reviewed the data obtained by SPICE between April
and June 2020 and selected representative results obtained with
different slits and a range of exposure times between 5 s and 180
s. Standard instrumental corrections have been applied to the raw
data.
Results: The paper discusses the first observations
of the Sun on different targets and presents an example of the full
spectra from the quiet Sun, identifying over 40 spectral lines from
neutral hydrogen and ions of carbon, oxygen, nitrogen, neon, sulphur,
magnesium, and iron. These lines cover the temperature range between
20 000 K and 1 million K (10 MK in flares), providing slices of the
Sun's atmosphere in narrow temperature intervals. We provide a list
of count rates for the 23 brightest spectral lines. We show examples
of raster images of the quiet Sun in several strong transition region
lines, where we have found unusually bright, compact structures in the
quiet Sun network, with extreme intensities up to 25 times greater
than the average intensity across the image. The lifetimes of these
structures can exceed 2.5 hours. We identify them as a transition
region signature of coronal bright points and compare their areas and
intensity enhancements. We also show the first above-limb measurements
with SPICE above the polar limb in C III, O VI, and Ne VIII lines, and
far off limb measurements in the equatorial plane in Mg IX, Ne VIII,
and O VI lines. We discuss the potential to use abundance diagnostics
methods to study the variability of the elemental composition that can
be compared with in situ measurements to help confirm the magnetic
connection between the spacecraft location and the Sun's surface,
and locate the sources of the solar wind.
Conclusions: The
SPICE instrument successfully performs measurements of EUV spectra
and raster images that will make vital contributions to the scientific
success of the Solar Orbiter mission.
Title: First observations and performance of the RPW instrument on
board the Solar Orbiter mission
Authors: Maksimovic, M.; Souček, J.; Chust, T.; Khotyaintsev, Y.;
Kretzschmar, M.; Bonnin, X.; Vecchio, A.; Alexandrova, O.; Bale, S. D.;
Bérard, D.; Brochot, J. -Y.; Edberg, N. J. T.; Eriksson, A.; Hadid,
L. Z.; Johansson, E. P. G.; Karlsson, T.; Katra, B.; Krasnoselskikh,
V.; Krupař, V.; Lion, S.; Lorfèvre, E.; Matteini, L.; Nguyen, Q. N.;
Píša, D.; Piberne, R.; Plettemeier, D.; Rucker, H. O.; Santolík,
O.; Steinvall, K.; Steller, M.; Štverák, Š.; Trávníček, P.;
Vaivads, A.; Zaslavsky, A.; Chaintreuil, S.; Dekkali, M.; Astier,
P. -A.; Barbary, G.; Boughedada, K.; Cecconi, B.; Chapron, F.; Collin,
C.; Dias, D.; Guéguen, L.; Lamy, L.; Leray, V.; Malac-Allain, L. R.;
Pantellini, F.; Parisot, J.; Plasson, P.; Thijs, S.; Fratter, I.;
Bellouard, E.; Danto, P.; Julien, S.; Guilhem, E.; Fiachetti, C.;
Sanisidro, J.; Laffaye, C.; Gonzalez, F.; Pontet, B.; Quéruel, N.;
Jannet, G.; Fergeau, P.; Dudok de Wit, T.; Vincent, T.; Agrapart,
C.; Pragout, J.; Bergerard-Timofeeva, M.; Delory, G. T.; Turin, P.;
Jeandet, A.; Leroy, P.; Pellion, J. -C.; Bouzid, V.; Recart, W.;
Kolmašová, I.; Krupařová, O.; Uhlíř, L.; Lán, R.; Baše, J.;
André, M.; Bylander, L.; Cripps, V.; Cully, C.; Jansson, S. -E.;
Puccio, W.; Břínek, J.; Ottacher, H.; Angelini, V.; Berthomier,
M.; Evans, V.; Goetz, K.; Hellinger, P.; Horbury, T. S.; Issautier,
K.; Kontar, E.; Le Contel, O.; Louarn, P.; Martinović, M.; Müller,
D.; O'Brien, H.; Owen, C. J.; Retino, A.; Rodríguez-Pacheco, J.;
Sahraoui, F.; Sanchez, L.; Walsh, A. P.; Wimmer-Schweingruber, R. F.;
Zouganelis, I.
Bibcode: 2021A&A...656A..41M
Altcode:
The Radio and Plasma Waves (RPW) instrument on the ESA Solar Orbiter
mission is designed to measure in situ magnetic and electric fields
and waves from the continuum up to several hundred kHz. The RPW also
observes solar and heliospheric radio emissions up to 16 MHz. It was
switched on and its antennae were successfully deployed two days after
the launch of Solar Orbiter on February 10, 2020. Since then, the
instrument has acquired enough data to make it possible to assess its
performance and the electromagnetic disturbances it experiences. In this
article, we assess its scientific performance and present the first RPW
observations. In particular, we focus on a statistical analysis of the
first observations of interplanetary dust by the instrument's Thermal
Noise Receiver. We also review the electro-magnetic disturbances that
RPW suffers, especially those which potential users of the instrument
data should be aware of before starting their research work.
Title: The Magnetic Origin of Solar Campfires
Authors: Panesar, Navdeep K.; Tiwari, Sanjiv K.; Berghmans, David;
Cheung, Mark C. M.; Müller, Daniel; Auchere, Frederic; Zhukov, Andrei
Bibcode: 2021ApJ...921L..20P
Altcode: 2021arXiv211006846P
Solar campfires are fine-scale heating events, recently observed by
Extreme Ultraviolet Imager (EUI) on board Solar Orbiter. Here we use EUI
174 Å images, together with EUV images from Solar Dynamics Observatory
(SDO)/Atmospheric Imaging Assembly (AIA), and line-of-sight magnetograms
from SDO/Helioseismic and Magnetic Imager (HMI) to investigate the
magnetic origin of 52 randomly selected campfires in the quiet solar
corona. We find that (i) the campfires are rooted at the edges of
photospheric magnetic network lanes; (ii) most of the campfires reside
above the neutral line between majority-polarity magnetic flux patch and
a merging minority-polarity flux patch, with a flux cancelation rate of
~1018 Mx hr-1; (iii) some of the campfires occur
repeatedly from the same neutral line; (iv) in the large majority of
instances, campfires are preceded by a cool-plasma structure, analogous
to minifilaments in coronal jets; and (v) although many campfires have
"complex" structure, most campfires resemble small-scale jets, dots,
or loops. Thus, "campfire" is a general term that includes different
types of small-scale solar dynamic features. They contain sufficient
magnetic energy (~1026-1027 erg) to heat the solar
atmosphere locally to 0.5-2.5 MK. Their lifetimes range from about 1
minute to over 1 hr, with most of the campfires having a lifetime of
<10 minutes. The average lengths and widths of the campfires are 5400
± 2500 km and 1600 ± 640 km, respectively. Our observations suggest
that (a) the presence of magnetic flux ropes may be ubiquitous in the
solar atmosphere and not limited to coronal jets and larger-scale
eruptions that make CMEs, and (b) magnetic flux cancelation is the
fundamental process for the formation and triggering of most campfires.
Title: Search for the doubly charmed baryon
Ωcc+
Authors: LHCb Collaboration; Aaij, R.; Abellán Beteta, C.; Ackernley,
T.; Adeva, B.; Adinolfi, M.; Afsharnia, H.; Aidala, C. A.; Aiola, S.;
Ajaltouni, Z.; Akar, S.; Albrecht, J.; Alessio, F.; Alexander, M.;
Alfonso Albero, A.; Aliouche, Z.; Alkhazov, G.; Alvarez Cartelle, P.;
Amato, S.; Amhis, Y.; An, L.; Anderlini, L.; Andreianov, A.; Andreotti,
M.; Archilli, F.; Artamonov, A.; Artuso, M.; Arzymatov, K.; Aslanides,
E.; Atzeni, M.; Audurier, B.; Bachmann, S.; Bachmayer, M.; Back, J. J.;
Baladron Rodriguez, P.; Balagura, V.; Baldini, W.; Baptista Leite, J.;
Barlow, R. J.; Barsuk, S.; Barter, W.; Bartolini, M.; Baryshnikov, F.;
Basels, J. M.; Bassi, G.; Batsukh, B.; Battig, A.; Bay, A.; Becker, M.;
Bedeschi, F.; Bediaga, I.; Beiter, A.; Belavin, V.; Belin, S.; Bellee,
V.; Belous, K.; Belov, I.; Belyaev, I.; Bencivenni, G.; Ben-Haim, E.;
Berezhnoy, A.; Bernet, R.; Berninghoff, D.; Bernstein, H. C.; Bertella,
C.; Bertolin, A.; Betancourt, C.; Betti, F.; Bezshyiko, I.; Bhasin,
S.; Bhom, J.; Bian, L.; Bieker, M. S.; Bifani, S.; Billoir, P.; Birch,
M.; Bishop, F. C. R.; Bitadze, A.; Bizzeti, A.; Bjørn, M.; Blago,
M. P.; Blake, T.; Blanc, F.; Blusk, S.; Bobulska, D.; Boelhauve, J. A.;
Boente Garcia, O.; Boettcher, T.; Boldyrev, A.; Bondar, A.; Bondar,
N.; Borghi, S.; Borisyak, M.; Borsato, M.; Borsuk, J. T.; Bouchiba,
S. A.; Bowcock, T. J. V.; Boyer, A.; Bozzi, C.; Bradley, M. J.; Braun,
S.; Brea Rodriguez, A.; Brodski, M.; Brodzicka, J.; Brossa Gonzalo,
A.; Brundu, D.; Buonaura, A.; Burr, C.; Bursche, A.; Butkevich, A.;
Butter, J. S.; Buytaert, J.; Byczynski, W.; Cadeddu, S.; Cai, H.;
Calabrese, R.; Calefice, L.; Calero Diaz, L.; Cali, S.; Calladine,
R.; Calvi, M.; Calvo Gomez, M.; Camargo Magalhaes, P.; Campana,
P.; Campoverde Quezada, A. F.; Capelli, S.; Capriotti, L.; Carbone,
A.; Carboni, G.; Cardinale, R.; Cardini, A.; Carli, I.; Carniti, P.;
Carus, L.; Carvalho Akiba, K.; Casais Vidal, A.; Casse, G.; Cattaneo,
M.; Cavallero, G.; Celani, S.; Cerasoli, J.; Chadwick, A. J.; Chapman,
M. G.; Charles, M.; Charpentier, P.; Chatzikonstantinidis, G.; Chavez
Barajas, C. A.; Chefdeville, M.; Chen, C.; Chen, S.; Chernov, A.;
Chobanova, V.; Cholak, S.; Chrzaszcz, M.; Chubykin, A.; Chulikov, V.;
Ciambrone, P.; Cicala, M. F.; Cid Vidal, X.; Ciezarek, G.; Clarke,
P. E. L.; Clemencic, M.; Cliff, H. V.; Closier, J.; Cobbledick, J. L.;
Coco, V.; Coelho, J. A. B.; Cogan, J.; Cogneras, E.; Cojocariu,
L.; Collins, P.; Colombo, T.; Congedo, L.; Contu, A.; Cooke, N.;
Coombs, G.; Corti, G.; Costa Sobral, C. M.; Couturier, B.; Craik,
D. C.; Crkovská, J.; Cruz Torres, M.; Currie, R.; Da Silva, C. L.;
Dadabaev, S.; Dall'Occo, E.; Dalseno, J.; D'Ambrosio, C.; Danilina,
A.; d'Argent, P.; Davis, A.; De Aguiar Francisco, O.; De Bruyn,
K.; De Capua, S.; De Cian, M.; De Miranda, J. M.; De Paula, L.;
De Serio, M.; De Simone, D.; De Simone, P.; de Vries, J. A.; Dean,
C. T.; Decamp, D.; Del Buono, L.; Delaney, B.; Dembinski, H. -P.;
Dendek, A.; Denysenko, V.; Derkach, D.; Deschamps, O.; Desse, F.;
Dettori, F.; Dey, B.; Di Cicco, A.; Di Nezza, P.; Didenko, S.; Dieste
Maronas, L.; Dijkstra, H.; Dobishuk, V.; Donohoe, A. M.; Dordei, F.;
dos Reis, A. C.; Douglas, L.; Dovbnya, A.; Downes, A. G.; Dreimanis,
K.; Dudek, M. W.; Dufour, L.; Duk, V.; Durante, P.; Durham, J. M.;
Dutta, D.; Dziurda, A.; Dzyuba, A.; Easo, S.; Egede, U.; Egorychev,
V.; Eidelman, S.; Eisenhardt, S.; Ek-In, S.; Eklund, L.; Ely, S.;
Ene, A.; Epple, E.; Escher, S.; Eschle, J.; Esen, S.; Evans, T.;
Falabella, A.; Fan, J.; Fan, Y.; Fang, B.; Farry, S.; Fazzini, D.;
Féo, M.; Fernandez Prieto, A.; Fernandez-tenllado Arribas, J. M.;
Fernez, A. D.; Ferrari, F.; Ferreira Lopes, L.; Ferreira Rodrigues, F.;
Ferreres Sole, S.; Ferrillo, M.; Ferro-Luzzi, M.; Filippov, S.; Fini,
R. A.; Fiorini, M.; Firlej, M.; Fischer, K. M.; Fitzgerald, D. S.;
Fitzpatrick, C.; Fiutowski, T.; Fkiaras, A.; Fleuret, F.; Fontana,
M.; Fontanelli, F.; Forty, R.; Franco Lima, V.; Franco Sevilla, M.;
Frank, M.; Franzoso, E.; Frau, G.; Frei, C.; Friday, D. A.; Fu, J.;
Fuehring, Q.; Funk, W.; Gabriel, E.; Gaintseva, T.; Gallas Torreira,
A.; Galli, D.; Gambetta, S.; Gan, Y.; Gandelman, M.; Gandini, P.;
Gao, Y.; Garau, M.; Garcia Martin, L. M.; Garcia Moreno, P.; García
Pardiñas, J.; Garcia Plana, B.; Garcia Rosales, F. A.; Garrido, L.;
Gaspar, C.; Geertsema, R. E.; Gerick, D.; Gerken, L. L.; Gersabeck,
E.; Gersabeck, M.; Gershon, T.; Gerstel, D.; Ghez, P.; Gibson, V.;
Giemza, H. K.; Giovannetti, M.; Gioventù, A.; Gironella Gironell, P.;
Giubega, L.; Giugliano, C.; Gizdov, K.; Gkougkousis, E. L.; Gligorov,
V. V.; Göbel, C.; Golobardes, E.; Golubkov, D.; Golutvin, A.; Gomes,
A.; Gomez Fernandez, S.; Goncalves Abrantes, F.; Goncerz, M.; Gong,
G.; Gorbounov, P.; Gorelov, I. V.; Gotti, C.; Govorkova, E.; Grabowski,
J. P.; Grammatico, T.; Granado Cardoso, L. A.; Graugés, E.; Graverini,
E.; Graziani, G.; Grecu, A.; Greeven, L. M.; Griffith, P.; Grillo, L.;
Gromov, S.; Gruberg Cazon, B. R.; Gu, C.; Guarise, M.; Günther, P. A.;
Gushchin, E.; Guth, A.; Guz, Y.; Gys, T.; Hadavizadeh, T.; Haefeli,
G.; Haen, C.; Haimberger, J.; Halewood-leagas, T.; Hamilton, P. M.;
Hammerich, J. P.; Han, Q.; Han, X.; Hancock, T. H.; Hansmann-Menzemer,
S.; Harnew, N.; Harrison, T.; Hasse, C.; Hatch, M.; He, J.; Hecker,
M.; Heijhoff, K.; Heinicke, K.; Hennequin, A. M.; Hennessy, K.; Henry,
L.; Heuel, J.; Hicheur, A.; Hill, D.; Hilton, M.; Hollitt, S. E.; Hu,
J.; Hu, J.; Hu, W.; Hu, X.; Huang, W.; Huang, X.; Hulsbergen, W.;
Hunter, R. J.; Hushchyn, M.; Hutchcroft, D.; Hynds, D.; Ibis, P.;
Idzik, M.; Ilin, D.; Ilten, P.; Inglessi, A.; Ishteev, A.; Ivshin,
K.; Jacobsson, R.; Jakobsen, S.; Jans, E.; Jashal, B. K.; Jawahery,
A.; Jevtic, V.; Jezabek, M.; Jiang, F.; John, M.; Johnson, D.; Jones,
C. R.; Jones, T. P.; Jost, B.; Jurik, N.; Kandybei, S.; Kang, Y.;
Karacson, M.; Karpov, M.; Keizer, F.; Kenzie, M.; Ketel, T.; Khanji,
B.; Kharisova, A.; Kholodenko, S.; Kirn, T.; Kirsebom, V. S.; Kitouni,
O.; Klaver, S.; Klimaszewski, K.; Koliiev, S.; Kondybayeva, A.;
Konoplyannikov, A.; Kopciewicz, P.; Kopecna, R.; Koppenburg, P.;
Korolev, M.; Kostiuk, I.; Kot, O.; Kotriakhova, S.; Kravchenko, P.;
Kravchuk, L.; Krawczyk, R. D.; Kreps, M.; Kress, F.; Kretzschmar, S.;
Krokovny, P.; Krupa, W.; Krzemien, W.; Kucewicz, W.; Kucharczyk, M.;
Kudryavtsev, V.; Kuindersma, H. S.; Kunde, G. J.; Kvaratskheliya, T.;
Lacarrere, D.; Lafferty, G.; Lai, A.; Lampis, A.; Lancierini, D.; Lane,
J. J.; Lane, R.; Lanfranchi, G.; Langenbruch, C.; Langer, J.; Lantwin,
O.; Latham, T.; Lazzari, F.; Le Gac, R.; Lee, S. H.; Lefèvre, R.;
Leflat, A.; Legotin, S.; Leroy, O.; Lesiak, T.; Leverington, B.;
Li, H.; Li, L.; Li, P.; Li, S.; Li, Y.; Li, Y.; Li, Z.; Liang, X.;
Lin, T.; Lindner, R.; Lisovskyi, V.; Litvinov, R.; Liu, G.; Liu,
H.; Liu, S.; Loi, A.; Lomba Castro, J.; Longstaff, I.; Lopes, J. H.;
Lovell, G. H.; Lu, Y.; Lucchesi, D.; Luchuk, S.; Lucio Martinez, M.;
Lukashenko, V.; Luo, Y.; Lupato, A.; Luppi, E.; Lupton, O.; Lusiani,
A.; Lyu, X.; Ma, L.; Ma, R.; Maccolini, S.; Machefert, F.; Maciuc, F.;
Macko, V.; Mackowiak, P.; Maddrell-Mander, S.; Madejczyk, O.; Madhan
Mohan, L. R.; Maev, O.; Maevskiy, A.; Maisuzenko, D.; Majewski, M. W.;
Malczewski, J. J.; Malde, S.; Malecki, B.; Malinin, A.; Maltsev, T.;
Malygina, H.; Manca, G.; Mancinelli, G.; Manuzzi, D.; Marangotto, D.;
Maratas, J.; Marchand, J. F.; Marconi, U.; Mariani, S.; Marin Benito,
C.; Marinangeli, M.; Marks, J.; Marshall, A. M.; Marshall, P. J.;
Martellotti, G.; Martinazzoli, L.; Martinelli, M.; Martinez Santos, D.;
Martinez Vidal, F.; Massafferri, A.; Materok, M.; Matev, R.; Mathad,
A.; Mathe, Z.; Matiunin, V.; Matteuzzi, C.; Mattioli, K. R.; Mauri,
A.; Maurice, E.; Mauricio, J.; Mazurek, M.; McCann, M.; Mcconnell,
L.; Mcgrath, T. H.; McNab, A.; McNulty, R.; Mead, J. V.; Meadows, B.;
Meier, G.; Meinert, N.; Melnychuk, D.; Meloni, S.; Merk, M.; Merli,
A.; Meyer Garcia, L.; Mikhasenko, M.; Milanes, D. A.; Millard, E.;
Milovanovic, M.; Minard, M. -N.; Minotti, A.; Minzoni, L.; Mitchell,
S. E.; Mitreska, B.; Mitzel, D. S.; Mödden, A.; Mohammed, R. A.;
Moise, R. D.; Mombächer, T.; Monroy, I. A.; Monteil, S.; Morandin, M.;
Morello, G.; Morello, M. J.; Moron, J.; Morris, A. B.; Morris, A. G.;
Mountain, R.; Mu, H.; Muheim, F.; Mulder, M.; Müller, D.; Müller,
K.; Murphy, C. H.; Murray, D.; Muzzetto, P.; Naik, P.; Nakada, T.;
Nandakumar, R.; Nanut, T.; Nasteva, I.; Needham, M.; Neri, I.; Neri,
N.; Neubert, S.; Neufeld, N.; Newcombe, R.; Nguyen, T. D.; Nguyen-Mau,
C.; Niel, E. M.; Nieswand, S.; Nikitin, N.; Nolte, N. S.; Normand,
C.; Nunez, C.; Oblakowska-Mucha, A.; Obraztsov, V.; O'Hanlon, D. P.;
Oldeman, R.; Olivares, M. E.; Onderwater, C. J. G.; O'neil, R. H.;
Ossowska, A.; Otalora Goicochea, J. M.; Ovsiannikova, T.; Owen,
P.; Oyanguren, A.; Pagare, B.; Pais, P. R.; Pajero, T.; Palano,
A.; Palutan, M.; Pan, Y.; Panshin, G.; Papanestis, A.; Pappagallo,
M.; Pappalardo, L. L.; Pappenheimer, C.; Parker, W.; Parkes, C.;
Parkinson, C. J.; Passalacqua, B.; Passaleva, G.; Pastore, A.; Patel,
M.; Patrignani, C.; Pawley, C. J.; Pearce, A.; Pellegrino, A.; Pepe
Altarelli, M.; Perazzini, S.; Pereima, D.; Perret, P.; Petric, M.;
Petridis, K.; Petrolini, A.; Petrov, A.; Petrucci, S.; Petruzzo, M.;
Pham, T. T. H.; Philippov, A.; Pica, L.; Piccini, M.; Pietrzyk, B.;
Pietrzyk, G.; Pili, M.; Pinci, D.; Pisani, F.; Resmi, P. K.; Placinta,
V.; Plews, J.; Plo Casasus, M.; Polci, F.; Poli Lener, M.; Poliakova,
M.; Poluektov, A.; Polukhina, N.; Polyakov, I.; Polycarpo, E.; Pomery,
G. J.; Ponce, S.; Popov, D.; Popov, S.; Poslavskii, S.; Prasanth, K.;
Promberger, L.; Prouve, C.; Pugatch, V.; Pullen, H.; Punzi, G.; Qi,
H.; Qian, W.; Qin, J.; Qin, N.; Quagliani, R.; Quintana, B.; Raab,
N. V.; Rabadan Trejo, R. I.; Rachwal, B.; Rademacker, J. H.; Rama,
M.; Ramos Pernas, M.; Rangel, M. S.; Ratnikov, F.; Raven, G.; Reboud,
M.; Redi, F.; Reiss, F.; Remon Alepuz, C.; Ren, Z.; Renaudin, V.;
Ribatti, R.; Ricciardi, S.; Rinnert, K.; Robbe, P.; Robertson, G.;
Rodrigues, A. B.; Rodrigues, E.; Rodriguez Lopez, J. A.; Rollings,
A.; Roloff, P.; Romanovskiy, V.; Romero Lamas, M.; Romero Vidal, A.;
Roth, J. D.; Rotondo, M.; Rudolph, M. S.; Ruf, T.; Ruiz Vidal, J.;
Ryzhikov, A.; Ryzka, J.; Saborido Silva, J. J.; Sagidova, N.; Sahoo,
N.; Saitta, B.; Salomoni, M.; Sanchez Gonzalo, D.; Sanchez Gras, C.;
Santacesaria, R.; Santamarina Rios, C.; Santimaria, M.; Santovetti,
E.; Saranin, D.; Sarpis, G.; Sarpis, M.; Sarti, A.; Satriano, C.;
Satta, A.; Saur, M.; Savrina, D.; Sazak, H.; Scantlebury Smead,
L. G.; Scarabotto, A.; Schael, S.; Schiller, M.; Schindler, H.;
Schmelling, M.; Schmidt, B.; Schneider, O.; Schopper, A.; Schubiger,
M.; Schulte, S.; Schune, M. H.; Schwemmer, R.; Sciascia, B.; Sellam,
S.; Semennikov, A.; Senghi Soares, M.; Sergi, A.; Serra, N.; Sestini,
L.; Seuthe, A.; Seyfert, P.; Shang, Y.; Shangase, D. M.; Shapkin,
M.; Shchemerov, I.; Shchutska, L.; Shears, T.; Shekhtman, L.; Shen,
Z.; Shevchenko, V.; Shields, E. B.; Shmanin, E.; Shupperd, J. D.;
Siddi, B. G.; Silva Coutinho, R.; Simi, G.; Simone, S.; Skidmore, N.;
Skwarnicki, T.; Slater, M. W.; Slazyk, I.; Smallwood, J. C.; Smeaton,
J. G.; Smetkina, A.; Smith, E.; Smith, M.; Snoch, A.; Soares, M.;
Soares Lavra, L.; Sokoloff, M. D.; Soler, F. J. P.; Solovev, A.;
Solovyev, I.; Souza De Almeida, F. L.; Souza De Paula, B.; Spaan,
B.; Spadaro Norella, E.; Spradlin, P.; Stagni, F.; Stahl, M.; Stahl,
S.; Stefko, P.; Steinkamp, O.; Stenyakin, O.; Stevens, H.; Stone,
S.; Stramaglia, M. E.; Straticiuc, M.; Strekalina, D.; Suljik, F.;
Sun, J.; Sun, L.; Sun, Y.; Svihra, P.; Swallow, P. N.; Swientek, K.;
Szabelski, A.; Szumlak, T.; Szymanski, M.; Taneja, S.; Tanner, A. R.;
Terentev, A.; Teubert, F.; Thomas, E.; Thomson, K. A.; Tisserand,
V.; T'Jampens, S.; Tobin, M.; Tomassetti, L.; Torres Machado, D.;
Tou, D. Y.; Tran, M. T.; Trifonova, E.; Trippl, C.; Tuci, G.; Tully,
A.; Tuning, N.; Ukleja, A.; Unverzagt, D. J.; Ursov, E.; Usachov,
A.; Ustyuzhanin, A.; Uwer, U.; Vagner, A.; Vagnoni, V.; Valassi,
A.; Valenti, G.; Valls Canudas, N.; van Beuzekom, M.; Van Dijk, M.;
van Herwijnen, E.; Van Hulse, C. B.; van Veghel, M.; Vazquez Gomez,
R.; Vazquez Regueiro, P.; Vázquez Sierra, C.; Vecchi, S.; Velthuis,
J. J.; Veltri, M.; Venkateswaran, A.; Veronesi, M.; Vesterinen,
M.; Vieira, D.; Vieites Diaz, M.; Viemann, H.; Vilasis-Cardona,
X.; Vilella Figueras, E.; Villa, A.; Vincent, P.; Vom Bruch, D.;
Vorobyev, A.; Vorobyev, V.; Voropaev, N.; Vos, K.; Waldi, R.; Walsh,
J.; Wang, C.; Wang, J.; Wang, J.; Wang, J.; Wang, J.; Wang, M.; Wang,
R.; Wang, Y.; Wang, Z.; Wang, Z.; Wark, H. M.; Watson, N. K.; Weber,
S. G.; Websdale, D.; Weisser, C.; Westhenry, B. D. C.; White, D. J.;
Whitehead, M.; Wiedner, D.; Wilkinson, G.; Wilkinson, M.; Williams,
I.; Williams, M.; Williams, M. R. J.; Wilson, F. F.; Wislicki, W.;
Witek, M.; Witola, L.; Wormser, G.; Wotton, S. A.; Wu, H.; Wyllie,
K.; Xiang, Z.; Xiao, D.; Xie, Y.; Xu, A.; Xu, J.; Xu, L.; Xu, M.;
Xu, Q.; Xu, Z.; Xu, Z.; Yang, D.; Yang, S.; Yang, Y.; Yang, Z.; Yang,
Z.; Yao, Y.; Yeomans, L. E.; Yin, H.; Yu, J.; Yuan, X.; Yushchenko,
O.; Zaffaroni, E.; Zavertyaev, M.; Zdybal, M.; Zenaiev, O.; Zeng, M.;
Zhang, D.; Zhang, L.; Zhang, S.; Zhang, Y.; Zhang, Y.; Zharkova, A.;
Zhelezov, A.; Zheng, Y.; Zhou, X.; Zhou, Y.; Zhu, X.; Zhu, Z.; Zhukov,
V.; Zonneveld, J. B.; Zou, Q.; Zucchelli, S.; Zuliani, D.; Zunica, G.
Bibcode: 2021SCPMA..6401062L
Altcode: 2021arXiv210506841A
A search for the doubly charmed baryon Ωcc+
with the decay mode Ωcc+ →
Ξc+K−π+ is
performed using proton-proton collision data at a centre-of-mass
energy of 13 TeV collected by the LHCb experiment from 2016
to 2018, corresponding to an integrated luminosity of 5.4
fb−1. No significant signal is observed within the
invariant mass range of 3.6 to 4.0GeV/c2. Upper limits
are set on the ratio R of the production cross-section times
the total branching fraction of the Ωcc+
→ Ξc+K−π+
decay with respect to the Ξcc
++→Λc+K−π+π+
decay. Upper limits at 95% credibility level for R in the
range 0.005 to 0.11 are obtained for different hypotheses on the
Ωcc+ mass and lifetime in the rapidity range
from 2.0 to 4.5 and transverse momentum range from 4 to 15 GeV/c.
Title: The cometary matter between volatiles and macromolecules
Authors: Hänni, Nora; Altwegg, Kathrin; Müller, Daniel; Pestoni,
Boris; Rubin, Martin; Wampfler, Susanne
Bibcode: 2021EPSC...15..681H
Altcode:
Small and volatile molecules are the most abundant constituents of a
comet's neutral coma. Thanks to ESA's Rosetta mission, the neutral
coma of comet 67P/Churyumov-Gerasimenko (67P hereafter) has been
analyzed in great spatial and temporal detail, e.g., by Rubin et
al. (2019) or by Läuter et al. (2020). However, the Double Focusing
Mass Spectrometer (DFMS) - part of the Rosetta Orbiter Spectrometer for
Ion and Neutral Analysis (ROSINA; Balsiger et al. 2007) - delivered data
which contains information about the transition region between volatiles
and macromolecular matter. Manual fitting of individual spectra allows
to resolve pure hydrocarbon from heteroatom-bearing species also in the
higher mass-range of the instrument, up to mass-to-charge (m/z) ratios
of 140.While Altwegg et al. (2019) have reported tentative detections
of some heavier species like benzoic acid or naphthalene, spectra of
m/z>70 have not been investigated systematically. Here, we will
present preliminary results from the first comprehensive analysis of a
full data set (from m/z=12 to m/z=140) collected on August 3, 2015. On
this day, the comet was close to its perihelion and the dust activity,
as seen by the OSIRIS camera (Vincent et al. 2016), was high. Probably
due to sublimation of molecules from ejected and heated-up dust grains,
ROSINA/DFMS registered many signals above m/z=70. Due to the problem
of isomerism and the lack of reference data, we chose to follow a
statistical approach for our analysis. Larger species tend to expose
a lower degree of saturation and the H/C ratio seems to approach
that of highly unsaturated insoluble organic matter (IOM), cf., e.g.,
Sandford 2008. Although we cannot identify individual molecules in the
complex gas mixture that makes up for the cometary coma, we are able to
characterize for the first time the larger organic species that bridge
the small volatiles and the macromolecular matter observed in 67P's
dust by the Rosetta secondary ion mass spectrometer COSIMA (Fray et
al. 2016). Altwegg et al., 2019, Annu. Rev. Astron. Astrophys., 57,
113-55.Balsiger H. et al., 2007, Space Sci. Rev., 128, 745-801.Fray
et al., 2016, Nature, 538, 72-74.Läuter et al., 2020, MNRAS, 498,
3, 3995-4004.Rubin et al., 2019, MNRAS, 489, 594-607.Sandford, 2008,
Annu. Rev. Anal. Chem. 1, 549-78.Vincent et al., 2016, MNRAS, 462
(Suppl_1), 184-194.
Title: BepiColombo's cruise phase: unique opportunity for synergistic
observations
Authors: Hadid, L. Z.; Génot, V.; Aizawa, S.; Milillo, A.; Zender,
J.; Murakami, G.; Benkhoff, J.; Zouganelis, I.; Alberti, T.; André,
N.; Bebesi, Z.; Califano, F.; Dimmock, A. P.; Dosa, M.; Escoubet,
C. P.; Griton, L.; Ho, G. C.; Horbury, T. S.; Iwai, K.; Janvier, M.;
Kilpua, E.; Lavraud, B.; Madar, A.; Miyoshi, Y.; Müller, D.; Pinto,
R. F.; Rouillard, A. P.; Raines, J. M.; Raouafi, N.; Sahraoui, F.;
Sánchez-Cano, B.; Shiota, D.; Vainio, R.; Walsh, A.
Bibcode: 2021FrASS...8..154H
Altcode:
The investigation of multi-spacecraft coordinated observations
during the cruise phase of BepiColombo (ESA/JAXA) are reported,
with a particular emphasis on the recently launched missions,
Solar Orbiter (ESA/NASA) and Parker Solar Probe (NASA). Despite
some payload constraints, many instruments onboard BepiColombo
are operating during its cruise phase simultaneously covering a
wide range of heliocentric distances [0.28 AU - 0.5 AU]. Hence, the
various spacecraft configurations and the combined in-situ and remote
sensing measurements from the different spacecraft, offer unique
opportunities for BepiColombo to be part of these unprecedented
multipoint synergistic observations and for potential scientific
studies in the inner heliosphere, even before its orbit insertion
around Mercury in December 2025. The main goal of this report is to
present the coordinated observation opportunities during the cruise
phase of BepiColombo (excluding the planetary flybys). We summarize
the identified science topics, the operational instruments, the method
we have used to identify the windows of opportunity and discuss the
planning of joint observations in the future.
Title: Static cosmological solutions in quadratic gravity
Authors: Müller, Daniel; Toporensky, Alexey
Bibcode: 2021GReGr..53...60M
Altcode: 2021arXiv210413460M
We consider conditions for existence and stability of a static
cosmological solution in quadratic gravity. It appears that such
a solution for a Universe filled by only one type of perfect fluid
is possible in a wide range of the equation of state parameter w and
for both positively and negatively spatially curved Universe. We show
that the static solution for the negative curvature is always unstable
if we require positive energy density of the matter content. On the
other hand, a static solution with positive spatial curvature can
be stable under certain restrictions. Stability of this solution
with respect to isotropic perturbation requires that the coupling
constant with the R2 therm in the Lagrangian of the theory
is positive, and the equations of state parameter w is located in a
rather narrow interval. Nevertheless, the stability condition does not
require violation of the strong energy condition. Taking into account
anisotropic perturbations leads to further restrictions on the values
of coupling constants and the parameter w.
Title: The Solar Orbiter mission - Exploring the Sun and heliosphere
Authors: Mueller, Daniel; Zouganelis, Yannis; Nieves-Chinchilla,
Teresa; St. Cyr, Chris
Bibcode: 2021EGUGA..23.2981M
Altcode:
Solar Orbiter, launched on 10 February 2020, is a space mission of
international collaboration between ESA and NASA. It is exploring
the linkage between the Sun and the heliosphere and has started to
collect unique data at solar distances down to 0.49 AU. By ultimately
approaching as close as 0.28 AU, Solar Orbiter will view the Sun with
very high spatial resolution and combine this with in-situ measurements
of the surrounding heliosphere. Over the course of the mission, the
highly elliptical orbit will get progressively more inclined to the
ecliptic plane. Thanks to this new perspective, Solar Orbiter will
deliver images and comprehensive data of the unexplored Sun"s polar
regions and the side of the Sun not visible from Earth. This talk
will highlight first science results from Solar Orbiter and provide
a mission status update.
Title: Analyzing 67P's dusty coma
Authors: Hänni, Nora; Altwegg, Kathrin; Müller, Daniel; Pestoni,
Boris; Rubin, Martin; Wampfler, Susanne
Bibcode: 2021EGUGA..23.1719H
Altcode:
While the volatile species in comet 67P/Churyumov-Gerasimenko"s coma
have been analyzed in great spatial and temporal detail, e.g., Rubin et
al. (2019) or Läuter et al. (2020), little is so far known about the
less volatile, heavier species. There is growing evidence, however,
that less volatile species, such as salts, may play a key role in
explaining some of the puzzling properties of comets, as for instance
shown by Altwegg et al. (2020). These authors also have demonstrated
the unique capability of ROSINA/DFMS (Rosetta Orbiter Spectrometer
for Ion and Neutral Analysis/ Double Focusing Mass Spectrometer;
Balsiger et al. (2007)) to detect exactly such little volatile species
in-situ, namely during a dust event on 5 September 2016 (when a dust
grain entered the instrument and sublimated inside).Complementary
information on 67P"s dusty coma can be obtained from data collected
during time periods of high dust activity. A clear advantage of such
data is they also allow for a quantitative interpretation thanks to
the much more stable measurement conditions. Moreover, a comparison to
data collected during a time period of little dust activity (e.g., to
the days around end of May 2015 as in Rubin et al. 2019) also allows to
link species to dust.End of July / beginning of August 2015, the comet
was approaching its perihelion and ejecting a lot of dust, as seen by
the OSIRIS camera (Vincent et al. 2016). The data from this period are
therefore a promising starting point for the search of heavier species
(m > 100 Da). Altwegg et al. (2019), for instance, reported on the
tentative identifications of the simplest polyaromatic hydrocarbon
species naphthalene as well as of benzoic acid, the simplest aromatic
carboxylic acid. To confirm these identifications and to achieve a more
complete inventory of heavier and chemically more complex species, we
are now analyzing these data sets strategically. In our contribution we
will share what we have learned from pushing the exploration of 67P"s
dusty coma. Altwegg et al., 2020, Nat. Astron., 4, 533-540.Altwegg et
al., 2019, Annu. Rev. Astron. Astrophys., 57, 113-55.Balsiger H. et al.,
2007, Space Sci. Rev., 128, 745-801.Läuter et al., 2020, MNRAS, 498,
3, 3995-4004.Rubin et al., 2019, MNRAS, 489, 594-607. Vincent et al.,
2016, MNRAS, 462 (Suppl_1), 184-194.
Title: Signatures of coronal hole substructure in the solar wind:
combined Solar Orbiter remote sensing and in situ measurements
Authors: Horbury, T. S.; Laker, R.; Rodriguez, L.; Steinvall, K.;
Maksimovic, M.; Livi, S.; Berghmans, D.; Auchere, F.; Zhukov, A. N.;
Khotyaintsev, Yu. V.; Woodham, L.; Matteini, L.; Stawarz, J.; Woolley,
T.; Bale, S. D.; Rouillard, A.; O'Brien, H.; Evans, V.; Angelini,
V.; Owen, C.; Solanki, S. K.; Nicula, B.; Muller, D.; Zouganelis, I.
Bibcode: 2021arXiv210414960H
Altcode:
Context. The Sun's complex corona is the source of the solar wind
and interplanetary magnetic field. While the large scale morphology
is well understood, the impact of variations in coronal properties
on the scale of a few degrees on properties of the interplanetary
medium is not known. Solar Orbiter, carrying both remote sensing
and in situ instruments into the inner solar system, is intended
to make these connections better than ever before. Aims. We combine
remote sensing and in situ measurements from Solar Orbiter's first
perihelion at 0.5 AU to study the fine scale structure of the solar
wind from the equatorward edge of a polar coronal hole with the aim
of identifying characteristics of the corona which can explain the in
situ variations. Methods. We use in situ measurements of the magnetic
field, density and solar wind speed to identify structures on scales
of hours at the spacecraft. Using Potential Field Source Surface
mapping we estimate the source locations of the measured solar wind
as a function of time and use EUI images to characterise these solar
sources. Results. We identify small scale stream interactions in the
solar wind with compressed magnetic field and density along with speed
variations which are associated with corrugations in the edge of the
coronal hole on scales of several degrees, demonstrating that fine
scale coronal structure can directly influence solar wind properties
and drive variations within individual streams. Conclusions. This early
analysis already demonstrates the power of Solar Orbiter's combined
remote sensing and in situ payload and shows that with future, closer
perihelia it will be possible dramatically to improve our knowledge
of the coronal sources of fine scale solar wind structure, which is
important both for understanding the phenomena driving the solar wind
and predicting its impacts at the Earth and elsewhere.
Title: On the order reduction
Authors: de Medeiros, Waleska P. F.; Müller, Daniel
Bibcode: 2021EPJC...81..231D
Altcode: 2020arXiv200900629D
In this work we present an extension of the technique of the order
reduction to higher perturbative approximations in an iterative
fashion. The intention is also to analyze more carefully the conditions
for the validity of the order reduction technique. With this in mind, a
few simple situations in which the iterative order reduction converges
analytically to the exact solutions are presented as examples. It
is discovered that the order reduction as a perturbative iterative
technique does not converge in the weak coupling limit as most
of the known perturbative schemes, at least when applied to these
examples. Also, considering these specific examples, the convergence
of the order reduction occurs in strong coupling regimes. As a more
realistic case, the order reduction is applied to Starobinsky's
inflationary model is presented. It is verified that the method
converges to the inflationary solution in the slow-roll regime.
Title: Solar Orbiter: Mission and spacecraft design
Authors: García Marirrodriga, C.; Pacros, A.; Strandmoe, S.; Arcioni,
M.; Arts, A.; Ashcroft, C.; Ayache, L.; Bonnefous, Y.; Brahimi,
N.; Cipriani, F.; Damasio, C.; De Jong, P.; Déprez, G.; Fahmy, S.;
Fels, R.; Fiebrich, J.; Hass, C.; Hernández, C.; Icardi, L.; Junge,
A.; Kletzkine, P.; Laget, P.; Le Deuff, Y.; Liebold, F.; Lodiot, S.;
Marliani, F.; Mascarello, M.; Müller, D.; Oganessian, A.; Olivier,
P.; Palombo, E.; Philippe, C.; Ragnit, U.; Ramachandran, J.; Sánchez
Pérez, J. M.; Stienstra, M. M.; Thürey, S.; Urwin, A.; Wirth, K.;
Zouganelis, I.
Bibcode: 2021A&A...646A.121G
Altcode:
The main scientific goal of Solar Orbiter is to address the central
question of heliophysics: `how does the Sun create and control
the heliosphere?' To achieve this goal, the spacecraft carries a
unique combination of ten scientific instruments (six remote-sensing
instruments and four in-situ instruments) towards the innermost
regions of the Solar System, to as close as 0.28 AU from the Sun during
segments of its orbit. The orbital inclination will be progressively
increased so that the spacecraft reaches higher solar latitudes (up
to 34° towards the end of the mission), making detailed studies of
the polar regions of the Sun possible for the first time. This paper
presents the spacecraft and its intended trip around the Sun. We
also discuss the main engineering challenges that had to be addressed
during the development cycle, instrument integration, and testing of
the spacecraft.
Title: The Solar Orbiter Mission - On its way to explore the Sun
and heliosphere
Authors: Zouganelis, Y.; Mueller, D.; Zouganelis, Y.; Gilbert, H. R.;
Nieves-Chinchilla, T.; St Cyr, O. C.
Bibcode: 2020AGUFMSH035..01Z
Altcode:
Solar Orbiter, launched on 10 February 2020 (UTC), is a space
mission of international collaboration between ESA and NASA. It
is exploring the linkage between the Sun and the heliosphere and,
during its first months of operation, has started to collect unique
data at solar distances down to 0.51 AU. By ultimately approaching
as close as 0.28 AU, Solar Orbiter will view the Sun with very high
spatial resolution and combine this with in-situ measurements of the
surrounding heliosphere. Over the course of the mission, the highly
elliptical orbit will get progressively more inclined to the ecliptic
plane. Thanks to this new perspective, Solar Orbiter will deliver images
and comprehensive data of the unexplored Sun's polar regions and the
side of the Sun not visible from Earth. This talk will highlight first
data from Solar Orbiter and provide a mission status update.
Title: Relative coronal abundance diagnostics with Solar Orbiter/SPICE
Authors: Zambrana Prado, N.; Buchlin, E.; Peter, H.; Young, P. R.;
Auchere, F.; Carlsson, M.; Fludra, A.; Hassler, D.; Aznar Cuadrado,
R.; Caminade, S.; Caldwell, M.; DeForest, C.; Fredvik, T.; Harra,
L.; Janvier, M.; Kucera, T. A.; Giunta, A. S.; Grundy, T.; Müller,
D.; Parenti, S.; Schmutz, W. K.; Schühle, U.; Sidher, S.; Teriaca,
L.; Thompson, W. T.; Williams, D.
Bibcode: 2020AGUFMSH038..09Z
Altcode:
Linking solar activity on the surface and in the corona to the inner
heliosphere is one of Solar Orbiter's main goals. Its UV spectrometer
SPICE (SPectral Imaging of the Coronal Environment) will provide
relative abundance measurements which will be key in this quest
as different structures on the Sun have different abundances as a
consequence of the FIP (First Ionization Potential) effect. Solar
Orbiter's unique combination of remote sensing and in-situ instruments
coupled with observation from other missions such as Parker Solar
Probe will allow us to compare in-situ and remote sensing composition
data. With the addition of modeling, these new results will allow us
to trace back the source of heliospheric plasma. As high telemetry
will not always be available with SPICE, we have developed a method
for measuring relative abundances that is both telemetry efficient
and reliable. Unlike methods based on Differential Emission Measure
(DEM) inversion, the Linear Combination Ratio (LCR) method does not
require a large number of spectral lines. This new method is based
on linear combinations of UV spectral lines. The coefficients of
the combinations are optimized such that the ratio of two linear
combinations of radiances would yield the relative abundance of two
elements. We present some abundance diagnostics tested on different
combinations of spectral lines observable by SPICE.
Title: 3D Visualisation of Solar Data with JHelioviewer
Authors: Mueller, D.; Nicula, B.; Verstringe, F.; Bourgoignie, B.;
Csillaghy, A.; Laube, S.; Berghmans, D.; Ireland, J.; Fleck, B.
Bibcode: 2020AGUFMSH0360001M
Altcode:
The Solar Orbiter and Parker Solar Probe missions focus on exploring
the linkage between the Sun and the heliosphere. These new missions
are collecting unique data that will allow us to study the coupling
between macroscopic physical processes to those on kinetic scales, the
generation of solar energetic particles and their propagation into the
heliosphere and the origin and acceleration of solar wind plasma. The scientific community now has access to large volumes of complex
remote-sensing and in-situ observations from different vantage points,
complemented by petabytes of simulation data. Answering overarching
science questions like "How do solar transients drive heliospheric
variability and space weather?" will only be possible if the science
community has the necessary tools at hand to visualize these data
and assimilate them into sophisticated models. A key piece
needed to bridge the gap between observables, derived quantities like
magnetic field extrapolations and model output is a tool to routinely
and intuitively visualise large heterogeneous, multidimensional,
time-dependent data sets. The open-source JHelioviewer software,
which is part of the ESA/NASA Helioviewer Project, is addressing this
need. This contribution highlights recent extensions of JHelioviewer's
functionality, in particular those of interest for Solar Orbiter.
Title: Dynamics and thermal structure in the quiet Sun seen by SPICE
Authors: Peter, H.; Aznar Cuadrado, R.; Schühle, U.; Teriaca, L.;
Auchere, F.; Carlsson, M.; Fludra, A.; Hassler, D.; Buchlin, E.;
Caminade, S.; Caldwell, M.; DeForest, C.; Fredvik, T.; Harra, L. K.;
Janvier, M.; Kucera, T. A.; Giunta, A. S.; Grundy, T.; Müller, D.;
Parenti, S.; Schmutz, W. K.; Sidher, S.; Thompson, W. T.; Williams,
D.; Young, P. R.
Bibcode: 2020AGUFMSH038..03P
Altcode:
We will present some of the early data of the Spectral Imaging of the
Coronal Environment (SPICE) instrument on Solar Orbiter. One of the
unique features of SPICE is its capability to record a wide range of
wavelengths in the extreme UV with the possibility to record spectral
lines giving access to a continuous plasma temperature range from 10.000
K to well above 1 MK. The data taken so far were for commissioning
purposes and they can be used for a preliminary evaluation of the
science performance of the instrument. Here we will concentrate on
sample spectra covering the whole wavelength region and on the early
raster maps acquired in bright lines in the quiet Sun close to disk
center. Looking at different quiet Sun features we investigate the
thermal structure of the atmosphere and flow structures. For this
we apply fits to the spectral profiles and check the performance in
terms of Doppler shifts and line widths to retrieve the structure of
the network in terms of dynamics. While the amount of data available
so far is limited, we will have a first look on how quiet Sun plasma
responds to heating events. For this, we will compare spectral lines
forming at different temperatures recorded at strictly the same time.
Title: First Results From SPICE EUV Spectrometer on Solar Orbiter
Authors: Fludra, A.; Caldwell, M.; Giunta, A. S.; Grundy, T.; Guest,
S.; Sidher, S.; Auchere, F.; Carlsson, M.; Hassler, D.; Peter, H.;
Aznar Cuadrado, R.; Buchlin, E.; Caminade, S.; DeForest, C.; Fredvik,
T.; Harra, L. K.; Janvier, M.; Kucera, T. A.; Leeks, S.; Mueller,
D.; Parenti, S.; Schmutz, W. K.; Schühle, U.; Teriaca, L.; Thompson,
W. T.; Tustain, S.; Williams, D.; Young, P. R.
Bibcode: 2020AGUFMSH038..02F
Altcode:
SPICE (Spectral Imaging of Coronal Environment) is one of the remote
sensing instruments onboard Solar Orbiter. It is an EUV imaging
spectrometer observing the Sun in two wavelength bands: 69.6-79.4 nm
and 96.6-105.1 nm. SPICE is capable of recording full spectra in these
bands with exposures as short as 1s. SPICE is the only Solar Orbiter
instrument that can measure EUV spectra from the disk and low corona
of the Sun and record all spectral lines simultaneously. SPICE uses
one of three narrow slits, 2"x11', 4''x11', 6''x11', or a wide slit
30''x14'. The primary mirror can be scanned in a direction perpendicular
to the slit, allowing raster images of up to 16' in size. We
present an overview of the first SPICE data taken on several days
during the instrument commissioning carried out by the RAL Space team
between 2020 April 21 and 2020 June 14. We also include results from
SPICE observations at the first Solar Orbiter perihelion at 0.52AU,
taken between June 16-21st. We give examples of full spectra
from the quiet Sun near disk centre and provide a list of key spectral
lines emitted in a range of temperatures between 10,000 K and over 1
million K, from neutral hydrogen and ions of carbon, oxygen, nitrogen,
neon, sulphur and magnesium. We show examples of first raster images
in several strong lines, obtained with different slits and a range
of exposure times between 5s and 180s. We describe the temperature
coverage and density diagnostics, determination of plasma flows, and
discuss possible applications to studies of the elemental abundances
in the corona. We also show the first off-limb measurements with SPICE,
as obtained when the spacecraft pointed at the limb.
Title: Calibrating optical distortions in the Solar Orbiter SPICE
spectrograph
Authors: Thompson, W. T.; Schühle, U.; Young, P. R.; Auchere, F.;
Carlsson, M.; Fludra, A.; Hassler, D.; Peter, H.; Aznar Cuadrado, R.;
Buchlin, E.; Caldwell, M.; DeForest, C.; Fredvik, T.; Harra, L. K.;
Janvier, M.; Kucera, T. A.; Giunta, A. S.; Grundy, T.; Müller, D.;
Parenti, S.; Caminade, S.; Schmutz, W. K.; Teriaca, L.; Williams,
D.; Sidher, S.
Bibcode: 2020AGUFMSH0360029T
Altcode:
The Spectral Imaging of the Coronal Environment (SPICE) instrument on
Solar Orbiter is a high-resolution imaging spectrometer operating
at extreme ultraviolet (EUV) wavelengths from 70.4-79.0 nm and
97.3-104.9 nm. A single-mirror off-axis paraboloid focuses the solar
image onto the entrance slit of the spectrometer section. A Toroidal
Variable Line Space (TVLS) grating images the entrance slit onto a
pair of MCP-intensified APS detectors. Ray-tracing analysis prior
to launch showed that the instrument was subject to a number of
small image distortions which need to be corrected in the final data
product. We compare the ray tracing results with measurements made in
flight. Co-alignment with other telescopes on Solar Orbiter will also
be examined.
Title: First results from the EUI and SPICE observations of Alpha
Leo near Solar Orbiter first perihelion
Authors: Buchlin, E.; Teriaca, L.; Giunta, A. S.; Grundy, T.; Andretta,
V.; Auchere, F.; Peter, H.; Berghmans, D.; Carlsson, M.; Fludra, A.;
Harra, L.; Hassler, D.; Long, D.; Rochus, P. L.; Schühle, U.; Aznar
Cuadrado, R.; Caldwell, M.; Caminade, S.; DeForest, C.; Fredvik, T.;
Gissot, S.; Heerlein, K.; Janvier, M.; Kraaikamp, E.; Kucera, T. A.;
Müller, D.; Parenti, S.; Schmutz, W. K.; Sidher, S.; Smith, P.;
Stegen, K.; Thompson, W. T.; Verbeeck, C.; Williams, D.; Young, P. R.
Bibcode: 2020AGUFMSH0360024B
Altcode:
On June 16th 2020 Solar Orbiter made a dedicated observing campaign
where the spacecraft pointed to the solar limb to allow some of the
high resolution instruments to observe the ingress (at the east limb)
and later the egress (west limb) of the occultation of the star Alpha
Leonis by the solar disk. The star was chosen because its luminosity and
early spectral type ensure high and stable flux at wavelengths between
100 and 122 nanometers, a range observed by the High Resolution EUI
Lyman alpha telescope (HRI-LYA) and by the long wavelength channel
of the SPICE spectrograph. Star observations, when feasible, allow
to gather a great deal of information on the instrument performances,
such as the radiometric performance and the instrument optical point
spread function (PSF). We report here the first results from the
above campaign for the two instruments.
Title: Solar Orbiter: connecting remote sensing and in situ
measurements
Authors: Horbury, T. S.; Auchere, F.; Antonucci, E.; Berghmans, D.;
Bruno, R.; Carlsson, M.; del Toro Iniesta, J. C.; Fludra, A.; Harra,
L.; Hassler, D.; Heinzel, P.; Howard, R. A.; Krucker, S.; Livi, S. A.;
Long, D.; Louarn, P.; Maksimovic, M.; Mueller, D.; Owen, C. J.; Peter,
H.; Rochus, P. L.; Rodriguez-Pacheco, J.; Romoli, M.; Schühle, U.;
Solanki, S. K.; Teriaca, L.; Wimmer-Schweingruber, R. F.; Zouganelis,
Y.; Laker, R.
Bibcode: 2020AGUFMSH038..10H
Altcode:
A key science goal of the Solar Orbiter mission is to make connections
between phenomena on the Sun and their manifestations in interplanetary
space. To that end, the spacecraft carries a carefully tailored
payload of six remote sensing instruments and four making in situ
measurements. During June 2020, while the spacecraft was around 0.5
AU from the Sun, the remote sensing instruments operated for several
days. While this was primarily an engineering activity, the resulting
observations provided outstanding measurements and represent the ideal
first opportunity to investigate the potential for making connections
between the remote sensing and in situ payloads on Solar Orbiter. We present a preliminary analysis of the available remote sensing and
in situ observations, showing how connections can be made, and discuss
the potential for further, more precise mapping to be performed as
the mission progresses.
Title: First results from combined EUI and SPICE observations of
Lyman lines of Hydrogen and He II
Authors: Teriaca, L.; Aznar Cuadrado, R.; Giunta, A. S.; Grundy, T.;
Parenti, S.; Auchere, F.; Vial, J. C.; Fludra, A.; Berghmans, D.;
Carlsson, M.; Harra, L.; Hassler, D.; Long, D.; Peter, H.; Rochus,
P. L.; Schühle, U.; Buchlin, E.; Caldwell, M.; Caminade, S.; DeForest,
C.; Fredvik, T.; Gissot, S.; Heerlein, K.; Janvier, M.; Kraaikamp,
E.; Kucera, T. A.; Mueller, D.; Schmutz, W. K.; Sidher, S.; Smith, P.;
Stegen, K.; Thompson, W. T.; Verbeeck, C.; Williams, D.; Young, P. R.
Bibcode: 2020AGUFMSH0360003T
Altcode:
The Solar Orbiter spacecraft carries a powerful set of remote
sensing instruments that allow studying the solar atmosphere with
unprecedented diagnostic capabilities. Many such diagnostics require
the simultaneous usage of more than one instrument. One example of that
is the capability, for the first time, to obtain (near) simultaneous
spatially resolved observations of the emission from the first three
lines of the Lyman series of hydrogen and of He II Lyman alpha. In fact,
the SPectral Imaging of the Coronal Environment (SPICE) spectrometer
can observe the Lyman beta and gamma lines in its long wavelength
(SPICE-LW) channel, the High Resolution Lyman Alpha (HRI-LYA) telescope
of the Extreme Ultraviolet Imager (EUI) acquires narrow band images in
the Lyman alpha line while the Full Disk Imager (FSI) of EUI can take
images dominated by the Lyman alpha line of ionized Helium at 30.4 nm
(FSI-304). Being hydrogen and helium the main components of our star,
these very bright transitions play an important role in the energy
budget of the outer atmosphere via radiative losses and the measurement
of their profiles and radiance ratios is a fundamental constraint to
any comprehensive modelization effort of the upper solar chromosphere
and transition region. Additionally, monitoring their average ratios
can serve as a check out for the relative radiometric performance of
the two instruments throughout the mission. Although the engineering
data acquired so far are far from ideal in terms of time simultaneity
(often only within about 1 h) and line coverage (often only Lyman beta
was acquired by SPICE and not always near simultaneous images from all
three telescopes are available) the analysis we present here still
offers a great opportunity to have a first look at the potential of
this diagnostic from the two instruments. In fact, we have identified
a series of datasets obtained at disk center and at various positions
at the solar limb that allow studying the Lyman alpha to beta radiance
ratio and their relation to He II 30.4 as a function of the position
on the Sun (disk center versus limb and quiet Sun versus coronal holes).
Title: Evidence for Top Quark Production in Nucleus-Nucleus Collisions
Authors: Sirunyan, A. M.; Tumasyan, A.; Adam, W.; Ambrogi, F.;
Bergauer, T.; Dragicevic, M.; Erö, J.; Escalante Del Valle, A.;
Frühwirth, R.; Jeitler, M.; Krammer, N.; Lechner, L.; Liko, D.;
Madlener, T.; Mikulec, I.; Rad, N.; Schieck, J.; Schöfbeck, R.;
Spanring, M.; Templ, S.; Waltenberger, W.; Wulz, C. -E.; Zarucki,
M.; Chekhovsky, V.; Litomin, A.; Makarenko, V.; Suarez Gonzalez, J.;
Darwish, M. R.; De Wolf, E. A.; Di Croce, D.; Janssen, X.; Kello,
T.; Lelek, A.; Pieters, M.; Rejeb Sfar, H.; Van Haevermaet, H.; Van
Mechelen, P.; Van Putte, S.; Van Remortel, N.; Blekman, F.; Bols,
E. S.; Chhibra, S. S.; D'Hondt, J.; De Clercq, J.; Lontkovskyi, D.;
Lowette, S.; Marchesini, I.; Moortgat, S.; Python, Q.; Tavernier, S.;
Van Doninck, W.; Van Mulders, P.; Beghin, D.; Bilin, B.; Clerbaux, B.;
De Lentdecker, G.; Delannoy, H.; Dorney, B.; Favart, L.; Grebenyuk,
A.; Kalsi, A. K.; Makarenko, I.; Moureaux, L.; Pétré, L.; Popov,
A.; Postiau, N.; Starling, E.; Thomas, L.; Vander Velde, C.; Vanlaer,
P.; Vannerom, D.; Wezenbeek, L.; Cornelis, T.; Dobur, D.; Khvastunov,
I.; Niedziela, M.; Roskas, C.; Skovpen, K.; Tytgat, M.; Verbeke, W.;
Vermassen, B.; Vit, M.; Bruno, G.; Bury, F.; Caputo, C.; David, P.;
Delaere, C.; Delcourt, M.; Donertas, I. S.; Giammanco, A.; Lemaitre,
V.; Prisciandaro, J.; Saggio, A.; Taliercio, A.; Teklishyn, M.;
Vischia, P.; Wuyckens, S.; Zobec, J.; Alves, G. A.; Correia Silva,
G.; Hensel, C.; Moraes, A.; Aldá Júnior, W. L.; Belchior Batista
Das Chagas, E.; Carvalho, W.; Chinellato, J.; Coelho, E.; Da Costa,
E. M.; Da Silveira, G. G.; De Jesus Damiao, D.; Fonseca De Souza, S.;
Malbouisson, H.; Martins, J.; Matos Figueiredo, D.; Medina Jaime, M.;
Melo De Almeida, M.; Mora Herrera, C.; Mundim, L.; Nogima, H.; Rebello
Teles, P.; Sanchez Rosas, L. J.; Santoro, A.; Silva Do Amaral, S. M.;
Sznajder, A.; Thiel, M.; Tonelli Manganote, E. J.; Torres Da Silva
De Araujo, F.; Vilela Pereira, A.; Bernardes, C. A.; Calligaris,
L.; Fernandez Perez Tomei, T. R.; Gregores, E. M.; Lemos, D. S.;
Mercadante, P. G.; Novaes, S. F.; Padula, Sandra S.; Aleksandrov, A.;
Antchev, G.; Atanasov, I.; Hadjiiska, R.; Iaydjiev, P.; Misheva, M.;
Rodozov, M.; Shopova, M.; Sultanov, G.; Bonchev, M.; Dimitrov, A.;
Ivanov, T.; Litov, L.; Pavlov, B.; Petkov, P.; Petrov, A.; Fang, W.;
Guo, Q.; Wang, H.; Yuan, L.; Ahmad, M.; Hu, Z.; Wang, Y.; Chapon, E.;
Chen, G. M.; Chen, H. S.; Chen, M.; Jiang, C. H.; Leggat, D.; Liao,
H.; Liu, Z.; Sharma, R.; Spiezia, A.; Tao, J.; Wang, J.; Zhang, H.;
Zhang, S.; Zhao, J.; Agapitos, A.; Ban, Y.; Chen, C.; Chen, G.; Levin,
A.; Li, J.; Li, L.; Li, Q.; Lyu, X.; Mao, Y.; Qian, S. J.; Wang, D.;
Wang, Q.; Xiao, J.; You, Z.; Gao, X.; Xiao, M.; Avila, C.; Cabrera,
A.; Florez, C.; Fraga, J.; Sarkar, A.; Segura Delgado, M. A.; Mejia
Guisao, J.; Ramirez, F.; Ruiz Alvarez, J. D.; Salazar González,
C. A.; Vanegas Arbelaez, N.; Giljanovic, D.; Godinovic, N.; Lelas,
D.; Puljak, I.; Sculac, T.; Antunovic, Z.; Kovac, M.; Brigljevic, V.;
Ferencek, D.; Majumder, D.; Mesic, B.; Roguljic, M.; Starodumov, A.;
Susa, T.; Ather, M. W.; Attikis, A.; Erodotou, E.; Ioannou, A.; Kole,
G.; Kolosova, M.; Konstantinou, S.; Mavromanolakis, G.; Mousa, J.;
Nicolaou, C.; Ptochos, F.; Razis, P. A.; Rykaczewski, H.; Saka, H.;
Tsiakkouri, D.; Finger, M.; Finger, M.; Kveton, A.; Tomsa, J.; Ayala,
E.; Carrera Jarrin, E.; Salama, E.; Lotfy, A.; Mahmoud, M. A.; Bhowmik,
S.; Carvalho Antunes De Oliveira, A.; Dewanjee, R. K.; Ehataht,
K.; Kadastik, M.; Raidal, M.; Veelken, C.; Eerola, P.; Forthomme,
L.; Kirschenmann, H.; Osterberg, K.; Voutilainen, M.; Brücken, E.;
Garcia, F.; Havukainen, J.; Karimäki, V.; Kim, M. S.; Kinnunen, R.;
Lampén, T.; Lassila-Perini, K.; Laurila, S.; Lehti, S.; Lindén, T.;
Siikonen, H.; Tuominen, E.; Tuominiemi, J.; Luukka, P.; Tuuva, T.;
Besancon, M.; Couderc, F.; Dejardin, M.; Denegri, D.; Faure, J. L.;
Ferri, F.; Ganjour, S.; Givernaud, A.; Gras, P.; Hamel de Monchenault,
G.; Jarry, P.; Leloup, C.; Lenzi, B.; Locci, E.; Malcles, J.; Rander,
J.; Rosowsky, A.; Sahin, M. Ö.; Savoy-Navarro, A.; Titov, M.; Yu,
G. B.; Ahuja, S.; Amendola, C.; Beaudette, F.; Bonanomi, M.; Busson,
P.; Charlot, C.; Davignon, O.; Diab, B.; Falmagne, G.; Granier de
Cassagnac, R.; Kucher, I.; Lobanov, A.; Martin Perez, C.; Nguyen, M.;
Ochando, C.; Paganini, P.; Rembser, J.; Salerno, R.; Sauvan, J. B.;
Sirois, Y.; Zabi, A.; Zghiche, A.; Agram, J. -L.; Andrea, J.; Bloch,
D.; Bourgatte, G.; Brom, J. -M.; Chabert, E. C.; Collard, C.; Fontaine,
J. -C.; Gelé, D.; Goerlach, U.; Grimault, C.; Le Bihan, A. -C.; Van
Hove, P.; Asilar, E.; Beauceron, S.; Bernet, C.; Boudoul, G.; Camen,
C.; Carle, A.; Chanon, N.; Chierici, R.; Contardo, D.; Depasse, P.;
El Mamouni, H.; Fay, J.; Gascon, S.; Gouzevitch, M.; Ille, B.; Jain,
Sa.; Laktineh, I. B.; Lattaud, H.; Lesauvage, A.; Lethuillier, M.;
Mirabito, L.; Torterotot, L.; Touquet, G.; Vander Donckt, M.; Viret,
S.; Khvedelidze, A.; Tsamalaidze, Z.; Feld, L.; Klein, K.; Lipinski,
M.; Meuser, D.; Pauls, A.; Preuten, M.; Rauch, M. P.; Schulz, J.;
Teroerde, M.; Eliseev, D.; Erdmann, M.; Fackeldey, P.; Fischer, B.;
Ghosh, S.; Hebbeker, T.; Hoepfner, K.; Keller, H.; Mastrolorenzo,
L.; Merschmeyer, M.; Meyer, A.; Millet, P.; Mocellin, G.; Mondal,
S.; Mukherjee, S.; Noll, D.; Novak, A.; Pook, T.; Pozdnyakov, A.;
Quast, T.; Radziej, M.; Rath, Y.; Reithler, H.; Roemer, J.; Schmidt,
A.; Schuler, S. C.; Sharma, A.; Wiedenbeck, S.; Zaleski, S.; Dziwok,
C.; Flügge, G.; Haj Ahmad, W.; Hlushchenko, O.; Kress, T.; Nowack,
A.; Pistone, C.; Pooth, O.; Roy, D.; Sert, H.; Stahl, A.; Ziemons,
T.; Aarup Petersen, H.; Aldaya Martin, M.; Asmuss, P.; Babounikau,
I.; Baxter, S.; Behnke, O.; Bermúdez Martínez, A.; Bin Anuar,
A. A.; Borras, K.; Botta, V.; Brunner, D.; Campbell, A.; Cardini,
A.; Connor, P.; Consuegra Rodríguez, S.; Danilov, V.; De Wit, A.;
Defranchis, M. M.; Didukh, L.; Domínguez Damiani, D.; Eckerlin, G.;
Eckstein, D.; Eichhorn, T.; Elwood, A.; Estevez Banos, L. I.; Gallo,
E.; Geiser, A.; Giraldi, A.; Grohsjean, A.; Guthoff, M.; Haranko, M.;
Harb, A.; Jafari, A.; Jomhari, N. Z.; Jung, H.; Kasem, A.; Kasemann,
M.; Kaveh, H.; Keaveney, J.; Kleinwort, C.; Knolle, J.; Krücker,
D.; Lange, W.; Lenz, T.; Lidrych, J.; Lipka, K.; Lohmann, W.; Mankel,
R.; Melzer-Pellmann, I. -A.; Metwally, J.; Meyer, A. B.; Meyer, M.;
Missiroli, M.; Mnich, J.; Mussgiller, A.; Myronenko, V.; Otarid, Y.;
Pérez Adán, D.; Pflitsch, S. K.; Pitzl, D.; Raspereza, A.; Saibel,
A.; Savitskyi, M.; Scheurer, V.; Schütze, P.; Schwanenberger,
C.; Shevchenko, R.; Singh, A.; Sosa Ricardo, R. E.; Tholen, H.;
Tonon, N.; Turkot, O.; Vagnerini, A.; Van De Klundert, M.; Walsh,
R.; Walter, D.; Wen, Y.; Wichmann, K.; Wissing, C.; Wuchterl, S.;
Zenaiev, O.; Zlebcik, R.; Aggleton, R.; Bein, S.; Benato, L.; Benecke,
A.; De Leo, K.; Dreyer, T.; Ebrahimi, A.; Feindt, F.; Fröhlich, A.;
Garbers, C.; Garutti, E.; Gonzalez, D.; Gunnellini, P.; Haller, J.;
Hinzmann, A.; Karavdina, A.; Kasieczka, G.; Klanner, R.; Kogler, R.;
Kurz, S.; Kutzner, V.; Lange, J.; Lange, T.; Malara, A.; Multhaup, J.;
Niemeyer, C. E. N.; Nigamova, A.; Pena Rodriguez, K. J.; Reimers, A.;
Rieger, O.; Schleper, P.; Schumann, S.; Schwandt, J.; Schwarz, D.;
Sonneveld, J.; Stadie, H.; Steinbrück, G.; Vormwald, B.; Zoi, I.;
Akbiyik, M.; Baselga, M.; Baur, S.; Bechtel, J.; Berger, T.; Butz,
E.; Caspart, R.; Chwalek, T.; De Boer, W.; Dierlamm, A.; El Morabit,
K.; Faltermann, N.; Flöh, K.; Giffels, M.; Gottmann, A.; Hartmann,
F.; Heidecker, C.; Husemann, U.; Iqbal, M. A.; Katkov, I.; Kudella,
S.; Maier, S.; Metzler, M.; Mitra, S.; Mozer, M. U.; Müller, D.;
Müller, Th.; Musich, M.; Quast, G.; Rabbertz, K.; Rauser, J.;
Savoiu, D.; Schäfer, D.; Schnepf, M.; Schröder, M.; Seith, D.;
Shvetsov, I.; Simonis, H. J.; Ulrich, R.; Wassmer, M.; Weber, M.;
Wöhrmann, C.; Wolf, R.; Wozniewski, S.; Anagnostou, G.; Asenov, P.;
Daskalakis, G.; Geralis, T.; Kyriakis, A.; Loukas, D.; Paspalaki,
G.; Stakia, A.; Diamantopoulou, M.; Karasavvas, D.; Karathanasis, G.;
Kontaxakis, P.; Koraka, C. K.; Manousakis-katsikakis, A.; Panagiotou,
A.; Papavergou, I.; Saoulidou, N.; Theofilatos, K.; Vellidis,
K.; Vourliotis, E.; Bakas, G.; Kousouris, K.; Papakrivopoulos,
I.; Tsipolitis, G.; Zacharopoulou, A.; Evangelou, I.; Foudas, C.;
Gianneios, P.; Katsoulis, P.; Kokkas, P.; Mallios, S.; Manitara, K.;
Manthos, N.; Papadopoulos, I.; Strologas, J.; Tsitsonis, D.; Bartók,
M.; Chudasama, R.; Csanad, M.; Gadallah, M. M. A.; Major, P.; Mandal,
K.; Mehta, A.; Pasztor, G.; Surányi, O.; Veres, G. I.; Bencze, G.;
Hajdu, C.; Horvath, D.; Sikler, F.; Veszpremi, V.; Vesztergombi,
G.; Beni, N.; Czellar, S.; Karancsi, J.; Molnar, J.; Szillasi, Z.;
Teyssier, D.; Raics, P.; Trocsanyi, Z. L.; Ujvari, B.; Csorgo, T.;
Lökös, S.; Nemes, F.; Novak, T.; Choudhury, S.; Komaragiri, J. R.;
Kumar, D.; Panwar, L.; Tiwari, P. C.; Bahinipati, S.; Dash, D.; Kar,
C.; Mal, P.; Mishra, T.; Muraleedharan Nair Bindhu, V. K.; Nayak,
A.; Sahoo, D. K.; Sur, N.; Swain, S. K.; Bansal, S.; Beri, S. B.;
Bhatnagar, V.; Chauhan, S.; Dhingra, N.; Gupta, R.; Kaur, A.; Kaur,
A.; Kaur, S.; Kumari, P.; Lohan, M.; Meena, M.; Sandeep, K.; Sharma,
S.; Singh, J. B.; Virdi, A. K.; Ahmed, A.; Bhardwaj, A.; Choudhary,
B. C.; Garg, R. B.; Gola, M.; Keshri, S.; Kumar, A.; Naimuddin, M.;
Priyanka, P.; Ranjan, K.; Shah, A.; Bharti, M.; Bhattacharya, R.;
Bhattacharya, S.; Bhowmik, D.; Dutta, S.; Ghosh, S.; Gomber, B.;
Maity, M.; Mondal, K.; Nandan, S.; Palit, P.; Purohit, A.; Rout,
P. K.; Saha, G.; Sarkar, S.; Sharan, M.; Singh, B.; Thakur, S.;
Behera, P. K.; Behera, S. C.; Kalbhor, P.; Muhammad, A.; Pradhan,
R.; Pujahari, P. R.; Sharma, A.; Sikdar, A. K.; Dutta, D.; Jha, V.;
Kumar, V.; Mishra, D. K.; Naskar, K.; Netrakanti, P. K.; Pant, L. M.;
Shukla, P.; Aziz, T.; Bhat, M. A.; Dugad, S.; Kumar Verma, R.; Sarkar,
U.; Banerjee, S.; Bhattacharya, S.; Chatterjee, S.; Das, P.; Guchait,
M.; Karmakar, S.; Kumar, S.; Majumder, G.; Mazumdar, K.; Mukherjee,
S.; Roy, D.; Sahoo, N.; Dube, S.; Kansal, B.; Kapoor, A.; Kothekar,
K.; Pandey, S.; Rane, A.; Rastogi, A.; Sharma, S.; Bakhshiansohi,
H.; Chenarani, S.; Etesami, S. M.; Khakzad, M.; Mohammadi Najafabadi,
M.; Naseri, M.; Felcini, M.; Grunewald, M.; Abbrescia, M.; Aly, R.;
Aruta, C.; Calabria, C.; Colaleo, A.; Creanza, D.; De Filippis, N.;
De Palma, M.; Di Florio, A.; Di Pilato, A.; Elmetenawee, W.; Fiore,
L.; Gelmi, A.; Iaselli, G.; Ince, M.; Lezki, S.; Maggi, G.; Maggi,
M.; Margjeka, I.; Merlin, J. A.; My, S.; Nuzzo, S.; Pompili, A.;
Pugliese, G.; Ranieri, A.; Selvaggi, G.; Silvestris, L.; Simone,
F. M.; Venditti, R.; Verwilligen, P.; Abbiendi, G.; Battilana, C.;
Bonacorsi, D.; Borgonovi, L.; Braibant-Giacomelli, S.; Campanini, R.;
Capiluppi, P.; Castro, A.; Cavallo, F. R.; Ciocca, C.; Cuffiani, M.;
Dallavalle, G. M.; Diotalevi, T.; Fabbri, F.; Fanfani, A.; Fontanesi,
E.; Giacomelli, P.; Grandi, C.; Guiducci, L.; Iemmi, F.; Lo Meo,
S.; Marcellini, S.; Masetti, G.; Navarria, F. L.; Perrotta, A.;
Primavera, F.; Rossi, A. M.; Rovelli, T.; Siroli, G. P.; Tosi, N.;
Albergo, S.; Costa, S.; Di Mattia, A.; Potenza, R.; Tricomi, A.; Tuve,
C.; Barbagli, G.; Cassese, A.; Ceccarelli, R.; Ciulli, V.; Civinini,
C.; D'Alessandro, R.; Fiori, F.; Focardi, E.; Latino, G.; Lenzi, P.;
Lizzo, M.; Meschini, M.; Paoletti, S.; Seidita, R.; Sguazzoni, G.;
Viliani, L.; Benussi, L.; Bianco, S.; Piccolo, D.; Bozzo, M.; Ferro,
F.; Mulargia, R.; Robutti, E.; Tosi, S.; Benaglia, A.; Beschi, A.;
Brivio, F.; Cetorelli, F.; Ciriolo, V.; De Guio, F.; Dinardo, M. E.;
Dini, P.; Gennai, S.; Ghezzi, A.; Govoni, P.; Guzzi, L.; Malberti,
M.; Malvezzi, S.; Menasce, D.; Monti, F.; Moroni, L.; Paganoni, M.;
Pedrini, D.; Ragazzi, S.; Tabarelli de Fatis, T.; Valsecchi, D.; Zuolo,
D.; Buontempo, S.; Cavallo, N.; De Iorio, A.; Fabozzi, F.; Fienga,
F.; Iorio, A. O. M.; Layer, L.; Lista, L.; Meola, S.; Paolucci,
P.; Rossi, B.; Sciacca, C.; Voevodina, E.; Azzi, P.; Bacchetta,
N.; Bisello, D.; Boletti, A.; Bragagnolo, A.; Carlin, R.; Checchia,
P.; De Castro Manzano, P.; Dorigo, T.; Dosselli, U.; Gasparini, F.;
Gasparini, U.; Hoh, S. Y.; Margoni, M.; Meneguzzo, A. T.; Presilla, M.;
Ronchese, P.; Rossin, R.; Simonetto, F.; Strong, G.; Tiko, A.; Tosi,
M.; Zanetti, M.; Zotto, P.; Zucchetta, A.; Zumerle, G.; Braghieri,
A.; Calzaferri, S.; Fiorina, D.; Montagna, P.; Ratti, S. P.; Re,
V.; Ressegotti, M.; Riccardi, C.; Salvini, P.; Vai, I.; Vitulo, P.;
Biasini, M.; Bilei, G. M.; Ciangottini, D.; Fanò, L.; Lariccia, P.;
Mantovani, G.; Mariani, V.; Menichelli, M.; Moscatelli, F.; Rossi, A.;
Santocchia, A.; Spiga, D.; Tedeschi, T.; Androsov, K.; Azzurri, P.;
Bagliesi, G.; Bertacchi, V.; Bianchini, L.; Boccali, T.; Castaldi, R.;
Ciocci, M. A.; Dell'Orso, R.; Di Domenico, M. R.; Donato, S.; Giannini,
L.; Giassi, A.; Grippo, M. T.; Ligabue, F.; Manca, E.; Mandorli, G.;
Messineo, A.; Palla, F.; Rizzi, A.; Rolandi, G.; Roy Chowdhury, S.;
Scribano, A.; Shafiei, N.; Spagnolo, P.; Tenchini, R.; Tonelli, G.;
Turini, N.; Venturi, A.; Verdini, P. G.; Cavallari, F.; Cipriani,
M.; Del Re, D.; Di Marco, E.; Diemoz, M.; Longo, E.; Meridiani, P.;
Organtini, G.; Pandolfi, F.; Paramatti, R.; Quaranta, C.; Rahatlou, S.;
Rovelli, C.; Santanastasio, F.; Soffi, L.; Tramontano, R.; Amapane,
N.; Arcidiacono, R.; Argiro, S.; Arneodo, M.; Bartosik, N.; Bellan,
R.; Bellora, A.; Biino, C.; Cappati, A.; Cartiglia, N.; Cometti, S.;
Costa, M.; Covarelli, R.; Demaria, N.; Kiani, B.; Legger, F.; Mariotti,
C.; Maselli, S.; Migliore, E.; Monaco, V.; Monteil, E.; Monteno, M.;
Obertino, M. M.; Ortona, G.; Pacher, L.; Pastrone, N.; Pelliccioni,
M.; Pinna Angioni, G. L.; Ruspa, M.; Salvatico, R.; Siviero, F.; Sola,
V.; Solano, A.; Soldi, D.; Staiano, A.; Trocino, D.; Belforte, S.;
Candelise, V.; Casarsa, M.; Cossutti, F.; Da Rold, A.; Della Ricca,
G.; Vazzoler, F.; Dogra, S.; Huh, C.; Kim, B.; Kim, D. H.; Kim, G. N.;
Lee, J.; Lee, S. W.; Moon, C. S.; Oh, Y. D.; Pak, S. I.; Sekmen, S.;
Yang, Y. C.; Kim, H.; Moon, D. H.; Francois, B.; Kim, T. J.; Park,
J.; Cho, S.; Choi, S.; Go, Y.; Ha, S.; Hong, B.; Lee, K.; Lee, K. S.;
Lim, J.; Park, J.; Park, S. K.; Roh, Y.; Yoo, J.; Goh, J.; Gurtu,
A.; Kim, H. S.; Kim, Y.; Almond, J.; Bhyun, J. H.; Choi, J.; Jeon,
S.; Kim, J.; Kim, J. S.; Ko, S.; Kwon, H.; Lee, H.; Lee, K.; Lee, S.;
Nam, K.; Oh, B. H.; Oh, M.; Oh, S. B.; Radburn-Smith, B. C.; Seo, H.;
Yang, U. K.; Yoon, I.; Jeon, D.; Kim, J. H.; Ko, B.; Lee, J. S. H.;
Park, I. C.; Watson, I. J.; Yoo, H. D.; Choi, Y.; Hwang, C.; Jeong,
Y.; Lee, H.; Lee, J.; Lee, Y.; Yu, I.; Veckalns, V.; Juodagalvis, A.;
Rinkevicius, A.; Tamulaitis, G.; Wan Abdullah, W. A. T.; Yusli, M. N.;
Zolkapli, Z.; Benitez, J. F.; Castaneda Hernandez, A.; Murillo Quijada,
J. A.; Valencia Palomo, L.; Castilla-Valdez, H.; De La Cruz-Burelo,
E.; Heredia-De La Cruz, I.; Lopez-Fernandez, R.; Sanchez-Hernandez,
A.; Carrillo Moreno, S.; Oropeza Barrera, C.; Ramirez-Garcia, M.;
Vazquez Valencia, F.; Eysermans, J.; Pedraza, I.; Salazar Ibarguen,
H. A.; Uribe Estrada, C.; Morelos Pineda, A.; Mijuskovic, J.; Raicevic,
N.; Krofcheck, D.; Bheesette, S.; Butler, P. H.; Ahmad, A.; Asghar,
M. I.; Awan, M. I. M.; Hassan, Q.; Hoorani, H. R.; Khan, W. A.; Shah,
M. A.; Shoaib, M.; Waqas, M.; Avati, V.; Grzanka, L.; Malawski, M.;
Bialkowska, H.; Bluj, M.; Boimska, B.; Frueboes, T.; Górski, M.;
Kazana, M.; Szleper, M.; Traczyk, P.; Zalewski, P.; Bunkowski, K.;
Byszuk, A.; Doroba, K.; Kalinowski, A.; Konecki, M.; Krolikowski,
J.; Olszewski, M.; Walczak, M.; Araujo, M.; Bargassa, P.; Bastos, D.;
Di Francesco, A.; Faccioli, P.; Galinhas, B.; Gallinaro, M.; Hollar,
J.; Leonardo, N.; Niknejad, T.; Seixas, J.; Shchelina, K.; Toldaiev,
O.; Varela, J.; Afanasiev, S.; Gavrilenko, M.; Golunov, A.; Golutvin,
I.; Gorbounov, N.; Gorbunov, I.; Kamenev, A.; Karjavine, V.; Korenkov,
V.; Lanev, A.; Malakhov, A.; Matveev, V.; Moisenz, P.; Palichik, V.;
Perelygin, V.; Seitova, D.; Shmatov, S.; Smirnov, V.; Teryaev, O.;
Voytishin, N.; Zarubin, A.; Gavrilov, G.; Golovtcov, V.; Ivanov, Y.;
Kim, V.; Kuznetsova, E.; Murzin, V.; Oreshkin, V.; Smirnov, I.; Sosnov,
D.; Sulimov, V.; Uvarov, L.; Volkov, S.; Vorobyev, A.; Andreev, Yu.;
Dermenev, A.; Gninenko, S.; Golubev, N.; Karneyeu, A.; Kirsanov, M.;
Krasnikov, N.; Pashenkov, A.; Pivovarov, G.; Tlisov, D.; Toropin, A.;
Epshteyn, V.; Gavrilov, V.; Lychkovskaya, N.; Nikitenko, A.; Popov,
V.; Pozdnyakov, I.; Safronov, G.; Spiridonov, A.; Stepennov, A.;
Toms, M.; Vlasov, E.; Zhokin, A.; Aushev, T.; Chistov, R.; Danilov,
M.; Parygin, P.; Philippov, D.; Polikarpov, S.; Andreev, V.; Azarkin,
M.; Dremin, I.; Kirakosyan, M.; Terkulov, A.; Baskakov, A.; Belyaev,
A.; Boos, E.; Dudko, L.; Ershov, A.; Gribushin, A.; Kodolova, O.;
Korotkikh, V.; Lokhtin, I.; Obraztsov, S.; Petrushanko, S.; Savrin,
V.; Snigirev, A.; Blinov, V.; Dimova, T.; Kardapoltsev, L.; Ovtin,
I.; Skovpen, Y.; Azhgirey, I.; Bayshev, I.; Kachanov, V.; Kalinin,
A.; Konstantinov, D.; Petrov, V.; Ryutin, R.; Sobol, A.; Troshin,
S.; Tyurin, N.; Uzunian, A.; Volkov, A.; Babaev, A.; Iuzhakov, A.;
Okhotnikov, V.; Borchsh, V.; Ivanchenko, V.; Tcherniaev, E.; Adzic, P.;
Cirkovic, P.; Dordevic, M.; Milenovic, P.; Milosevic, J.; Stojanovic,
M.; Aguilar-Benitez, M.; Alcaraz Maestre, J.; Álvarez Fernández, A.;
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S.; O'Dell, V.; Papadimitriou, V.; Pedro, K.; Pena, C.; Prokofyev,
O.; Ravera, F.; Reinsvold Hall, A.; Ristori, L.; Schneider, B.;
Sexton-Kennedy, E.; Smith, N.; Soha, A.; Spalding, W. J.; Spiegel,
L.; Stoynev, S.; Strait, J.; Taylor, L.; Tkaczyk, S.; Tran, N. V.;
Uplegger, L.; Vaandering, E. W.; Wang, M.; Weber, H. A.; Woodard,
A.; Acosta, D.; Avery, P.; Bourilkov, D.; Cadamuro, L.; Cherepanov,
V.; Errico, F.; Field, R. D.; Guerrero, D.; Joshi, B. M.; Kim, M.;
Konigsberg, J.; Korytov, A.; Lo, K. H.; Matchev, K.; Menendez, N.;
Mitselmakher, G.; Rosenzweig, D.; Shi, K.; Wang, J.; Wang, S.; Zuo,
X.; Joshi, Y. R.; Adams, T.; Askew, A.; Diaz, D.; Habibullah, R.;
Hagopian, S.; Hagopian, V.; Johnson, K. F.; Khurana, R.; Kolberg,
T.; Martinez, G.; Prosper, H.; Schiber, C.; Yohay, R.; Zhang, J.;
Baarmand, M. M.; Butalla, S.; Elkafrawy, T.; Hohlmann, M.; Noonan, D.;
Rahmani, M.; Saunders, M.; Yumiceva, F.; Adams, M. R.; Apanasevich,
L.; Becerril Gonzalez, H.; Cavanaugh, R.; Chen, X.; Dittmer, S.;
Evdokimov, O.; Gerber, C. E.; Hangal, D. A.; Hofman, D. J.; Mills, C.;
Oh, G.; Roy, T.; Tonjes, M. B.; Varelas, N.; Viinikainen, J.; Wang,
H.; Wang, X.; Wu, Z.; Alhusseini, M.; Bilki, B.; Dilsiz, K.; Durgut,
S.; Gandrajula, R. P.; Haytmyradov, M.; Khristenko, V.; Köseyan,
O. K.; Merlo, J. -P.; Mestvirishvili, A.; Moeller, A.; Nachtman,
J.; Ogul, H.; Onel, Y.; Ozok, F.; Penzo, A.; Snyder, C.; Tiras,
E.; Wetzel, J.; Yi, K.; Amram, O.; Blumenfeld, B.; Corcodilos, L.;
Eminizer, M.; Gritsan, A. V.; Kyriacou, S.; Maksimovic, P.; Mantilla,
C.; Roskes, J.; Swartz, M.; Vámi, T. Á.; Baldenegro Barrera, C.;
Baringer, P.; Bean, A.; Bylinkin, A.; Isidori, T.; Khalil, S.; King,
J.; Krintiras, G.; Kropivnitskaya, A.; Lindsey, C.; Mcbrayer, W.;
Minafra, N.; Murray, M.; Rogan, C.; Royon, C.; Sanders, S.; Schmitz,
E.; Tapia Takaki, J. D.; Wang, Q.; Williams, J.; Wilson, G.; Duric,
S.; Ivanov, A.; Kaadze, K.; Kim, D.; Maravin, Y.; Mendis, D. R.;
Mitchell, T.; Modak, A.; Mohammadi, A.; Rebassoo, F.; Wright, D.;
Adams, E.; Baden, A.; Baron, O.; Belloni, A.; Eno, S. C.; Feng, Y.;
Hadley, N. J.; Jabeen, S.; Jeng, G. Y.; Kellogg, R. G.; Koeth, T.;
Mignerey, A. C.; Nabili, S.; Seidel, M.; Skuja, A.; Tonwar, S. C.;
Wang, L.; Wong, K.; Abercrombie, D.; Allen, B.; Bi, R.; Brandt, S.;
Busza, W.; Cali, I. A.; Chen, Y.; D'Alfonso, M.; Gomez Ceballos, G.;
Goncharov, M.; Harris, P.; Hsu, D.; Hu, M.; Klute, M.; Kovalskyi,
D.; Krupa, J.; Lee, Y. -J.; Luckey, P. D.; Maier, B.; Marini, A. C.;
Mcginn, C.; Mironov, C.; Narayanan, S.; Niu, X.; Paus, C.; Rankin,
D.; Roland, C.; Roland, G.; Shi, Z.; Stephans, G. S. F.; Sumorok, K.;
Tatar, K.; Velicanu, D.; Wang, J.; Wang, T. W.; Wang, Z.; Wyslouch,
B.; Chatterjee, R. M.; Evans, A.; Guts, S.; Hansen, P.; Hiltbrand, J.;
Jain, Sh.; Krohn, M.; Kubota, Y.; Lesko, Z.; Mans, J.; Revering, M.;
Rusack, R.; Saradhy, R.; Schroeder, N.; Strobbe, N.; Wadud, M. A.;
Acosta, J. G.; Oliveros, S.; Bloom, K.; Chauhan, S.; Claes, D. R.;
Fangmeier, C.; Finco, L.; Golf, F.; González Fernández, J. R.;
Kravchenko, I.; Siado, J. E.; Snow, G. R.; Stieger, B.; Tabb, W.;
Agarwal, G.; Harrington, C.; Iashvili, I.; Kharchilava, A.; McLean,
C.; Nguyen, D.; Parker, A.; Pekkanen, J.; Rappoccio, S.; Roozbahani,
B.; Alverson, G.; Barberis, E.; Freer, C.; Haddad, Y.; Hortiangtham,
A.; Madigan, G.; Marzocchi, B.; Morse, D. M.; Nguyen, V.; Orimoto,
T.; Skinnari, L.; Tishelman-Charny, A.; Wamorkar, T.; Wang, B.;
Wisecarver, A.; Wood, D.; Bhattacharya, S.; Bueghly, J.; Chen, Z.;
Gilbert, A.; Gunter, T.; Hahn, K. A.; Odell, N.; Schmitt, M. H.;
Sung, K.; Velasco, M.; Bucci, R.; Dev, N.; Goldouzian, R.; Hildreth,
M.; Hurtado Anampa, K.; Jessop, C.; Karmgard, D. J.; Lannon, K.;
Li, W.; Loukas, N.; Marinelli, N.; Mcalister, I.; Meng, F.; Mohrman,
K.; Musienko, Y.; Ruchti, R.; Siddireddy, P.; Taroni, S.; Wayne, M.;
Wightman, A.; Wolf, M.; Zygala, L.; Alimena, J.; Bylsma, B.; Cardwell,
B.; Durkin, L. S.; Francis, B.; Hill, C.; Ji, W.; Lefeld, A.; Winer,
B. L.; Yates, B. R.; Dezoort, G.; Elmer, P.; Greenberg, B.; Haubrich,
N.; Higginbotham, S.; Kalogeropoulos, A.; Kopp, G.; Kwan, S.; Lange,
D.; Lucchini, M. T.; Luo, J.; Marlow, D.; Mei, K.; Ojalvo, I.; Olsen,
J.; Palmer, C.; Piroué, P.; Stickland, D.; Tully, C.; Malik, S.;
Norberg, S.; Barnes, V. E.; Chawla, R.; Das, S.; Gutay, L.; Jones,
M.; Jung, A. W.; Mahakud, B.; Negro, G.; Neumeister, N.; Peng, C. C.;
Piperov, S.; Qiu, H.; Schulte, J. F.; Trevisani, N.; Wang, F.; Xiao,
R.; Xie, W.; Cheng, T.; Dolen, J.; Parashar, N.; Baty, A.; Dildick, S.;
Ecklund, K. M.; Freed, S.; Geurts, F. J. M.; Kilpatrick, M.; Kumar,
A.; Li, W.; Padley, B. P.; Redjimi, R.; Roberts, J.; Rorie, J.; Shi,
W.; Stahl Leiton, A. G.; Tu, Z.; Zhang, A.; Bodek, A.; de Barbaro,
P.; Demina, R.; Dulemba, J. L.; Fallon, C.; Ferbel, T.; Galanti,
M.; Garcia-Bellido, A.; Hindrichs, O.; Khukhunaishvili, A.; Ranken,
E.; Taus, R.; Chiarito, B.; Chou, J. P.; Gandrakota, A.; Gershtein,
Y.; Halkiadakis, E.; Hart, A.; Heindl, M.; Hughes, E.; Kaplan, S.;
Karacheban, O.; Laflotte, I.; Lath, A.; Montalvo, R.; Nash, K.;
Osherson, M.; Salur, S.; Schnetzer, S.; Somalwar, S.; Stone, R.;
Thayil, S. A.; Thomas, S.; Acharya, H.; Delannoy, A. G.; Spanier,
S.; Bouhali, O.; Dalchenko, M.; Delgado, A.; Eusebi, R.; Gilmore,
J.; Huang, T.; Kamon, T.; Kim, H.; Luo, S.; Malhotra, S.; Marley,
D.; Mueller, R.; Overton, D.; Perniè, L.; Rathjens, D.; Safonov, A.;
Akchurin, N.; Damgov, J.; Hegde, V.; Kunori, S.; Lamichhane, K.; Lee,
S. W.; Mengke, T.; Muthumuni, S.; Peltola, T.; Undleeb, S.; Volobouev,
I.; Wang, Z.; Whitbeck, A.; Appelt, E.; Greene, S.; Gurrola, A.;
Janjam, R.; Johns, W.; Maguire, C.; Melo, A.; Ni, H.; Padeken, K.;
Romeo, F.; Sheldon, P.; Tuo, S.; Velkovska, J.; Verweij, M.; Ang, L.;
Arenton, M. W.; Cox, B.; Cummings, G.; Hakala, J.; Hirosky, R.; Joyce,
M.; Ledovskoy, A.; Neu, C.; Tannenwald, B.; Wang, Y.; Wolfe, E.; Xia,
F.; Karchin, P. E.; Poudyal, N.; Sturdy, J.; Thapa, P.; Black, K.;
Bose, T.; Buchanan, J.; Caillol, C.; Dasu, S.; De Bruyn, I.; Dodd, L.;
Galloni, C.; He, H.; Herndon, M.; Hervé, A.; Hussain, U.; Lanaro, A.;
Loeliger, A.; Loveless, R.; Madhusudanan Sreekala, J.; Mallampalli,
A.; Pinna, D.; Ruggles, T.; Savin, A.; Shang, V.; Sharma, V.; Smith,
W. H.; Teague, D.; Trembath-reichert, S.; Vetens, W.; CMS Collaboration
Bibcode: 2020PhRvL.125v2001S
Altcode:
Ultrarelativistic heavy ion collisions recreate in the laboratory
the thermodynamical conditions prevailing in the early universe up to
10-6 sec , thereby allowing the study of the quark-gluon
plasma (QGP), a state of quantum chromodynamics (QCD) matter with
deconfined partons. The top quark, the heaviest elementary particle
known, is accessible in nucleus-nucleus collisions at the CERN
LHC, and constitutes a novel probe of the QGP. Here, we report the
first evidence for the production of top quarks in nucleus-nucleus
collisions, using lead-lead collision data at a nucleon-nucleon
center-of-mass energy of 5.02 TeV recorded by the CMS experiment. Two
methods are used to measure the cross section for top quark pair
production (σt t ¯ ) via the selection of charged
leptons (electrons or muons) and bottom quarks. One method relies
on the leptonic information alone, and the second one exploits,
in addition, the presence of bottom quarks. The measured cross
sections, σt t ¯=2.5 4-0.74+0.84 and
2.03-0.64+0.71 μ b , respectively, are compatible
with expectations from scaled proton-proton data and QCD predictions.
Title: Coordination within the remote sensing payload on the Solar
Orbiter mission
Authors: Auchère, F.; Andretta, V.; Antonucci, E.; Bach, N.;
Battaglia, M.; Bemporad, A.; Berghmans, D.; Buchlin, E.; Caminade,
S.; Carlsson, M.; Carlyle, J.; Cerullo, J. J.; Chamberlin, P. C.;
Colaninno, R. C.; Davila, J. M.; De Groof, A.; Etesi, L.; Fahmy,
S.; Fineschi, S.; Fludra, A.; Gilbert, H. R.; Giunta, A.; Grundy,
T.; Haberreiter, M.; Harra, L. K.; Hassler, D. M.; Hirzberger, J.;
Howard, R. A.; Hurford, G.; Kleint, L.; Kolleck, M.; Krucker, S.;
Lagg, A.; Landini, F.; Long, D. M.; Lefort, J.; Lodiot, S.; Mampaey,
B.; Maloney, S.; Marliani, F.; Martinez-Pillet, V.; McMullin, D. R.;
Müller, D.; Nicolini, G.; Orozco Suarez, D.; Pacros, A.; Pancrazzi,
M.; Parenti, S.; Peter, H.; Philippon, A.; Plunkett, S.; Rich, N.;
Rochus, P.; Rouillard, A.; Romoli, M.; Sanchez, L.; Schühle, U.;
Sidher, S.; Solanki, S. K.; Spadaro, D.; St Cyr, O. C.; Straus, T.;
Tanco, I.; Teriaca, L.; Thompson, W. T.; del Toro Iniesta, J. C.;
Verbeeck, C.; Vourlidas, A.; Watson, C.; Wiegelmann, T.; Williams,
D.; Woch, J.; Zhukov, A. N.; Zouganelis, I.
Bibcode: 2020A&A...642A...6A
Altcode:
Context. To meet the scientific objectives of the mission, the Solar
Orbiter spacecraft carries a suite of in-situ (IS) and remote sensing
(RS) instruments designed for joint operations with inter-instrument
communication capabilities. Indeed, previous missions have shown that
the Sun (imaged by the RS instruments) and the heliosphere (mainly
sampled by the IS instruments) should be considered as an integrated
system rather than separate entities. Many of the advances expected
from Solar Orbiter rely on this synergistic approach between IS and
RS measurements.
Aims: Many aspects of hardware development,
integration, testing, and operations are common to two or more
RS instruments. In this paper, we describe the coordination effort
initiated from the early mission phases by the Remote Sensing Working
Group. We review the scientific goals and challenges, and give an
overview of the technical solutions devised to successfully operate
these instruments together.
Methods: A major constraint for the
RS instruments is the limited telemetry (TM) bandwidth of the Solar
Orbiter deep-space mission compared to missions in Earth orbit. Hence,
many of the strategies developed to maximise the scientific return from
these instruments revolve around the optimisation of TM usage, relying
for example on onboard autonomy for data processing, compression,
and selection for downlink. The planning process itself has been
optimised to alleviate the dynamic nature of the targets, and an
inter-instrument communication scheme has been implemented which can
be used to autonomously alter the observing modes. We also outline the
plans for in-flight cross-calibration, which will be essential to the
joint data reduction and analysis.
Results: The RS instrument
package on Solar Orbiter will carry out comprehensive measurements
from the solar interior to the inner heliosphere. Thanks to the close
coordination between the instrument teams and the European Space
Agency, several challenges specific to the RS suite were identified
and addressed in a timely manner.
Title: Models and data analysis tools for the Solar Orbiter mission
Authors: Rouillard, A. P.; Pinto, R. F.; Vourlidas, A.; De Groof, A.;
Thompson, W. T.; Bemporad, A.; Dolei, S.; Indurain, M.; Buchlin, E.;
Sasso, C.; Spadaro, D.; Dalmasse, K.; Hirzberger, J.; Zouganelis, I.;
Strugarek, A.; Brun, A. S.; Alexandre, M.; Berghmans, D.; Raouafi,
N. E.; Wiegelmann, T.; Pagano, P.; Arge, C. N.; Nieves-Chinchilla,
T.; Lavarra, M.; Poirier, N.; Amari, T.; Aran, A.; Andretta, V.;
Antonucci, E.; Anastasiadis, A.; Auchère, F.; Bellot Rubio, L.;
Nicula, B.; Bonnin, X.; Bouchemit, M.; Budnik, E.; Caminade, S.;
Cecconi, B.; Carlyle, J.; Cernuda, I.; Davila, J. M.; Etesi, L.;
Espinosa Lara, F.; Fedorov, A.; Fineschi, S.; Fludra, A.; Génot,
V.; Georgoulis, M. K.; Gilbert, H. R.; Giunta, A.; Gomez-Herrero, R.;
Guest, S.; Haberreiter, M.; Hassler, D.; Henney, C. J.; Howard, R. A.;
Horbury, T. S.; Janvier, M.; Jones, S. I.; Kozarev, K.; Kraaikamp,
E.; Kouloumvakos, A.; Krucker, S.; Lagg, A.; Linker, J.; Lavraud,
B.; Louarn, P.; Maksimovic, M.; Maloney, S.; Mann, G.; Masson, A.;
Müller, D.; Önel, H.; Osuna, P.; Orozco Suarez, D.; Owen, C. J.;
Papaioannou, A.; Pérez-Suárez, D.; Rodriguez-Pacheco, J.; Parenti,
S.; Pariat, E.; Peter, H.; Plunkett, S.; Pomoell, J.; Raines, J. M.;
Riethmüller, T. L.; Rich, N.; Rodriguez, L.; Romoli, M.; Sanchez,
L.; Solanki, S. K.; St Cyr, O. C.; Straus, T.; Susino, R.; Teriaca,
L.; del Toro Iniesta, J. C.; Ventura, R.; Verbeeck, C.; Vilmer, N.;
Warmuth, A.; Walsh, A. P.; Watson, C.; Williams, D.; Wu, Y.; Zhukov,
A. N.
Bibcode: 2020A&A...642A...2R
Altcode:
Context. The Solar Orbiter spacecraft will be equipped with a wide
range of remote-sensing (RS) and in situ (IS) instruments to record
novel and unprecedented measurements of the solar atmosphere and
the inner heliosphere. To take full advantage of these new datasets,
tools and techniques must be developed to ease multi-instrument and
multi-spacecraft studies. In particular the currently inaccessible
low solar corona below two solar radii can only be observed
remotely. Furthermore techniques must be used to retrieve coronal
plasma properties in time and in three dimensional (3D) space. Solar
Orbiter will run complex observation campaigns that provide interesting
opportunities to maximise the likelihood of linking IS data to their
source region near the Sun. Several RS instruments can be directed
to specific targets situated on the solar disk just days before
data acquisition. To compare IS and RS, data we must improve our
understanding of how heliospheric probes magnetically connect to the
solar disk.
Aims: The aim of the present paper is to briefly
review how the current modelling of the Sun and its atmosphere
can support Solar Orbiter science. We describe the results of a
community-led effort by European Space Agency's Modelling and Data
Analysis Working Group (MADAWG) to develop different models, tools,
and techniques deemed necessary to test different theories for the
physical processes that may occur in the solar plasma. The focus here
is on the large scales and little is described with regards to kinetic
processes. To exploit future IS and RS data fully, many techniques have
been adapted to model the evolving 3D solar magneto-plasma from the
solar interior to the solar wind. A particular focus in the paper is
placed on techniques that can estimate how Solar Orbiter will connect
magnetically through the complex coronal magnetic fields to various
photospheric and coronal features in support of spacecraft operations
and future scientific studies.
Methods: Recent missions such as
STEREO, provided great opportunities for RS, IS, and multi-spacecraft
studies. We summarise the achievements and highlight the challenges
faced during these investigations, many of which motivated the Solar
Orbiter mission. We present the new tools and techniques developed
by the MADAWG to support the science operations and the analysis of
the data from the many instruments on Solar Orbiter.
Results:
This article reviews current modelling and tool developments that ease
the comparison of model results with RS and IS data made available
by current and upcoming missions. It also describes the modelling
strategy to support the science operations and subsequent exploitation
of Solar Orbiter data in order to maximise the scientific output
of the mission.
Conclusions: The on-going community effort
presented in this paper has provided new models and tools necessary
to support mission operations as well as the science exploitation of
the Solar Orbiter data. The tools and techniques will no doubt evolve
significantly as we refine our procedure and methodology during the
first year of operations of this highly promising mission.
Title: Coordination of the in situ payload of Solar Orbiter
Authors: Walsh, A. P.; Horbury, T. S.; Maksimovic, M.; Owen, C. J.;
Rodríguez-Pacheco, J.; Wimmer-Schweingruber, R. F.; Zouganelis,
I.; Anekallu, C.; Bonnin, X.; Bruno, R.; Carrasco Blázquez, I.;
Cernuda, I.; Chust, T.; De Groof, A.; Espinosa Lara, F.; Fazakerley,
A. N.; Gilbert, H. R.; Gómez-Herrero, R.; Ho, G. C.; Krucker,
S.; Lepri, S. T.; Lewis, G. R.; Livi, S.; Louarn, P.; Müller, D.;
Nieves-Chinchilla, T.; O'Brien, H.; Osuna, P.; Plasson, P.; Raines,
J. M.; Rouillard, A. P.; St Cyr, O. C.; Sánchez, L.; Soucek, J.;
Varsani, A.; Verscharen, D.; Watson, C. J.; Watson, G.; Williams, D. R.
Bibcode: 2020A&A...642A...5W
Altcode:
Solar Orbiter's in situ coordination working group met frequently
during the development of the mission with the goal of ensuring
that its in situ payload has the necessary level of coordination to
maximise science return. Here we present the results of that work,
namely how the design of each of the in situ instruments (EPD, MAG,
RPW, SWA) was guided by the need for coordination, the importance of
time synchronisation, and how science operations will be conducted
in a coordinated way. We discuss the mechanisms by which instrument
sampling schemes are aligned such that complementary measurements
will be made simultaneously by different instruments, and how burst
modes are scheduled to allow a maximum overlap of burst intervals
between the four instruments (telemetry constraints mean different
instruments can spend different amounts of time in burst mode). We
also explain how onboard autonomy, inter-instrument communication,
and selective data downlink will be used to maximise the number of
transient events that will be studied using high-resolution modes of
all the instruments. Finally, we briefly address coordination between
Solar Orbiter's in situ payload and other missions.
Title: The Solar Orbiter Science Activity Plan. Translating solar
and heliospheric physics questions into action
Authors: Zouganelis, I.; De Groof, A.; Walsh, A. P.; Williams, D. R.;
Müller, D.; St Cyr, O. C.; Auchère, F.; Berghmans, D.; Fludra,
A.; Horbury, T. S.; Howard, R. A.; Krucker, S.; Maksimovic, M.;
Owen, C. J.; Rodríguez-Pacheco, J.; Romoli, M.; Solanki, S. K.;
Watson, C.; Sanchez, L.; Lefort, J.; Osuna, P.; Gilbert, H. R.;
Nieves-Chinchilla, T.; Abbo, L.; Alexandrova, O.; Anastasiadis, A.;
Andretta, V.; Antonucci, E.; Appourchaux, T.; Aran, A.; Arge, C. N.;
Aulanier, G.; Baker, D.; Bale, S. D.; Battaglia, M.; Bellot Rubio,
L.; Bemporad, A.; Berthomier, M.; Bocchialini, K.; Bonnin, X.; Brun,
A. S.; Bruno, R.; Buchlin, E.; Büchner, J.; Bucik, R.; Carcaboso,
F.; Carr, R.; Carrasco-Blázquez, I.; Cecconi, B.; Cernuda Cangas, I.;
Chen, C. H. K.; Chitta, L. P.; Chust, T.; Dalmasse, K.; D'Amicis, R.;
Da Deppo, V.; De Marco, R.; Dolei, S.; Dolla, L.; Dudok de Wit, T.;
van Driel-Gesztelyi, L.; Eastwood, J. P.; Espinosa Lara, F.; Etesi,
L.; Fedorov, A.; Félix-Redondo, F.; Fineschi, S.; Fleck, B.; Fontaine,
D.; Fox, N. J.; Gandorfer, A.; Génot, V.; Georgoulis, M. K.; Gissot,
S.; Giunta, A.; Gizon, L.; Gómez-Herrero, R.; Gontikakis, C.; Graham,
G.; Green, L.; Grundy, T.; Haberreiter, M.; Harra, L. K.; Hassler,
D. M.; Hirzberger, J.; Ho, G. C.; Hurford, G.; Innes, D.; Issautier,
K.; James, A. W.; Janitzek, N.; Janvier, M.; Jeffrey, N.; Jenkins,
J.; Khotyaintsev, Y.; Klein, K. -L.; Kontar, E. P.; Kontogiannis,
I.; Krafft, C.; Krasnoselskikh, V.; Kretzschmar, M.; Labrosse, N.;
Lagg, A.; Landini, F.; Lavraud, B.; Leon, I.; Lepri, S. T.; Lewis,
G. R.; Liewer, P.; Linker, J.; Livi, S.; Long, D. M.; Louarn, P.;
Malandraki, O.; Maloney, S.; Martinez-Pillet, V.; Martinovic, M.;
Masson, A.; Matthews, S.; Matteini, L.; Meyer-Vernet, N.; Moraitis,
K.; Morton, R. J.; Musset, S.; Nicolaou, G.; Nindos, A.; O'Brien,
H.; Orozco Suarez, D.; Owens, M.; Pancrazzi, M.; Papaioannou, A.;
Parenti, S.; Pariat, E.; Patsourakos, S.; Perrone, D.; Peter, H.;
Pinto, R. F.; Plainaki, C.; Plettemeier, D.; Plunkett, S. P.; Raines,
J. M.; Raouafi, N.; Reid, H.; Retino, A.; Rezeau, L.; Rochus, P.;
Rodriguez, L.; Rodriguez-Garcia, L.; Roth, M.; Rouillard, A. P.;
Sahraoui, F.; Sasso, C.; Schou, J.; Schühle, U.; Sorriso-Valvo, L.;
Soucek, J.; Spadaro, D.; Stangalini, M.; Stansby, D.; Steller, M.;
Strugarek, A.; Štverák, Š.; Susino, R.; Telloni, D.; Terasa, C.;
Teriaca, L.; Toledo-Redondo, S.; del Toro Iniesta, J. C.; Tsiropoula,
G.; Tsounis, A.; Tziotziou, K.; Valentini, F.; Vaivads, A.; Vecchio,
A.; Velli, M.; Verbeeck, C.; Verdini, A.; Verscharen, D.; Vilmer, N.;
Vourlidas, A.; Wicks, R.; Wimmer-Schweingruber, R. F.; Wiegelmann,
T.; Young, P. R.; Zhukov, A. N.
Bibcode: 2020A&A...642A...3Z
Altcode: 2020arXiv200910772Z
Solar Orbiter is the first space mission observing the solar plasma
both in situ and remotely, from a close distance, in and out of the
ecliptic. The ultimate goal is to understand how the Sun produces
and controls the heliosphere, filling the Solar System and driving
the planetary environments. With six remote-sensing and four in-situ
instrument suites, the coordination and planning of the operations are
essential to address the following four top-level science questions:
(1) What drives the solar wind and where does the coronal magnetic field
originate?; (2) How do solar transients drive heliospheric variability?;
(3) How do solar eruptions produce energetic particle radiation that
fills the heliosphere?; (4) How does the solar dynamo work and drive
connections between the Sun and the heliosphere? Maximising the
mission's science return requires considering the characteristics
of each orbit, including the relative position of the spacecraft
to Earth (affecting downlink rates), trajectory events (such
as gravitational assist manoeuvres), and the phase of the solar
activity cycle. Furthermore, since each orbit's science telemetry
will be downloaded over the course of the following orbit, science
operations must be planned at mission level, rather than at the level
of individual orbits. It is important to explore the way in which those
science questions are translated into an actual plan of observations
that fits into the mission, thus ensuring that no opportunities are
missed. First, the overarching goals are broken down into specific,
answerable questions along with the required observations and the
so-called Science Activity Plan (SAP) is developed to achieve this. The
SAP groups objectives that require similar observations into Solar
Orbiter Observing Plans, resulting in a strategic, top-level view of
the optimal opportunities for science observations during the mission
lifetime. This allows for all four mission goals to be addressed. In
this paper, we introduce Solar Orbiter's SAP through a series of
examples and the strategy being followed.
Title: The Polarimetric and Helioseismic Imager on Solar Orbiter
Authors: Solanki, S. K.; del Toro Iniesta, J. C.; Woch, J.; Gandorfer,
A.; Hirzberger, J.; Alvarez-Herrero, A.; Appourchaux, T.; Martínez
Pillet, V.; Pérez-Grande, I.; Sanchis Kilders, E.; Schmidt, W.;
Gómez Cama, J. M.; Michalik, H.; Deutsch, W.; Fernandez-Rico, G.;
Grauf, B.; Gizon, L.; Heerlein, K.; Kolleck, M.; Lagg, A.; Meller, R.;
Müller, R.; Schühle, U.; Staub, J.; Albert, K.; Alvarez Copano, M.;
Beckmann, U.; Bischoff, J.; Busse, D.; Enge, R.; Frahm, S.; Germerott,
D.; Guerrero, L.; Löptien, B.; Meierdierks, T.; Oberdorfer, D.;
Papagiannaki, I.; Ramanath, S.; Schou, J.; Werner, S.; Yang, D.;
Zerr, A.; Bergmann, M.; Bochmann, J.; Heinrichs, J.; Meyer, S.;
Monecke, M.; Müller, M. -F.; Sperling, M.; Álvarez García, D.;
Aparicio, B.; Balaguer Jiménez, M.; Bellot Rubio, L. R.; Cobos
Carracosa, J. P.; Girela, F.; Hernández Expósito, D.; Herranz, M.;
Labrousse, P.; López Jiménez, A.; Orozco Suárez, D.; Ramos, J. L.;
Barandiarán, J.; Bastide, L.; Campuzano, C.; Cebollero, M.; Dávila,
B.; Fernández-Medina, A.; García Parejo, P.; Garranzo-García, D.;
Laguna, H.; Martín, J. A.; Navarro, R.; Núñez Peral, A.; Royo, M.;
Sánchez, A.; Silva-López, M.; Vera, I.; Villanueva, J.; Fourmond,
J. -J.; de Galarreta, C. Ruiz; Bouzit, M.; Hervier, V.; Le Clec'h,
J. C.; Szwec, N.; Chaigneau, M.; Buttice, V.; Dominguez-Tagle, C.;
Philippon, A.; Boumier, P.; Le Cocguen, R.; Baranjuk, G.; Bell,
A.; Berkefeld, Th.; Baumgartner, J.; Heidecke, F.; Maue, T.; Nakai,
E.; Scheiffelen, T.; Sigwarth, M.; Soltau, D.; Volkmer, R.; Blanco
Rodríguez, J.; Domingo, V.; Ferreres Sabater, A.; Gasent Blesa,
J. L.; Rodríguez Martínez, P.; Osorno Caudel, D.; Bosch, J.; Casas,
A.; Carmona, M.; Herms, A.; Roma, D.; Alonso, G.; Gómez-Sanjuan, A.;
Piqueras, J.; Torralbo, I.; Fiethe, B.; Guan, Y.; Lange, T.; Michel,
H.; Bonet, J. A.; Fahmy, S.; Müller, D.; Zouganelis, I.
Bibcode: 2020A&A...642A..11S
Altcode: 2019arXiv190311061S
Aims: This paper describes the Polarimetric and Helioseismic
Imager on the Solar Orbiter mission (SO/PHI), the first magnetograph and
helioseismology instrument to observe the Sun from outside the Sun-Earth
line. It is the key instrument meant to address the top-level science
question: How does the solar dynamo work and drive connections between
the Sun and the heliosphere? SO/PHI will also play an important role
in answering the other top-level science questions of Solar Orbiter,
while hosting the potential of a rich return in further science.
Methods: SO/PHI measures the Zeeman effect and the Doppler shift
in the Fe I 617.3 nm spectral line. To this end, the instrument
carries out narrow-band imaging spectro-polarimetry using a tunable
LiNbO3 Fabry-Perot etalon, while the polarisation modulation
is done with liquid crystal variable retarders. The line and the nearby
continuum are sampled at six wavelength points and the data are recorded
by a 2k × 2k CMOS detector. To save valuable telemetry, the raw data
are reduced on board, including being inverted under the assumption of
a Milne-Eddington atmosphere, although simpler reduction methods are
also available on board. SO/PHI is composed of two telescopes; one,
the Full Disc Telescope, covers the full solar disc at all phases of
the orbit, while the other, the High Resolution Telescope, can resolve
structures as small as 200 km on the Sun at closest perihelion. The high
heat load generated through proximity to the Sun is greatly reduced by
the multilayer-coated entrance windows to the two telescopes that allow
less than 4% of the total sunlight to enter the instrument, most of
it in a narrow wavelength band around the chosen spectral line.
Results: SO/PHI was designed and built by a consortium having partners
in Germany, Spain, and France. The flight model was delivered to
Airbus Defence and Space, Stevenage, and successfully integrated into
the Solar Orbiter spacecraft. A number of innovations were introduced
compared with earlier space-based spectropolarimeters, thus allowing
SO/PHI to fit into the tight mass, volume, power and telemetry budgets
provided by the Solar Orbiter spacecraft and to meet the (e.g. thermal)
challenges posed by the mission's highly elliptical orbit.
Title: The Solar Orbiter magnetometer
Authors: Horbury, T. S.; O'Brien, H.; Carrasco Blazquez, I.; Bendyk,
M.; Brown, P.; Hudson, R.; Evans, V.; Oddy, T. M.; Carr, C. M.; Beek,
T. J.; Cupido, E.; Bhattacharya, S.; Dominguez, J. -A.; Matthews, L.;
Myklebust, V. R.; Whiteside, B.; Bale, S. D.; Baumjohann, W.; Burgess,
D.; Carbone, V.; Cargill, P.; Eastwood, J.; Erdös, G.; Fletcher,
L.; Forsyth, R.; Giacalone, J.; Glassmeier, K. -H.; Goldstein, M. L.;
Hoeksema, T.; Lockwood, M.; Magnes, W.; Maksimovic, M.; Marsch, E.;
Matthaeus, W. H.; Murphy, N.; Nakariakov, V. M.; Owen, C. J.; Owens,
M.; Rodriguez-Pacheco, J.; Richter, I.; Riley, P.; Russell, C. T.;
Schwartz, S.; Vainio, R.; Velli, M.; Vennerstrom, S.; Walsh, R.;
Wimmer-Schweingruber, R. F.; Zank, G.; Müller, D.; Zouganelis, I.;
Walsh, A. P.
Bibcode: 2020A&A...642A...9H
Altcode:
The magnetometer instrument on the Solar Orbiter mission is designed
to measure the magnetic field local to the spacecraft continuously
for the entire mission duration. The need to characterise not only
the background magnetic field but also its variations on scales from
far above to well below the proton gyroscale result in challenging
requirements on stability, precision, and noise, as well as magnetic
and operational limitations on both the spacecraft and other
instruments. The challenging vibration and thermal environment has
led to significant development of the mechanical sensor design. The
overall instrument design, performance, data products, and operational
strategy are described.
Title: The Solar Orbiter SPICE instrument. An extreme UV imaging
spectrometer
Authors: SPICE Consortium; Anderson, M.; Appourchaux, T.; Auchère, F.;
Aznar Cuadrado, R.; Barbay, J.; Baudin, F.; Beardsley, S.; Bocchialini,
K.; Borgo, B.; Bruzzi, D.; Buchlin, E.; Burton, G.; Büchel, V.;
Caldwell, M.; Caminade, S.; Carlsson, M.; Curdt, W.; Davenne, J.;
Davila, J.; Deforest, C. E.; Del Zanna, G.; Drummond, D.; Dubau,
J.; Dumesnil, C.; Dunn, G.; Eccleston, P.; Fludra, A.; Fredvik, T.;
Gabriel, A.; Giunta, A.; Gottwald, A.; Griffin, D.; Grundy, T.; Guest,
S.; Gyo, M.; Haberreiter, M.; Hansteen, V.; Harrison, R.; Hassler,
D. M.; Haugan, S. V. H.; Howe, C.; Janvier, M.; Klein, R.; Koller,
S.; Kucera, T. A.; Kouliche, D.; Marsch, E.; Marshall, A.; Marshall,
G.; Matthews, S. A.; McQuirk, C.; Meining, S.; Mercier, C.; Morris,
N.; Morse, T.; Munro, G.; Parenti, S.; Pastor-Santos, C.; Peter, H.;
Pfiffner, D.; Phelan, P.; Philippon, A.; Richards, A.; Rogers, K.;
Sawyer, C.; Schlatter, P.; Schmutz, W.; Schühle, U.; Shaughnessy,
B.; Sidher, S.; Solanki, S. K.; Speight, R.; Spescha, M.; Szwec, N.;
Tamiatto, C.; Teriaca, L.; Thompson, W.; Tosh, I.; Tustain, S.; Vial,
J. -C.; Walls, B.; Waltham, N.; Wimmer-Schweingruber, R.; Woodward,
S.; Young, P.; de Groof, A.; Pacros, A.; Williams, D.; Müller, D.
Bibcode: 2020A&A...642A..14S
Altcode: 2019arXiv190901183A; 2019arXiv190901183S
Aims: The Spectral Imaging of the Coronal Environment (SPICE)
instrument is a high-resolution imaging spectrometer operating at
extreme ultraviolet wavelengths. In this paper, we present the concept,
design, and pre-launch performance of this facility instrument on the
ESA/NASA Solar Orbiter mission.
Methods: The goal of this paper
is to give prospective users a better understanding of the possible
types of observations, the data acquisition, and the sources that
contribute to the instrument's signal.
Results: The paper
discusses the science objectives, with a focus on the SPICE-specific
aspects, before presenting the instrument's design, including optical,
mechanical, thermal, and electronics aspects. This is followed by a
characterisation and calibration of the instrument's performance. The
paper concludes with descriptions of the operations concept and data
processing.
Conclusions: The performance measurements of the
various instrument parameters meet the requirements derived from the
mission's science objectives. The SPICE instrument is ready to perform
measurements that will provide vital contributions to the scientific
success of the Solar Orbiter mission.
Title: The divergence and curl in arbitrary basis
Authors: de Medeiros, Waleska P. F.; de Lima, Rodrigo R.; de Andrade,
Vanessa C.; Müller, Daniel
Bibcode: 2020arXiv201004267D
Altcode:
In this work, the divergence and curl operators are obtained using
the coordinate free non rigid basis formulation of differential
geometry. Although the authors have attempted to keep the presentation
self-contained as much as possible, some previous exposure to the
language of differential geometry may be helpful. In this sense the
work is aimed to late undergraduate or beginners graduate students
interested in mathematical physics. To illustrate the development, we
graphically present the eleven coordinate systems in which the Laplace
operator is separable. We detail the development of the basis and the
connection for the cylindrical and paraboloidal coordinate systems. We
also present in [1] codes both in Maxima and Maple for the spherical
orthonormal basis, which serves as a working model for calculations
in other situations of interest. Also in [1] the codes to obtain the
coordinate surfaces are given.
Title: Understanding the origins of the heliosphere: integrating
observations and measurements from Parker Solar Probe, Solar Orbiter,
and other space- and ground-based observatories
Authors: Velli, M.; Harra, L. K.; Vourlidas, A.; Schwadron,
N.; Panasenco, O.; Liewer, P. C.; Müller, D.; Zouganelis, I.;
St Cyr, O. C.; Gilbert, H.; Nieves-Chinchilla, T.; Auchère, F.;
Berghmans, D.; Fludra, A.; Horbury, T. S.; Howard, R. A.; Krucker,
S.; Maksimovic, M.; Owen, C. J.; Rodríguez-Pacheco, J.; Romoli,
M.; Solanki, S. K.; Wimmer-Schweingruber, R. F.; Bale, S.; Kasper,
J.; McComas, D. J.; Raouafi, N.; Martinez-Pillet, V.; Walsh, A. P.;
De Groof, A.; Williams, D.
Bibcode: 2020A&A...642A...4V
Altcode:
Context. The launch of Parker Solar Probe (PSP) in 2018, followed
by Solar Orbiter (SO) in February 2020, has opened a new window in
the exploration of solar magnetic activity and the origin of the
heliosphere. These missions, together with other space observatories
dedicated to solar observations, such as the Solar Dynamics Observatory,
Hinode, IRIS, STEREO, and SOHO, with complementary in situ observations
from WIND and ACE, and ground based multi-wavelength observations
including the DKIST observatory that has just seen first light,
promise to revolutionize our understanding of the solar atmosphere
and of solar activity, from the generation and emergence of the Sun's
magnetic field to the creation of the solar wind and the acceleration of
solar energetic particles.
Aims: Here we describe the scientific
objectives of the PSP and SO missions, and highlight the potential for
discovery arising from synergistic observations. Here we put particular
emphasis on how the combined remote sensing and in situ observations of
SO, that bracket the outer coronal and inner heliospheric observations
by PSP, may provide a reconstruction of the solar wind and magnetic
field expansion from the Sun out to beyond the orbit of Mercury in the
first phases of the mission. In the later, out-of-ecliptic portions of
the SO mission, the solar surface magnetic field measurements from SO
and the multi-point white-light observations from both PSP and SO will
shed light on the dynamic, intermittent solar wind escaping from helmet
streamers, pseudo-streamers, and the confined coronal plasma, and on
solar energetic particle transport.
Methods: Joint measurements
during PSP-SO alignments, and magnetic connections along the same
flux tube complemented by alignments with Earth, dual PSP-Earth,
and SO-Earth, as well as with STEREO-A, SOHO, and BepiColumbo will
allow a better understanding of the in situ evolution of solar-wind
plasma flows and the full three-dimensional distribution of the
solar wind from a purely observational point of view. Spectroscopic
observations of the corona, and optical and radio observations,
combined with direct in situ observations of the accelerating solar
wind will provide a new foundation for understanding the fundamental
physical processes leading to the energy transformations from solar
photospheric flows and magnetic fields into the hot coronal plasma
and magnetic fields and finally into the bulk kinetic energy of the
solar wind and solar energetic particles.
Results: We discuss
the initial PSP observations, which already provide a compelling
rationale for new measurement campaigns by SO, along with ground-
and space-based assets within the synergistic context described above.
Title: The Solar Orbiter mission. Science overview
Authors: Müller, D.; St. Cyr, O. C.; Zouganelis, I.; Gilbert, H. R.;
Marsden, R.; Nieves-Chinchilla, T.; Antonucci, E.; Auchère, F.;
Berghmans, D.; Horbury, T. S.; Howard, R. A.; Krucker, S.; Maksimovic,
M.; Owen, C. J.; Rochus, P.; Rodriguez-Pacheco, J.; Romoli, M.;
Solanki, S. K.; Bruno, R.; Carlsson, M.; Fludra, A.; Harra, L.;
Hassler, D. M.; Livi, S.; Louarn, P.; Peter, H.; Schühle, U.;
Teriaca, L.; del Toro Iniesta, J. C.; Wimmer-Schweingruber, R. F.;
Marsch, E.; Velli, M.; De Groof, A.; Walsh, A.; Williams, D.
Bibcode: 2020A&A...642A...1M
Altcode: 2020arXiv200900861M
Aims: Solar Orbiter, the first mission of ESA's Cosmic Vision
2015-2025 programme and a mission of international collaboration between
ESA and NASA, will explore the Sun and heliosphere from close up and
out of the ecliptic plane. It was launched on 10 February 2020 04:03
UTC from Cape Canaveral and aims to address key questions of solar and
heliospheric physics pertaining to how the Sun creates and controls
the Heliosphere, and why solar activity changes with time. To answer
these, the mission carries six remote-sensing instruments to observe
the Sun and the solar corona, and four in-situ instruments to measure
the solar wind, energetic particles, and electromagnetic fields. In
this paper, we describe the science objectives of the mission, and how
these will be addressed by the joint observations of the instruments
onboard.
Methods: The paper first summarises the mission-level
science objectives, followed by an overview of the spacecraft and
payload. We report the observables and performance figures of each
instrument, as well as the trajectory design. This is followed by a
summary of the science operations concept. The paper concludes with a
more detailed description of the science objectives.
Results:
Solar Orbiter will combine in-situ measurements in the heliosphere
with high-resolution remote-sensing observations of the Sun to address
fundamental questions of solar and heliospheric physics. The performance
of the Solar Orbiter payload meets the requirements derived from the
mission's science objectives. Its science return will be augmented
further by coordinated observations with other space missions and
ground-based observatories. ARRAY(0x207ce98)
Title: Generality of Starobinsky and Higgs inflation in the Jordan
frame
Authors: Mishra, Swagat S.; Müller, Daniel; Toporensky, Aleksey V.
Bibcode: 2020PhRvD.102f3523M
Altcode: 2019arXiv191201654M
We revisit the problem of generality of Starobinsky and Higgs
inflation. The known results obtained in the Einstein frame are
generalized for the case of an arbitrary initial energy of the
scalar field. These results are compared with the results obtained
directly in the Jordan frame, which, to our knowledge, has not been
thoroughly explored in the literature previously. We demonstrate that
the qualitative picture of initial conditions zone in the (ϕ ,ϕ ˙)
plane, which leads to sufficient amount of inflation, is quite similar
for both the frames in the case of Higgs inflation. For Starobinsky
inflation, the conformal transformation between the frames relates
the geometrical variables in the Jordan frame with the properties
of an effective scalar field in the Einstein frame. We show that
the transformation (H ,R )→(ϕ ,ϕ ˙) is not regular everywhere,
leading to some peculiarities in the zone of good initial conditions
in the (H ,R ) plane.
Title: BepiColombo and Solar Orbiter coordinated observations:
scientific cases and measurements opportunities
Authors: Hadid, Lina; Dosa, Melinda; Akos, Madar; Alberti, Tommaso;
Benkhoff, Johannes; Bebesi, Zsofia; Griton, Lea; Ho, George C.; Iwai,
Kazumasa; Janvier, Miho; Milillo, Anna; Miyoshi, Yoshizumi; Mueller,
Daniel; Murukami, Go; Raines, Jim M.; Shiota, Daikou; Walsh, Andrew;
Zender, Joe; Zouganelis, Yannis
Bibcode: 2020EGUGA..2217957H
Altcode:
BepiColombo and Solar Orbiter are two spacecraft that will be
both travelling in the inner heliosphere for 5 years, between the
launch of Solar Orbiter (planned in February 2020) and the end of
the cruise phase of BepiColombo (2018 - 2025). Both BepiColombo
(ESA/JAXA) and Solar Orbiter (ESA/NASA) are carrying exceptional and
complementary plasma instrumental payloads and magnetometers. Besides,
the remote-sensing instruments on board of Solar Orbiter will provide
invaluable information on the state of the Sun, and therefore some
contextual information for BepiColombo observations. During the
five years to come, BepiColombo will evolve between the Earth and
the orbit of Mercury, while Solar Orbiter's highly elliptical orbit
will cover distances from 1.02 AU to 0.28 AU. We present here the
scientific cases, modelling tools, measurement opportunities and
related instruments operations that have been identified in the frame
of potential coordinated observations campaign between the spacecraft.
Title: Solar Orbiter: Europe's mission to the Sun
Authors: Zouganelis, Yannis; Mueller, Daniel; St Cyr, Chris; Gilbert,
Holly; Nieves-Chinchilla, Teresa
Bibcode: 2020EGUGA..2222164Z
Altcode:
ESA's Solar Orbiter mission is scheduled for launch in February
2020, and will focus on exploring the linkage between the Sun and
the heliosphere. It is a collaborative mission with NASA that will
collect unique data that will allow us to study, e.g., the coupling
between macroscopic physical processes to those on kinetic scales, the
generation of solar energetic particles and their propagation into the
heliosphere, and the origin and acceleration of solar wind plasma. By
approaching as close as 0.28 AU, Solar Orbiter will view the Sun with
high spatial resolution and combine this with in-situ measurements
of the surrounding heliosphere. Over the course of the mission, the
highly elliptical orbit will get progressively more inclined to the
ecliptic plane. Thanks to this new perspective, Solar Orbiter will
deliver images and comprehensive data of the unexplored Sun's polar
regions and the side of the Sun not visible from Earth. This talk will
provide a mission overview, highlight synergies with NASA's Parker
Solar Probe and summarise current status.
Title: Europe's next mission to the Sun
Authors: Müller, D.; Zouganelis, I.; St. Cyr, O. C.; Gilbert, H. R.;
Nieves-Chinchilla, T.
Bibcode: 2020NatAs...4..205M
Altcode: 2020NatAs.tmp...19M
As the Solar Orbiter spacecraft is scheduled for launch this month,
European Space Agency (ESA) and NASA Project Scientists provide an
overview of this major ESA-NASA mission to the Sun.
Title: Search for the doubly charmed baryon Ξ_{cc}^+
Authors: Aaij, R.; Abellán Beteta, C.; Ackernley, T.; Adeva, B.;
Adinolfi, M.; Afsharnia, H.; Aidala, C. A.; Aiola, S.; Ajaltouni,
Z.; Akar, S.; Albicocco, P.; Albrecht, J.; Alessio, F.; Alexander,
M.; Alfonso Albero, A.; Alkhazov, G.; Alvarez Cartelle, P.; Alves,
A. A.; Amato, S.; Amhis, Y.; An, L.; Anderlini, L.; Andreassi, G.;
Andreotti, M.; Archilli, F.; Arnau Romeu, J.; Artamonov, A.; Artuso,
M.; Arzymatov, K.; Aslanides, E.; Atzeni, M.; Audurier, B.; Bachmann,
S.; Back, J. J.; Baker, S.; Balagura, V.; Baldini, W.; Baranov, A.;
Barlow, R. J.; Barsuk, S.; Barter, W.; Bartolini, M.; Baryshnikov,
F.; Bassi, G.; Batozskaya, V.; Batsukh, B.; Battig, A.; Battista,
V.; Bay, A.; Becker, M.; Bedeschi, F.; Bediaga, I.; Beiter, A.;
Bel, L. J.; Belavin, V.; Belin, S.; Beliy, N.; Bellee, V.; Belous,
K.; Belyaev, I.; Bencivenni, G.; Ben-Haim, E.; Benson, S.; Beranek,
S.; Berezhnoy, A.; Bernet, R.; Berninghoff, D.; Bernstein, H. C.;
Bertholet, E.; Bertolin, A.; Betancourt, C.; Betti, F.; Bettler,
M. O.; Bezshyiko, Ia.; Bhasin, S.; Bhom, J.; Bieker, M. S.; Bifani,
S.; Billoir, P.; Birnkraut, A.; Bizzeti, A.; Bjørn, M.; Blago,
M. P.; Blake, T.; Blanc, F.; Blusk, S.; Bobulska, D.; Bocci, V.;
Boente Garcia, O.; Boettcher, T.; Boldyrev, A.; Bondar, A.; Bondar,
N.; Borghi, S.; Borisyak, M.; Borsato, M.; Borsuk, J. T.; Bowcock,
T. J. V.; Bozzi, C.; Braun, S.; Brea Rodriguez, A.; Brodski, M.;
Brodzicka, J.; Brossa Gonzalo, A.; Brundu, D.; Buchanan, E.; Buonaura,
A.; Burr, C.; Bursche, A.; Butter, J. S.; Buytaert, J.; Byczynski, W.;
Cadeddu, S.; Cai, H.; Calabrese, R.; Cali, S.; Calladine, R.; Calvi,
M.; Calvo Gomez, M.; Camboni, A.; Campana, P.; Campora Perez, D. H.;
Capriotti, L.; Carbone, A.; Carboni, G.; Cardinale, R.; Cardini,
A.; Carniti, P.; Carvalho Akiba, K.; Casais Vidal, A.; Casse, G.;
Cattaneo, M.; Cavallero, G.; Cenci, R.; Cerasoli, J.; Chapman, M. G.;
Charles, M.; Charpentier, Ph.; Chatzikonstantinidis, G.; Chefdeville,
M.; Chekalina, V.; Chen, C.; Chen, S.; Chernov, A.; Chitic, S. -G.;
Chobanova, V.; Chrzaszcz, M.; Chubykin, A.; Ciambrone, P.; Cicala,
M. F.; Cid Vidal, X.; Ciezarek, G.; Cindolo, F.; Clarke, P. E. L.;
Clemencic, M.; Cliff, H. V.; Closier, J.; Cobbledick, J. L.; Coco, V.;
Coelho, J. A. B.; Cogan, J.; Cogneras, E.; Cojocariu, L.; Collins, P.;
Colombo, T.; Comerma-Montells, A.; Contu, A.; Cooke, N.; Coombs, G.;
Coquereau, S.; Corti, G.; Costa Sobral, C. M.; Couturier, B.; Craik,
D. C.; Crkovska, J.; Crocombe, A.; Cruz Torres, M.; Currie, R.; Da
Silva, C. L.; Dall'Occo, E.; Dalseno, J.; D'Ambrosio, C.; Danilina,
A.; d'Argent, P.; Davis, A.; De Aguiar Francisco, O.; De Bruyn, K.;
De Capua, S.; De Cian, M.; De Miranda, J. M.; De Paula, L.; De Serio,
M.; De Simone, P.; de Vries, J. A.; Dean, C. T.; Dean, W.; Decamp, D.;
Del Buono, L.; Delaney, B.; Dembinski, H. -P.; Demmer, M.; Dendek,
A.; Denysenko, V.; Derkach, D.; Deschamps, O.; Desse, F.; Dettori,
F.; Dey, B.; Di Canto, A.; Di Nezza, P.; Didenko, S.; Dijkstra, H.;
Dordei, F.; Dorigo, M.; dos Reis, A. C.; Douglas, L.; Dovbnya, A.;
Dreimanis, K.; Dudek, M. W.; Dufour, L.; Dujany, G.; Durante, P.;
Durham, J. M.; Dutta, D.; Dzhelyadin, R.; Dziewiecki, M.; Dziurda,
A.; Dzyuba, A.; Easo, S.; Egede, U.; Egorychev, V.; Eidelman, S.;
Eisenhardt, S.; Ekelhof, R.; Ek-In, S.; Eklund, L.; Ely, S.; Ene, A.;
Escher, S.; Esen, S.; Evans, T.; Falabella, A.; Fan, J.; Farley, N.;
Farry, S.; Fazzini, D.; Féo, M.; Fernandez Declara, P.; Fernandez
Prieto, A.; Ferrari, F.; Ferreira Lopes, L.; Ferreira Rodrigues,
F.; Ferreres Sole, S.; Ferrillo, M.; Ferro-Luzzi, M.; Filippov, S.;
Fini, R. A.; Fiorini, M.; Firlej, M.; Fischer, K. M.; Fitzpatrick,
C.; Fiutowski, T.; Fleuret, F.; Fontana, M.; Fontanelli, F.; Forty,
R.; Franco Lima, V.; Franco Sevilla, M.; Frank, M.; Frei, C.; Friday,
D. A.; Fu, J.; Fuehring, M.; Funk, W.; Gabriel, E.; Gallas Torreira,
A.; Galli, D.; Gallorini, S.; Gambetta, S.; Gan, Y.; Gandelman, M.;
Gandini, P.; Gao, Y.; Garcia Martin, L. M.; García Pardiñas, J.;
Garcia Plana, B.; Garcia Rosales, F. A.; Garra Tico, J.; Garrido,
L.; Gascon, D.; Gaspar, C.; Gerick, D.; Gersabeck, E.; Gersabeck,
M.; Gershon, T.; Gerstel, D.; Ghez, Ph.; Gibson, V.; Gioventù, A.;
Girard, O. G.; Gironella Gironell, P.; Giubega, L.; Giugliano, C.;
Gizdov, K.; Gligorov, V. V.; Göbel, C.; Golubkov, D.; Golutvin, A.;
Gomes, A.; Gorbounov, P.; Gorelov, I. V.; Gotti, C.; Govorkova, E.;
Grabowski, J. P.; Graciani Diaz, R.; Grammatico, T.; Granado Cardoso,
L. A.; Graugés, E.; Graverini, E.; Graziani, G.; Grecu, A.; Greim, R.;
Griffith, P.; Grillo, L.; Gruber, L.; Gruberg Cazon, B. R.; Gu, C.;
Gushchin, E.; Guth, A.; Guz, Yu.; Gys, T.; Hadavizadeh, T.; Haefeli,
G.; Haen, C.; Haines, S. C.; Hamilton, P. M.; Han, Q.; Han, X.;
Hancock, T. H.; Hansmann-Menzemer, S.; Harnew, N.; Harrison, T.; Hart,
R.; Hasse, C.; Hatch, M.; He, J.; Hecker, M.; Heijhoff, K.; Heinicke,
K.; Heister, A.; Hennequin, A. M.; Hennessy, K.; Henry, L.; Heuel,
J.; Hicheur, A.; Hidalgo Charman, R.; Hill, D.; Hilton, M.; Hopchev,
P. H.; Hu, J.; Hu, W.; Huang, W.; Huard, Z. C.; Hulsbergen, W.; Humair,
T.; Hunter, R. J.; Hushchyn, M.; Hutchcroft, D.; Hynds, D.; Ibis, P.;
Idzik, M.; Ilten, P.; Inglessi, A.; Inyakin, A.; Ivshin, K.; Jacobsson,
R.; Jakobsen, S.; Jalocha, J.; Jans, E.; Jashal, B. K.; Jawahery, A.;
Jevtic, V.; Jiang, F.; John, M.; Johnson, D.; Jones, C. R.; Jost, B.;
Jurik, N.; Kandybei, S.; Karacson, M.; Kariuki, J. M.; Kazeev, N.;
Kecke, M.; Keizer, F.; Kelsey, M.; Kenzie, M.; Ketel, T.; Khanji,
B.; Kharisova, A.; Kim, K. E.; Kirn, T.; Kirsebom, V. S.; Klaver,
S.; Klimaszewski, K.; Koliiev, S.; Kondybayeva, A.; Konoplyannikov,
A.; Kopciewicz, P.; Kopecna, R.; Koppenburg, P.; Kostiuk, I.; Kot,
O.; Kotriakhova, S.; Kravchuk, L.; Krawczyk, R. D.; Kreps, M.; Kress,
F.; Kretzschmar, S.; Krokovny, P.; Krupa, W.; Krzemien, W.; Kucewicz,
W.; Kucharczyk, M.; Kudryavtsev, V.; Kuindersma, H. S.; Kunde, G. J.;
Kuonen, A. K.; Kvaratskheliya, T.; Lacarrere, D.; Lafferty, G.; Lai,
A.; Lancierini, D.; Lane, J. J.; Lanfranchi, G.; Langenbruch, C.;
Latham, T.; Lazzari, F.; Lazzeroni, C.; Le Gac, R.; Lefèvre, R.;
Leflat, A.; Lemaitre, F.; Leroy, O.; Lesiak, T.; Leverington, B.;
Li, H.; Li, P. -R.; Li, X.; Li, Y.; Li, Z.; Liang, X.; Lindner, R.;
Lionetto, F.; Lisovskyi, V.; Liu, G.; Liu, X.; Loh, D.; Loi, A.; Lomba
Castro, J.; Longstaff, I.; Lopes, J. H.; Loustau, G.; Lovell, G. H.;
Lu, Y.; Lucchesi, D.; Lucio Martinez, M.; Luo, Y.; Lupato, A.; Luppi,
E.; Lupton, O.; Lusiani, A.; Lyu, X.; Maccolini, S.; Machefert, F.;
Maciuc, F.; Macko, V.; Mackowiak, P.; Maddrell-Mander, S.; Madhan
Mohan, L. R.; Maev, O.; Maevskiy, A.; Maguire, K.; Maisuzenko,
D.; Majewski, M. W.; Malde, S.; Malecki, B.; Malinin, A.; Maltsev,
T.; Malygina, H.; Manca, G.; Mancinelli, G.; Manera Escalero, R.;
Manuzzi, D.; Marangotto, D.; Maratas, J.; Marchand, J. F.; Marconi, U.;
Mariani, S.; Marin Benito, C.; Marinangeli, M.; Marino, P.; Marks, J.;
Marshall, P. J.; Martellotti, G.; Martinazzoli, L.; Martinelli, M.;
Martinez Santos, D.; Martinez Vidal, F.; Massafferri, A.; Materok,
M.; Matev, R.; Mathad, A.; Mathe, Z.; Matiunin, V.; Matteuzzi, C.;
Mattioli, K. R.; Mauri, A.; Maurice, E.; McCann, M.; Mcconnell, L.;
McNab, A.; McNulty, R.; Mead, J. V.; Meadows, B.; Meaux, C.; Meinert,
N.; Melnychuk, D.; Meloni, S.; Merk, M.; Merli, A.; Milanes, D. A.;
Millard, E.; Minard, M. -N.; Mineev, O.; Minzoni, L.; Mitchell, S. E.;
Mitreska, B.; Mitzel, D. S.; Modden, A.; Mogini, A.; Moise, R. D.;
Mombächer, T.; Monroy, I. A.; Monteil, S.; Morandin, M.; Morello, G.;
Morello, M. J.; Moron, J.; Morris, A. B.; Morris, A. G.; Mountain, R.;
Mu, H.; Muheim, F.; Mukherjee, M.; Mulder, M.; Müller, D.; Müller,
J.; Mëller, K.; Mëller, V.; Murphy, C. H.; Murray, D.; Muzzetto, P.;
Naik, P.; Nakada, T.; Nandakumar, R.; Nandi, A.; Nanut, T.; Nasteva,
I.; Needham, M.; Neri, N.; Neubert, S.; Neufeld, N.; Newcombe, R.;
Nguyen, T. D.; Nguyen-Mau, C.; Niel, E. M.; Nieswand, S.; Nikitin,
N.; Nolte, N. S.; Oblakowska-Mucha, A.; Obraztsov, V.; Ogilvy, S.;
O'Hanlon, D. P.; Oldeman, R.; Onderwater, C. J. G.; Osborn, J. D.;
Ossowska, A.; Otalora Goicochea, J. M.; Ovsiannikova, T.; Owen,
P.; Oyanguren, A.; Pais, P. R.; Pajero, T.; Palano, A.; Palutan, M.;
Panshin, G.; Papanestis, A.; Pappagallo, M.; Pappalardo, L. L.; Parker,
W.; Parkes, C.; Passaleva, G.; Pastore, A.; Patel, M.; Patrignani, C.;
Pearce, A.; Pellegrino, A.; Penso, G.; Pepe Altarelli, M.; Perazzini,
S.; Pereima, D.; Perret, P.; Pescatore, L.; Petridis, K.; Petrolini,
A.; Petrov, A.; Petrucci, S.; Petruzzo, M.; Pietrzyk, B.; Pietrzyk,
G.; Pikies, M.; Pili, M.; Pinci, D.; Pinzino, J.; Pisani, F.; Piucci,
A.; Placinta, V.; Playfer, S.; Plews, J.; Plo Casasus, M.; Polci,
F.; Poli Lener, M.; Poliakova, M.; Poluektov, A.; Polukhina, N.;
Polyakov, I.; Polycarpo, E.; Pomery, G. J.; Ponce, S.; Popov, A.;
Popov, D.; Poslavskii, S.; Prasanth, K.; Promberger, L.; Prouve,
C.; Pugatch, V.; Puig Navarro, A.; Pullen, H.; Punzi, G.; Qian,
W.; Qin, J.; Quagliani, R.; Quintana, B.; Raab, N. V.; Rachwal,
B.; Rademacker, J. H.; Rama, M.; Ramos Pernas, M.; Rangel, M. S.;
Ratnikov, F.; Raven, G.; Ravonel Salzgeber, M.; Reboud, M.; Redi,
F.; Reichert, S.; Reiss, F.; Remon Alepuz, C.; Ren, Z.; Renaudin,
V.; Ricciardi, S.; Richards, S.; Rinnert, K.; Robbe, P.; Robert, A.;
Rodrigues, A. B.; Rodrigues, E.; Rodriguez Lopez, J. A.; Roehrken, M.;
Roiser, S.; Rollings, A.; Romanovskiy, V.; Romero Lamas, M.; Romero
Vidal, A.; Roth, J. D.; Rotondo, M.; Rudolph, M. S.; Ruf, T.; Ruiz
Vidal, J.; Ryzka, J.; Saborido Silva, J. J.; Sagidova, N.; Saitta,
B.; Sanchez Gras, C.; Sanchez Mayordomo, C.; Sanmartin Sedes, B.;
Santacesaria, R.; Santamarina Rios, C.; Santimaria, M.; Santovetti, E.;
Sarpis, G.; Sarti, A.; Satriano, C.; Satta, A.; Saur, M.; Savrina, D.;
Scantlebury Smead, L. G.; Schael, S.; Schellenberg, M.; Schiller, M.;
Schindler, H.; Schmelling, M.; Schmelzer, T.; Schmidt, B.; Schneider,
O.; Schopper, A.; Schreiner, H. F.; Schubiger, M.; Schulte, S.;
Schune, M. H.; Schwemmer, R.; Sciascia, B.; Sciubba, A.; Sellam,
S.; Semennikov, A.; Sergi, A.; Serra, N.; Serrano, J.; Sestini, L.;
Seuthe, A.; Seyfert, P.; Shangase, D. M.; Shapkin, M.; Shears, T.;
Shekhtman, L.; Shevchenko, V.; Shmanin, E.; Shupperd, J. D.; Siddi,
B. G.; Silva Coutinho, R.; Silva de Oliveira, L.; Simi, G.; Simone,
S.; Skiba, I.; Skidmore, N.; Skwarnicki, T.; Slater, M. W.; Smeaton,
J. G.; Smetkina, A.; Smith, E.; Smith, I. T.; Smith, M.; Snoch, A.;
Soares, M.; Soares Lavra, L.; Sokoloff, M. D.; Soler, F. J. P.; Souza
De Paula, B.; Spaan, B.; Spadaro Norella, E.; Spradlin, P.; Stagni,
F.; Stahl, M.; Stahl, S.; Stefko, P.; Stefkova, S.; Steinkamp, O.;
Stemmle, S.; Stenyakin, O.; Stepanova, M.; Stevens, H.; Stocchi, A.;
Stone, S.; Stracka, S.; Stramaglia, M. E.; Straticiuc, M.; Straumann,
U.; Strokov, S.; Sun, J.; Sun, L.; Sun, Y.; Svihra, P.; Swientek,
K.; Szabelski, A.; Szumlak, T.; Szymanski, M.; Taneja, S.; Tang, Z.;
Tekampe, T.; Tellarini, G.; Teubert, F.; Thomas, E.; Thomson, K. A.;
Tilley, M. J.; Tisserand, V.; T'Jampens, S.; Tobin, M.; Tolk, S.;
Tomassetti, L.; Tonelli, D.; Tou, D. Y.; Tournefier, E.; Traill, M.;
Tran, M. T.; Trisovic, A.; Tsaregorodtsev, A.; Tuci, G.; Tully, A.;
Tuning, N.; Ukleja, A.; Usachov, A.; Ustyuzhanin, A.; Uwer, U.; Vagner,
A.; Vagnoni, V.; Valassi, A.; Valenti, G.; van Beuzekom, M.; Van Hecke,
H.; van Herwijnen, E.; Van Hulse, C. B.; van Tilburg, J.; van Veghel,
M.; Vazquez Gomez, R.; Vazquez Regueiro, P.; Vázquez Sierra, C.;
Vecchi, S.; Velthuis, J. J.; Veltri, M.; Venkateswaran, A.; Vernet,
M.; Veronesi, M.; Vesterinen, M.; Viana Barbosa, J. V.; Vieira, D.;
Vieites Diaz, M.; Viemann, H.; Vilasis-Cardona, X.; Vitkovskiy, A.;
Volkov, V.; Vollhardt, A.; Vom Bruch, D.; Vorobyev, A.; Vorobyev,
V.; Voropaev, N.; Waldi, R.; Walsh, J.; Wang, J.; Wang, J.; Wang,
M.; Wang, Y.; Wang, Z.; Ward, D. R.; Wark, H. M.; Watson, N. K.;
Websdale, D.; Weiden, A.; Weisser, C.; Westhenry, B. D. C.; White,
D. J.; Whitehead, M.; Wiedner, D.; Wilkinson, G.; Wilkinson, M.;
Williams, I.; Williams, M.; Williams, M. R. J.; Williams, T.; Wilson,
F. F.; Winn, M.; Wislicki, W.; Witek, M.; Wormser, G.; Wotton, S. A.;
Wu, H.; Wyllie, K.; Xiang, Z.; Xiao, D.; Xie, Y.; Xing, H.; Xu, A.;
Xu, L.; Xu, M.; Xu, Q.; Xu, Z.; Xu, Z.; Yang, Z.; Yang, Z.; Yao, Y.;
Yeomans, L. E.; Yin, H.; Yu, J.; Yuan, X.; Yushchenko, O.; Zarebski,
K. A.; Zavertyaev, M.; Zdybal, M.; Zeng, M.; Zhang, D.; Zhang, L.;
Zhang, S.; Zhang, W. C.; Zhang, Y.; Zhelezov, A.; Zheng, Y.; Zhou,
X.; Zhou, Y.; Zhu, X.; Zhukov, V.; Zonneveld, J. B.; Zucchelli, S.
Bibcode: 2020SCPMA..6321062A
Altcode:
A search for the doubly charmed baryon Ξ_{cc}^+ is performed through
its decay to the Λ_c^ + {K^ -}{π ^ +} final state, using proton-proton
collision data collected with the LHCb detector at centre-of-mass
energies of 7, 8 and 13 TeV. The data correspond to a total integrated
luminosity of 9 fb-1. No significant signal is observed in
the mass range from 3.4 to 3.8 GeV/ c 2. Upper limits are
set at 95% credibility level on the ratio of the Ξ_{cc}^+ production
cross-section times the branching fraction to that of Λ_c^ + and
Ξ_{cc}^{+ +} baryons. The limits are determined as functions of the
Ξ_{cc}^+ mass for different lifetime hypotheses, in the rapidity range
from 2.0 to 4.5 and the transverse momentum range from 4 to 15 GeV/ c.
Title: Search for the doubly charmed baryon Ξcc
+
Authors: LHCb Collaboration; Aaij, R.; Abellán Beteta, C.; Ackernley,
T.; Adeva, B.; Adinolfi, M.; Afsharnia, H.; Aidala, C. A.; Aiola, S.;
Ajaltouni, Z.; Akar, S.; Albicocco, P.; Albrecht, J.; Alessio, F.;
Alexander, M.; Alfonso Albero, A.; Alkhazov, G.; Alvarez Cartelle, P.;
Alves, A. A.; Amato, S.; Amhis, Y.; An, L.; Anderlini, L.; Andreassi,
G.; Andreotti, M.; Archilli, F.; Arnau Romeu, J.; Artamonov, A.;
Artuso, M.; Arzymatov, K.; Aslanides, E.; Atzeni, M.; Audurier, B.;
Bachmann, S.; Back, J. J.; Baker, S.; Balagura, V.; Baldini, W.;
Baranov, A.; Barlow, R. J.; Barsuk, S.; Barter, W.; Bartolini, M.;
Baryshnikov, F.; Bassi, G.; Batozskaya, V.; Batsukh, B.; Battig, A.;
Battista, V.; Bay, A.; Becker, M.; Bedeschi, F.; Bediaga, I.; Beiter,
A.; Bel, L. J.; Belavin, V.; Belin, S.; Beliy, N.; Bellee, V.; Belous,
K.; Belyaev, I.; Bencivenni, G.; Ben-Haim, E.; Benson, S.; Beranek,
S.; Berezhnoy, A.; Bernet, R.; Berninghoff, D.; Bernstein, H. C.;
Bertholet, E.; Bertolin, A.; Betancourt, C.; Betti, F.; Bettler,
M. O.; Bezshyiko, Ia.; Bhasin, S.; Bhom, J.; Bieker, M. S.; Bifani,
S.; Billoir, P.; Birnkraut, A.; Bizzeti, A.; Bjørn, M.; Blago,
M. P.; Blake, T.; Blanc, F.; Blusk, S.; Bobulska, D.; Bocci, V.;
Boente Garcia, O.; Boettcher, T.; Boldyrev, A.; Bondar, A.; Bondar,
N.; Borghi, S.; Borisyak, M.; Borsato, M.; Borsuk, J. T.; Bowcock,
T. J. V.; Bozzi, C.; Braun, S.; Brea Rodriguez, A.; Brodski, M.;
Brodzicka, J.; Brossa Gonzalo, A.; Brundu, D.; Buchanan, E.; Buonaura,
A.; Burr, C.; Bursche, A.; Butter, J. S.; Buytaert, J.; Byczynski, W.;
Cadeddu, S.; Cai, H.; Calabrese, R.; Cali, S.; Calladine, R.; Calvi,
M.; Calvo Gomez, M.; Camboni, A.; Campana, P.; Campora Perez, D. H.;
Capriotti, L.; Carbone, A.; Carboni, G.; Cardinale, R.; Cardini,
A.; Carniti, P.; Carvalho Akiba, K.; Casais Vidal, A.; Casse, G.;
Cattaneo, M.; Cavallero, G.; Cenci, R.; Cerasoli, J.; Chapman, M. G.;
Charles, M.; Charpentier, Ph.; Chatzikonstantinidis, G.; Chefdeville,
M.; Chekalina, V.; Chen, C.; Chen, S.; Chernov, A.; Chitic, S. -G.;
Chobanova, V.; Chrzaszcz, M.; Chubykin, A.; Ciambrone, P.; Cicala,
M. F.; Cid Vidal, X.; Ciezarek, G.; Cindolo, F.; Clarke, P. E. L.;
Clemencic, M.; Cliff, H. V.; Closier, J.; Cobbledick, J. L.; Coco, V.;
Coelho, J. A. B.; Cogan, J.; Cogneras, E.; Cojocariu, L.; Collins, P.;
Colombo, T.; Comerma-Montells, A.; Contu, A.; Cooke, N.; Coombs, G.;
Coquereau, S.; Corti, G.; Costa Sobral, C. M.; Couturier, B.; Craik,
D. C.; Crkovska, J.; Crocombe, A.; Cruz Torres, M.; Currie, R.; Da
Silva, C. L.; Dall'Occo, E.; Dalseno, J.; D'Ambrosio, C.; Danilina,
A.; d'Argent, P.; Davis, A.; De Aguiar Francisco, O.; De Bruyn, K.;
De Capua, S.; De Cian, M.; De Miranda, J. M.; De Paula, L.; De Serio,
M.; De Simone, P.; de Vries, J. A.; Dean, C. T.; Dean, W.; Decamp, D.;
Del Buono, L.; Delaney, B.; Dembinski, H. -P.; Demmer, M.; Dendek,
A.; Denysenko, V.; Derkach, D.; Deschamps, O.; Desse, F.; Dettori,
F.; Dey, B.; Di Canto, A.; Di Nezza, P.; Didenko, S.; Dijkstra, H.;
Dordei, F.; Dorigo, M.; dos Reis, A. C.; Douglas, L.; Dovbnya, A.;
Dreimanis, K.; Dudek, M. W.; Dufour, L.; Dujany, G.; Durante, P.;
Durham, J. M.; Dutta, D.; Dzhelyadin, R.; Dziewiecki, M.; Dziurda,
A.; Dzyuba, A.; Easo, S.; Egede, U.; Egorychev, V.; Eidelman, S.;
Eisenhardt, S.; Ekelhof, R.; Ek-In, S.; Eklund, L.; Ely, S.; Ene, A.;
Escher, S.; Esen, S.; Evans, T.; Falabella, A.; Fan, J.; Farley, N.;
Farry, S.; Fazzini, D.; Féo, M.; Fernandez Declara, P.; Fernandez
Prieto, A.; Ferrari, F.; Ferreira Lopes, L.; Ferreira Rodrigues,
F.; Ferreres Sole, S.; Ferrillo, M.; Ferro-Luzzi, M.; Filippov, S.;
Fini, R. A.; Fiorini, M.; Firlej, M.; Fischer, K. M.; Fitzpatrick,
C.; Fiutowski, T.; Fleuret, F.; Fontana, M.; Fontanelli, F.; Forty,
R.; Franco Lima, V.; Franco Sevilla, M.; Frank, M.; Frei, C.; Friday,
D. A.; Fu, J.; Fuehring, M.; Funk, W.; Gabriel, E.; Gallas Torreira,
A.; Galli, D.; Gallorini, S.; Gambetta, S.; Gan, Y.; Gandelman, M.;
Gandini, P.; Gao, Y.; Garcia Martin, L. M.; García Pardiñas, J.;
Garcia Plana, B.; Garcia Rosales, F. A.; Garra Tico, J.; Garrido,
L.; Gascon, D.; Gaspar, C.; Gerick, D.; Gersabeck, E.; Gersabeck,
M.; Gershon, T.; Gerstel, D.; Ghez, Ph.; Gibson, V.; Gioventù, A.;
Girard, O. G.; Gironella Gironell, P.; Giubega, L.; Giugliano, C.;
Gizdov, K.; Gligorov, V. V.; Göbel, C.; Golubkov, D.; Golutvin, A.;
Gomes, A.; Gorbounov, P.; Gorelov, I. V.; Gotti, C.; Govorkova, E.;
Grabowski, J. P.; Graciani Diaz, R.; Grammatico, T.; Granado Cardoso,
L. A.; Graugés, E.; Graverini, E.; Graziani, G.; Grecu, A.; Greim,
R.; Griffith, P.; Grillo, L.; Gruber, L.; Gruberg Cazon, B. R.;
Gu, C.; Gushchin, E.; Guth, A.; Guz, Yu.; Gys, T.; Hadavizadeh,
T.; Haefeli, G.; Haen, C.; Haines, S. C.; Hamilton, P. M.; Han,
Q.; Han, X.; Hancock, T. H.; Hansmann-Menzemer, S.; Harnew, N.;
Harrison, T.; Hart, R.; Hasse, C.; Hatch, M.; He, J.; Hecker, M.;
Heijhoff, K.; Heinicke, K.; Heister, A.; Hennequin, A. M.; Hennessy,
K.; Henry, L.; Heuel, J.; Hicheur, A.; Hidalgo Charman, R.; Hill,
D.; Hilton, M.; Hopchev, P. H.; Hu, J.; Hu, W.; Huang, W.; Huard,
Z. C.; Hulsbergen, W.; Humair, T.; Hunter, R. J.; Hushchyn, M.;
Hutchcroft, D.; Hynds, D.; Ibis, P.; Idzik, M.; Ilten, P.; Inglessi,
A.; Inyakin, A.; Ivshin, K.; Jacobsson, R.; Jakobsen, S.; Jalocha,
J.; Jans, E.; Jashal, B. K.; Jawahery, A.; Jevtic, V.; Jiang, F.;
John, M.; Johnson, D.; Jones, C. R.; Jost, B.; Jurik, N.; Kandybei,
S.; Karacson, M.; Kariuki, J. M.; Kazeev, N.; Kecke, M.; Keizer,
F.; Kelsey, M.; Kenzie, M.; Ketel, T.; Khanji, B.; Kharisova, A.;
Kim, K. E.; Kirn, T.; Kirsebom, V. S.; Klaver, S.; Klimaszewski, K.;
Koliiev, S.; Kondybayeva, A.; Konoplyannikov, A.; Kopciewicz, P.;
Kopecna, R.; Koppenburg, P.; Kostiuk, I.; Kot, O.; Kotriakhova, S.;
Kravchuk, L.; Krawczyk, R. D.; Kreps, M.; Kress, F.; Kretzschmar, S.;
Krokovny, P.; Krupa, W.; Krzemien, W.; Kucewicz, W.; Kucharczyk, M.;
Kudryavtsev, V.; Kuindersma, H. S.; Kunde, G. J.; Kuonen, A. K.;
Kvaratskheliya, T.; Lacarrere, D.; Lafferty, G.; Lai, A.; Lancierini,
D.; Lane, J. J.; Lanfranchi, G.; Langenbruch, C.; Latham, T.; Lazzari,
F.; Lazzeroni, C.; Le Gac, R.; Lefèvre, R.; Leflat, A.; Lemaitre, F.;
Leroy, O.; Lesiak, T.; Leverington, B.; Li, H.; Li, P. -R.; Li, X.;
Li, Y.; Li, Z.; Liang, X.; Lindner, R.; Lionetto, F.; Lisovskyi, V.;
Liu, G.; Liu, X.; Loh, D.; Loi, A.; Lomba Castro, J.; Longstaff, I.;
Lopes, J. H.; Loustau, G.; Lovell, G. H.; Lu, Y.; Lucchesi, D.; Lucio
Martinez, M.; Luo, Y.; Lupato, A.; Luppi, E.; Lupton, O.; Lusiani,
A.; Lyu, X.; Maccolini, S.; Machefert, F.; Maciuc, F.; Macko, V.;
Mackowiak, P.; Maddrell-Mander, S.; Madhan Mohan, L. R.; Maev, O.;
Maevskiy, A.; Maguire, K.; Maisuzenko, D.; Majewski, M. W.; Malde,
S.; Malecki, B.; Malinin, A.; Maltsev, T.; Malygina, H.; Manca,
G.; Mancinelli, G.; Manera Escalero, R.; Manuzzi, D.; Marangotto,
D.; Maratas, J.; Marchand, J. F.; Marconi, U.; Mariani, S.; Marin
Benito, C.; Marinangeli, M.; Marino, P.; Marks, J.; Marshall, P. J.;
Martellotti, G.; Martinazzoli, L.; Martinelli, M.; Martinez Santos, D.;
Martinez Vidal, F.; Massafferri, A.; Materok, M.; Matev, R.; Mathad,
A.; Mathe, Z.; Matiunin, V.; Matteuzzi, C.; Mattioli, K. R.; Mauri,
A.; Maurice, E.; McCann, M.; Mcconnell, L.; McNab, A.; McNulty,
R.; Mead, J. V.; Meadows, B.; Meaux, C.; Meinert, N.; Melnychuk,
D.; Meloni, S.; Merk, M.; Merli, A.; Milanes, D. A.; Millard, E.;
Minard, M. -N.; Mineev, O.; Minzoni, L.; Mitchell, S. E.; Mitreska,
B.; Mitzel, D. S.; Modden, A.; Mogini, A.; Moise, R. D.; Mombächer,
T.; Monroy, I. A.; Monteil, S.; Morandin, M.; Morello, G.; Morello,
M. J.; Moron, J.; Morris, A. B.; Morris, A. G.; Mountain, R.; Mu,
H.; Muheim, F.; Mukherjee, M.; Mulder, M.; Müller, D.; Müller, J.;
Mëller, K.; Mëller, V.; Murphy, C. H.; Murray, D.; Muzzetto, P.;
Naik, P.; Nakada, T.; Nandakumar, R.; Nandi, A.; Nanut, T.; Nasteva,
I.; Needham, M.; Neri, N.; Neubert, S.; Neufeld, N.; Newcombe, R.;
Nguyen, T. D.; Nguyen-Mau, C.; Niel, E. M.; Nieswand, S.; Nikitin,
N.; Nolte, N. S.; Oblakowska-Mucha, A.; Obraztsov, V.; Ogilvy, S.;
O'Hanlon, D. P.; Oldeman, R.; Onderwater, C. J. G.; Osborn, J. D.;
Ossowska, A.; Otalora Goicochea, J. M.; Ovsiannikova, T.; Owen,
P.; Oyanguren, A.; Pais, P. R.; Pajero, T.; Palano, A.; Palutan, M.;
Panshin, G.; Papanestis, A.; Pappagallo, M.; Pappalardo, L. L.; Parker,
W.; Parkes, C.; Passaleva, G.; Pastore, A.; Patel, M.; Patrignani, C.;
Pearce, A.; Pellegrino, A.; Penso, G.; Pepe Altarelli, M.; Perazzini,
S.; Pereima, D.; Perret, P.; Pescatore, L.; Petridis, K.; Petrolini,
A.; Petrov, A.; Petrucci, S.; Petruzzo, M.; Pietrzyk, B.; Pietrzyk,
G.; Pikies, M.; Pili, M.; Pinci, D.; Pinzino, J.; Pisani, F.; Piucci,
A.; Placinta, V.; Playfer, S.; Plews, J.; Plo Casasus, M.; Polci,
F.; Poli Lener, M.; Poliakova, M.; Poluektov, A.; Polukhina, N.;
Polyakov, I.; Polycarpo, E.; Pomery, G. J.; Ponce, S.; Popov, A.;
Popov, D.; Poslavskii, S.; Prasanth, K.; Promberger, L.; Prouve,
C.; Pugatch, V.; Puig Navarro, A.; Pullen, H.; Punzi, G.; Qian,
W.; Qin, J.; Quagliani, R.; Quintana, B.; Raab, N. V.; Rachwal,
B.; Rademacker, J. H.; Rama, M.; Ramos Pernas, M.; Rangel, M. S.;
Ratnikov, F.; Raven, G.; Ravonel Salzgeber, M.; Reboud, M.; Redi,
F.; Reichert, S.; Reiss, F.; Remon Alepuz, C.; Ren, Z.; Renaudin,
V.; Ricciardi, S.; Richards, S.; Rinnert, K.; Robbe, P.; Robert, A.;
Rodrigues, A. B.; Rodrigues, E.; Rodriguez Lopez, J. A.; Roehrken, M.;
Roiser, S.; Rollings, A.; Romanovskiy, V.; Romero Lamas, M.; Romero
Vidal, A.; Roth, J. D.; Rotondo, M.; Rudolph, M. S.; Ruf, T.; Ruiz
Vidal, J.; Ryzka, J.; Saborido Silva, J. J.; Sagidova, N.; Saitta,
B.; Sanchez Gras, C.; Sanchez Mayordomo, C.; Sanmartin Sedes, B.;
Santacesaria, R.; Santamarina Rios, C.; Santimaria, M.; Santovetti, E.;
Sarpis, G.; Sarti, A.; Satriano, C.; Satta, A.; Saur, M.; Savrina, D.;
Scantlebury Smead, L. G.; Schael, S.; Schellenberg, M.; Schiller, M.;
Schindler, H.; Schmelling, M.; Schmelzer, T.; Schmidt, B.; Schneider,
O.; Schopper, A.; Schreiner, H. F.; Schubiger, M.; Schulte, S.;
Schune, M. H.; Schwemmer, R.; Sciascia, B.; Sciubba, A.; Sellam,
S.; Semennikov, A.; Sergi, A.; Serra, N.; Serrano, J.; Sestini, L.;
Seuthe, A.; Seyfert, P.; Shangase, D. M.; Shapkin, M.; Shears, T.;
Shekhtman, L.; Shevchenko, V.; Shmanin, E.; Shupperd, J. D.; Siddi,
B. G.; Silva Coutinho, R.; Silva de Oliveira, L.; Simi, G.; Simone,
S.; Skiba, I.; Skidmore, N.; Skwarnicki, T.; Slater, M. W.; Smeaton,
J. G.; Smetkina, A.; Smith, E.; Smith, I. T.; Smith, M.; Snoch, A.;
Soares, M.; Soares Lavra, L.; Sokoloff, M. D.; Soler, F. J. P.; Souza
De Paula, B.; Spaan, B.; Spadaro Norella, E.; Spradlin, P.; Stagni,
F.; Stahl, M.; Stahl, S.; Stefko, P.; Stefkova, S.; Steinkamp, O.;
Stemmle, S.; Stenyakin, O.; Stepanova, M.; Stevens, H.; Stocchi, A.;
Stone, S.; Stracka, S.; Stramaglia, M. E.; Straticiuc, M.; Straumann,
U.; Strokov, S.; Sun, J.; Sun, L.; Sun, Y.; Svihra, P.; Swientek,
K.; Szabelski, A.; Szumlak, T.; Szymanski, M.; Taneja, S.; Tang,
Z.; Tekampe, T.; Tellarini, G.; Teubert, F.; Thomas, E.; Thomson,
K. A.; Tilley, M. J.; Tisserand, V.; T'Jampens, S.; Tobin, M.; Tolk,
S.; Tomassetti, L.; Tonelli, D.; Tou, D. Y.; Tournefier, E.; Traill,
M.; Tran, M. T.; Trisovic, A.; Tsaregorodtsev, A.; Tuci, G.; Tully,
A.; Tuning, N.; Ukleja, A.; Usachov, A.; Ustyuzhanin, A.; Uwer, U.;
Vagner, A.; Vagnoni, V.; Valassi, A.; Valenti, G.; van Beuzekom, M.;
Van Hecke, H.; van Herwijnen, E.; Van Hulse, C. B.; van Tilburg, J.;
van Veghel, M.; Vazquez Gomez, R.; Vazquez Regueiro, P.; Vázquez
Sierra, C.; Vecchi, S.; Velthuis, J. J.; Veltri, M.; Venkateswaran,
A.; Vernet, M.; Veronesi, M.; Vesterinen, M.; Viana Barbosa, J. V.;
Vieira, D.; Vieites Diaz, M.; Viemann, H.; Vilasis-Cardona, X.;
Vitkovskiy, A.; Volkov, V.; Vollhardt, A.; Vom Bruch, D.; Vorobyev,
A.; Vorobyev, V.; Voropaev, N.; Waldi, R.; Walsh, J.; Wang, J.; Wang,
J.; Wang, M.; Wang, Y.; Wang, Z.; Ward, D. R.; Wark, H. M.; Watson,
N. K.; Websdale, D.; Weiden, A.; Weisser, C.; Westhenry, B. D. C.;
White, D. J.; Whitehead, M.; Wiedner, D.; Wilkinson, G.; Wilkinson, M.;
Williams, I.; Williams, M.; Williams, M. R. J.; Williams, T.; Wilson,
F. F.; Winn, M.; Wislicki, W.; Witek, M.; Wormser, G.; Wotton, S. A.;
Wu, H.; Wyllie, K.; Xiang, Z.; Xiao, D.; Xie, Y.; Xing, H.; Xu, A.;
Xu, L.; Xu, M.; Xu, Q.; Xu, Z.; Xu, Z.; Yang, Z.; Yang, Z.; Yao, Y.;
Yeomans, L. E.; Yin, H.; Yu, J.; Yuan, X.; Yushchenko, O.; Zarebski,
K. A.; Zavertyaev, M.; Zdybal, M.; Zeng, M.; Zhang, D.; Zhang, L.;
Zhang, S.; Zhang, W. C.; Zhang, Y.; Zhelezov, A.; Zheng, Y.; Zhou,
X.; Zhou, Y.; Zhu, X.; Zhukov, V.; Zonneveld, J. B.; Zucchelli, S.
Bibcode: 2020SCPMA..6321062L
Altcode: 2020SCPMA..6321062A; 2019arXiv190912273L
A search for the doubly charmed baryon Ξcc
+ is performed through its decay to the
Λc+K-π+ final
state, using proton-proton collision data collected with the LHCb
detector at centre-of-mass energies of 7, 8 and 13 TeV. The data
correspond to a total integrated luminosity of 9 fb-1. No
significant signal is observed in the mass range from 3.4 to 3.8
GeV/c2. Upper limits are set at 95% credibility level on
the ratio of the Ξcc + production cross-section
times the branching fraction to that of Λc+
and Ξcc ++ baryons. The limits are determined
as functions of the Ξcc + mass for different
lifetime hypotheses, in the rapidity range from 2.0 to 4.5 and the
transverse momentum range from 4 to 15 GeV/c.
Title: The Solar Orbiter Mission - Getting Ready for Launch
Authors: Mueller, D.; St Cyr, O. C.; Zouganelis, Y.; Gilbert, H. R.;
Nieves-Chinchilla, T.
Bibcode: 2019AGUFMSH24A..01M
Altcode:
ESA's Solar Orbiter mission is scheduled for launch in February
2020, and will focus on exploring the linkage between the Sun and
the heliosphere. It is a collaborative mission with NASA that will
collect unique data that will allow us to study, e.g., the coupling
between macroscopic physical processes to those on kinetic scales, the
generation of solar energetic particles and their propagation into the
heliosphere, and the origin and acceleration of solar wind plasma. By
approaching as close as 0.28 AU, Solar Orbiter will view the Sun with
high spatial resolution and combine this with in-situ measurements
of the surrounding heliosphere. Over the course of the mission, the
highly elliptical orbit will get progressively more inclined to the
ecliptic plane. Thanks to this new perspective, Solar Orbiter will
deliver images and comprehensive data of the unexplored Sun's polar
regions and the side of the Sun not visible from Earth. This talk will
provide a mission overview, highlight synergies with NASA's Parker
Solar Probe and summarize pre-launch activities.
Title: Solar Orbiter's Science Activity Plan: Translating Questions
into Action
Authors: Zouganelis, Y.; Mueller, D.; De Groof, A.; Walsh, A. P.;
Williams, D.
Bibcode: 2019AGUFMSH21D3315Z
Altcode:
Solar Orbiter is a mission, scheduled for launch in February 2020,
with as main goal to observe solar activity from close by, both in and
out of the ecliptic, and to link it to the solar wind as sensed by its
in-situ sensors. The payload consists of 6 remote-sensing and 4 in-situ
instrument suites, which will have to coordinate their operations in
order to address the four mission objectives: (1) What drives the solar
wind and where does the heliospheric magnetic field originate? (2)
How do solar transients drive heliospheric variability? (3) How do
solar eruptions produce energetic particle radiation that fills the
heliosphere? (4) How does the solar dynamo work and drive connections
between the Sun and the heliosphere? We have to consider, however, that
each orbit around the Sun has different characteristics, including the
relative positions of the Earth and spacecraft (affecting downlink
rates and communications blackouts), trajectory events (such as
gravitational assist manoeuvres), and the phase of the solar activity
cycle. Furthermore, each orbit's science telemetry will be downloaded
during the next, so orbits cannot be planned individually. So how
will those science questions be translated into an actual plan of
observations that will fit into the mission? First, the component
questions are broken down into answerable questions along with the
observations they need from the payload. Then, in order to address this,
the so-called Science Activity Plan (SAP) has been developed. The
SAP groups together objectives that require similar observations
into Solar Orbiter Observing Plans (SOOPs), resulting in a strategic,
top-level view of the optimal opportunities for science observations
across the mission lifetime, allowing all four mission objectives to
be addressed. In this presentation, we introduce Solar Orbiter's SAP
through a series of examples and the strategy being followed.
Title: The SPICE (Spectral Imaging of the Coronal Environment)
Ultraviolet Imaging Spectrograph Investigation
Authors: Hassler, D.; Auchere, F.; Carlsson, M.; Fludra, A.; Giunta,
A. S.; Mueller, D.; Peter, H.; Parenti, S.; Teriaca, L.; Fredvik, T.
Bibcode: 2019AGUFMSH24A..02H
Altcode:
One of the primary objectives of the Solar Orbiter mission is to link
remote sensing observations of the solar surface structures with in-situ
observations of solar wind streams. The SPICE (Spectral Imaging of the
Coronal Environment) instrument will characterize the plasma properties
of regions near the Sun to directly compare with in-situ measurements
from both Solar Orbiter & Parker Solar Probe. Specifically, SPICE
will map outflow velocities of surface features to solar wind structures
with similar composition (FIP, M/q) measured in-situ by the SWA/HIS
instrument on Solar Orbiter. These observations will help discriminate
models of solar wind origin by matching composition signatures in
solar wind streams to surface feature composition, and discriminate
physical processes that inject material from closed structures into
solar wind streams. This presentation will provide an overview of
the SPICE investigation, including science & measurement objective,
instrument design, capabilities and performance as measured during
calibration prior to delivery to the Solar Orbiter spacecraft. The
presentation will also provide a description of the operations concept
and data processing during the mission.
Title: The Polarimetric and Helioseismic Imager on Solar Orbiter
Authors: Mueller, D.; Solanki, S. K.; del Toro Iniesta, J. C.
Bibcode: 2019AGUFMSH21D3292M
Altcode:
The Polarimetric and Helioseismic Imager on the Solar Orbiter mission
(SO/PHI) is the first magnetograph and helioseismology instrument
to observe the Sun from outside the Sun-Earth line. It is the key
instrument meant to address the top-level science question: How does
the solar dynamo work and drive connections between the Sun and the
heliosphere? SO/PHI will also play an important role in answering the
other top-level science questions of Solar Orbiter. It will provide
valuable supporting observations for Parker Solar Probe. The
instrument carries out narrow-band imaging spectro-polarimetry using a
tunable LiNbO3 Fabry-Perot etalon, while the polarisation modulation is
done with liquid crystal variable retarders (LCVRs). The line and the
nearby continuum are sampled at six wavelength points and the data are
recorded by a 2k x 2k CMOS detector. To save valuable telemetry, the
raw data are reduced already on board, including being inverted under
the assumption of a Milne-Eddington atmosphere. SO/PHI is composed of
two telescopes, the Full Disc Telescope (FDT), covers the full solar
disc at all phases of the orbit, while the High Resolution Telescope
(HRT), can resolve structures as small as 200 km on the Sun at closest
perihelion. The standard data products of SO/PHI are maps of the
photospheric magnetic field vector, line-of-sight velocity and continuum
intensity with a highest cadence of one minute. The operational modes
of SO/PHI are kept highly flexible allowing to adjust to the actual
science goal chosen for a Solar Orbiter operation window.
Title: Layer Selection in Progressive Transmission of
Motion-Compensated JPEG2000 Video
Authors: Maturana-Espinosa, José Carmelo; Garcia-Ortiz, Juan Pablo;
Müller, Daniel; Gonzalez-Ruiz, Vicente
Bibcode: 2019Elect...8.1032M
Altcode:
MCJ2K (Motion-Compensated JPEG2000) is a video codec based on MCTF
(Motion- Compensated Temporal Filtering) and J2K (JPEG2000). MCTF
analyzes a sequence of images, generating a collection of temporal
sub-bands, which are compressed with J2K. The R/D (Rate-Distortion)
performance in MCJ2K is better than the MJ2K (Motion JPEG2000)
extension, especially if there is a high level of temporal
redundancy. MCJ2K codestreams can be served by standard JPIP (J2K
Interactive Protocol) servers, thanks to the use of only J2K standard
file formats. In bandwidth-constrained scenarios, an important issue in
MCJ2K is determining the amount of data of each temporal sub-band that
must be transmitted to maximize the quality of the reconstructions
at the client side. To solve this problem, we have proposed two
rate-allocation algorithms which provide reconstructions that are
progressive in quality. The first, OSLA (Optimized Sub-band Layers
Allocation), determines the best progression of quality layers, but is
computationally expensive. The second, ESLA (Estimated-Slope sub-band
Layers Allocation), is sub-optimal in most cases, but much faster and
more convenient for real-time streaming scenarios. An experimental
comparison shows that even when a straightforward motion compensation
scheme is used, the R/D performance of MCJ2K competitive is compared
not only to MJ2K, but also with respect to other standard scalable
video codecs.
Title: The Next Generation Magnetic Spectrometer in Space: An
International Science Platform for Physics and Astrophysics at
Lagrange Point 2
Authors: Wakely, Scott; Schael, S.; Bay, A.; Beatty, J. J.; Berdugo,
J.; Buckley, J. H.; Caprioli, D.; Coutu, S.; von Doetinchem, P.;
Gast, H.; Heber, B.; Marrocchesi, P. S.; Mertsch, P.; Moskalenko, I.;
Müller, D.; Musser, J.; Nutter, S.; Ong, R. A.; Park, N.; Porter,
T. A.; Senatore, C.; Shchutska, L.
Bibcode: 2019BAAS...51g.172W
Altcode: 2019astro2020U.172W
This paper describes a proposed next-generation space-based magnet
spectrometer for physics and astrophysics.
Title: Cosmic-ray Isotope Measurements with HELIX
Authors: Park, N.; Beaufore, L.; Mbarek, R.; Muller, D.; Schreyer,
E.; Wakely, S.; Werner, T.; Wisher, I.; Tabata, M.; Gebhard, M.;
Kunkler, B.; Musser, J.; Michaels, K.; Visser, G.; Ellingwood, E.;
Hanna, D.; O'Brien, S.; Rosin, T.; Nutter, S.; Allison, P.; Beatty,
J.; McBride, K.; Chen, Y.; Coutu, S.; Mognet, I.; Yu, M.; Green, N.;
Tarle, G.; Tomasch, A.
Bibcode: 2019ICRC...36..121P
Altcode: 2019PoS...358..121P
No abstract at ADS
Title: Calibration of the Aerogel Tiles for the HELIX RICH
Authors: Allison, P.; Beatty, J.; Beaufore, L.; Chen, Y.; Coutu, S.;
Ellingwood, E.; Gebharb, M.; Green, N.; Hanna, D.; Kunkler, B.; Mognet,
S. I.; Mbarek, R.; McBride, K.; Michaels, K.; Muller, D.; Musser, J.;
Nutter, S.; O'Brien, S.; Park, N.; Rosin, T.; Schreyer, E.; Tarle,
G.; Tabata, M.; Tomasch, A.; Visser, G.; Wakely, S.; Werner, T.;
Wisher, I.; Yu, M.
Bibcode: 2019ICRC...36..133A
Altcode: 2019PoS...358..133A
No abstract at ADS
Title: Production of Silica Aerogel Radiator Tiles for the HELIX
RICH Detector
Authors: Allison, P.; Beatty, J.; Beaufore, L.; Chen, Y.; Coutu, S.;
Ellingwood, E.; Gebhard, M.; Green, N.; Hanna, D.; Kunkler, B.; Mognet,
S. I.; Mbarek, R.; McBride, K.; Michaels, K.; Muller, D.; Musser, J.;
Nutter, S.; O'Brien, S.; Park, N.; Rosin, T.; Schreyer, E.; Tarle,
G.; Tabata, M.; Tomasch, A.; Visser, G.; Wakely, S.; Werner, T.;
Wisher, I.; Yu, M.
Bibcode: 2019ICRC...36..139A
Altcode: 2019PoS...358..139A
No abstract at ADS
Title: ePESSTO Transient Classification Report for 2018-12-03
Authors: Pursiainen; M; Castro; N; Gutierrez; P, C.; Muller; T;
Yaron, O.
Bibcode: 2018TNSCR2051....1P
Altcode:
No abstract at ADS
Title: Space Weather JHelioviewer in a Heterogeneous World
Authors: West, Matthew; Berghmans, David; Mueller, Daniel; Jiggens,
Piers; Verstringe, Freek; Nicula, Bogdan; Bourgoignie, Bram
Bibcode: 2018cosp...42E3643W
Altcode:
The Space Weather JHelioviewer project aims to augment the freely
available services of the Helioviewer project with space weather
relevant capabilities. As such, it merges the output of several
networked software services by combining the display of 1D data
(timelines), 2D data (solar images and spectrograms), 3D data
(multispacecraft imaging, magnetic field lines mod- elling), solar
event detections (e.g., HEK), and space weather alerts. This talk will
highlight the experiences gathered while incorporating this system
with several diverse datasets and services.
Title: Biofilm in Space (BFS): designing a spaceflight experiment
Authors: Cortesao, Marta; Hellweg, Christine; Hemmersbach, Ruth;
Moeller, Ralf; Muecklich, Frank; Nisar, Zeena; Luo, Jiaqi; Zea, Luis;
Mueller, Daniel; Rubin, Phil
Bibcode: 2018cosp...42E.702C
Altcode:
Fungal growth has been detected aboard the Russian Space Station (Mir)
and the International Space Station (ISS), promoting biodegradation
of the spacecraft materials and compromising life-support systems
[1-2]. Defining filamentous fungi biofilms is currently in debate
among the scientific community. Nevertheless these are indeed
associated with higher tolerance and resistance to adverse conditions
[3-5]. To better monitor and control fungal contamination during
long duration spaceflight missions, the NASA-funded project "Biofilm
in Space (BFS)" comprises a spaceflight experiment aboard the ISS,
planned to be launched late 2018/early 2019 on a SpaceX flight. It
will study growth and biofilm formation in microgravity also testing
coupons of different materials (such as quartz, aluminum silicone, and
polycarbonate developed by the Saarland University), in the search for
spaceflight-relevant antimicrobial surfaces.To mature the experimental
design to be spaceflight ready, several pre-flight tests need to be
performed. For this, one of the tasks of the German Aerospace Center
(Institute of Aerospace Medicine, Cologne) is to define and optimize
the culturing conditions for the fungus Penicillium rubens on the
space hardware: the 12-well BioCell (developed by BioServe Space
Technologies). Because growth in the BioCell will inevitably differ from
common laboratory containers (such as flasks or multi-well plates), it
is important to assess: i) growth and biofilm formation in the BioCell;
ii) growth and adherence to coupons compared with planktonic growth
iii) needed adaptations for the space-proven culturing system. An
initial approach tested P. rubens growth in the 12-well BioCells,
both in simulated microgravity provided by clinorotation (μ x g)
and in ground static control (1 x g), as well as its adherence to two
different material coupons - cellulose membrane and aluminum. Results
revealed fungal growth on all the 12-wells of the BioCell culturing
system, within the tested 48h and 96h of incubation in both μ x g and
1 x g conditions. Biomass measurements showed more adhered biomass in
cellulose membrane coupons (average 100% increase) than in aluminum
coupons (average 3% increase). Additionally, fluorescence microscopy
of coupon-attached biomass disclosed their hyphal structure and
surrounding matrix. The 12-well BioCell was established as an adequate
culturing system for growth of P. rubens in the upcoming spaceflight
experiment aboard the ISS. This marks an important step in having new
methodologies to study filamentous fungi biofilms that will help to
develop the appropriate contamination-control measures, both on Earth
and in space. References1.Checinska, A. et al. Microbiomes of
the dust particles collected from the International Space Station and
Spacecraft Assembly Facilities. Microbiome 3, 50 (2015)2.Klintworth,
R. et al. Biological induced corrosion of materials II: new test methods
and experiences from MIR station. Acta Astronautica, 44(7), 569-578
(1999)3.Harding, M.W. et al. Can filamentous fungi form biofilms? Trends
in Microbiology 11, 475-80 (2009)4.Gutierrez-Correa, M. et al. Recent
advances on filamentous fungal biofilms for industrial uses. Applied
Biochemistry and Biotechnology 167, 1235-1253 (2012)5.Ramage, G. et
al. Our current understanding of fungal biofilms. Critical Reviews in
Microbiology 35, 340-355 (2009)
Title: Complex ecological interactions of Staphylococcus aureus in
tampons during menstruation
Authors: Jacquemond, Isaline; Muggeo, Anaëlle; Lamblin, Gery;
Tristan, Anne; Gillet, Yves; Bolze, Pierre Adrien; Bes, Michèle;
Gustave, Claude Alexandre; Rasigade, Jean-Philippe; Golfier,
François; Ferry, Tristan; Dubost, Audrey; Abrouk, Danis; Barreto,
Samuel; Prigent-Combaret, Claire; Thioulouse, Jean; Lina, Gérard;
Muller, Daniel
Bibcode: 2018NatSR...8.9942J
Altcode:
Menstrual toxic shock syndrome (mTSS) is a severe disease that occurs
in healthy women vaginally colonized by Staphylococcus aureus producing
toxic shock toxin 1 and who use tampons. The aim of the present study
was to determine the impact of the composition of vaginal microbial
communities on tampon colonisation by S. aureus during menses. We
analysed the microbiota in menstrual fluids extracted from tampons
from 108 healthy women and 7 mTSS cases. Using culture, S. aureus
was detected in menstrual fluids of 40% of healthy volunteers and
100% of mTSS patients. Between class analysis of culturomic and 16S
rRNA gene metabarcoding data indicated that the composition of the
tampons' microbiota differs according to the presence or absence of
S. aureus and identify discriminating genera. However, the bacterial
communities of tampon fluid positive for S. aureus did not cluster
together. No difference in tampon microbiome richness, diversity, and
ecological distance was observed between tampon vaginal fluids with
or without S. aureus, and between healthy donors carrying S. aureus
and mTSS patients. Our results show that the vagina is a major
niche of. S. aureus in tampon users and the composition of the tampon
microbiota control its virulence though more complex interactions than
simple inhibition by lactic acid-producing bacterial species.
Title: VizieR Online Data Catalog: The Czech Variable Star Catalogue
(Skarka+, 2017)
Authors: Skarka, M.; Masek, M.; Brat, L.; Cagas, Pa.; Jurysek, J.;
Honkova, K.; Zejda, M.; Smelcer, L.; Jelinek, M.; Lomoz, F.; Tylsar,
M.; Trnka, J.; Pejcha, O.; Pintr, P.; Lehky, M.; Janik, J.; Cervinka,
L.; Pribik, V.; Motl, D.; Walter, F.; Zasche, P.; Koss, K.; Hajek,
P.; Bilek, F.; Liska, J.; Kucakova, H.; Bodnar, F.; Beranek, J.;
Safar, J.; Moudra, M.; Orsulak, M.; Pintr, M.; Sobotka, P.; Dreveny,
R.; Juranova, A.; Polak, J.; Polster, J.; Onderkova, K.; Smolka, M.;
Auer, R. F.; Kocian, R.; Hladik, B.; Cagas, P.; Gres, A.; Muller,
D.; Capkova, H.; Kysely, J.; Hornoch, K.; Truparova, K.; Timko, L.;
Broz, M.; Bilek, M.; Sebela, P.; Hanzl, D.; Zampachova, E.; Secka,
J.; Pravec; P.; Mrnak, P.; Svoboda, P.; Ehrenberger, R.; Novotny,
F.; Poddany, S.; Prudil, Z.; Kuchtak, B.; Stegner, D.
Bibcode: 2018yCatp043018500S
Altcode:
The Czech Variable star catalogue (CzeV) was created by L. Brat (2005,
2006) as a public online database that serves as a list of variable
stars whose variability was discovered by observers from the Czech
Republic. The initial idea comes from M. Zejda, who compiled Czech
discoveries till the establishment of the CzeV catalogue. The CzeV is
managed and administrated by the Variable Star and Exoplanet Section
of the Czech Astronomical Society (VSES CAS) and is available at
http://var2.astro.cz/czev.php. (1 data file).
Title: Understanding the usage of the Helioviewer Project clients
and services
Authors: Ireland, Jack; Zahniy, Serge; Mueller, Daniel; Nicula, Bogdan;
Verstringe, Freek; Bourgoignie, Bram; Buchlin, Eric; Alingery, Pablo
Bibcode: 2018tess.conf30286I
Altcode:
The Helioviewer Project enables visual exploration of the Sun
and the inner heliosphere for everyone, everywhere via intuitive
interfaces and novel technology. The project mainly develops two
clients, helioviewer.org and JHelioviewer, and the server-side
capabilities accessed via those clients. Images from many different
ground and space-based sources are currently available from multiple
servers. Solar and heliospheric feature and event information,
magnetic field extrapolations and important time-series can also be
browsed and visualized using Helioviewer Project clients. Users of the
Helioviewer Project have made over two million movies and many millions
of screenshots since detailed (and anonymous) logging of Helioviewer
Project usage was implemented in February 2011. These usage logs are
analyzed to give a detailed breakdown on user interaction with solar
and heliospheric data via Helioviewer Project clients and services. We
present summary statistics on how our users are using our clients
and services, which data they are interested in, and how they choose
to interact with different data sources. At the poster presentation
we will also be soliciting ideas from the community to improve our
clients and services.
Title: Solar Orbiter Mission Status Update
Authors: Mueller, Daniel; Zouganelis, Yannis; St. Cyr, Chris;
Gilbert, Holly
Bibcode: 2018EGUGA..2014217M
Altcode:
ESA's next heliophysics mission, Solar Orbiter, will focus on exploring
the linkage between the Sun and the heliosphere. It will collect unique
data that will allow us to study, e.g., the coupling between macroscopic
physical processes to those on kinetic scales, the generation of solar
energetic particles and their propagation into the heliosphere and
the origin and acceleration of solar wind plasma. By approaching as
close as 0.28 AU, Solar Orbiter will view the Sun with high spatial
resolution and combine this with in-situ measurements of the surrounding
heliosphere. Thanks to its unique out-of-ecliptic orbit, Solar Orbiter
will deliver images and data of the unexplored Sun's polar regions
and the side of the Sun not visible from Earth. This talk will provide
an update on the mission's development status and highlight synergies
with NASA's Parker Solar Probe and the heliophysics observatory.
Title: Anisotropic cosmological solutions in R + R^2 gravity
Authors: Müller, Daniel; Ricciardone, Angelo; Starobinsky, Alexei A.;
Toporensky, Aleksey
Bibcode: 2018EPJC...78..311M
Altcode: 2017arXiv171008753M
In this paper we investigate the past evolution of an anisotropic
Bianchi I universe in R+R^2 gravity. Using the dynamical system approach
we show that there exists a new two-parameter set of solutions that
includes both an isotropic "false radiation" solution and an anisotropic
generalized Kasner solution, which is stable. We derive the analytic
behavior of the shear from a specific property of f( R) gravity and
the analytic asymptotic form of the Ricci scalar when approaching the
initial singularity. Finally, we numerically check our results.
Title: Order out of Randomness: Self-Organization Processes in
Astrophysics
Authors: Aschwanden, Markus J.; Scholkmann, Felix; Béthune, William;
Schmutz, Werner; Abramenko, Valentina; Cheung, Mark C. M.; Müller,
Daniel; Benz, Arnold; Chernov, Guennadi; Kritsuk, Alexei G.; Scargle,
Jeffrey D.; Melatos, Andrew; Wagoner, Robert V.; Trimble, Virginia;
Green, William H.
Bibcode: 2018SSRv..214...55A
Altcode: 2017arXiv170803394A
Self-organization is a property of dissipative nonlinear processes
that are governed by a global driving force and a local positive
feedback mechanism, which creates regular geometric and/or
temporal patterns, and decreases the entropy locally, in contrast
to random processes. Here we investigate for the first time a
comprehensive number of (17) self-organization processes that
operate in planetary physics, solar physics, stellar physics,
galactic physics, and cosmology. Self-organizing systems create
spontaneous " order out of randomness", during the evolution from an
initially disordered system to an ordered quasi-stationary system,
mostly by quasi-periodic limit-cycle dynamics, but also by harmonic
(mechanical or gyromagnetic) resonances. The global driving force
can be due to gravity, electromagnetic forces, mechanical forces
(e.g., rotation or differential rotation), thermal pressure, or
acceleration of nonthermal particles, while the positive feedback
mechanism is often an instability, such as the magneto-rotational
(Balbus-Hawley) instability, the convective (Rayleigh-Bénard)
instability, turbulence, vortex attraction, magnetic reconnection,
plasma condensation, or a loss-cone instability. Physical models
of astrophysical self-organization processes require hydrodynamic,
magneto-hydrodynamic (MHD), plasma, or N-body simulations. Analytical
formulations of self-organizing systems generally involve coupled
differential equations with limit-cycle solutions of the Lotka-Volterra
or Hopf-bifurcation type.
Title: ESA's Solar Orbiter Mission Status Update
Authors: Mueller, D.; Zouganelis, Y.; St Cyr, O. C.; Gilbert, H. R.
Bibcode: 2017AGUFMSH21C..03M
Altcode:
Solar Orbiter, the first mission of ESA's Cosmic Vision programme,
promises to deliver groundbreaking science with previously unavailable
observational capabilities provided by a suite of in-situ and
remote-sensing instruments in a unique orbit. The mission will
address the central question of heliophysics: How does the Sun create
and control the heliosphere? The heliosphere represents a uniquely
accessible domain of space, where fundamental physical processes common
to solar, astrophysical and laboratory plasmas can be studied under
conditions impossible to reproduce on Earth and unfeasible to observe
from astronomical distances. In this talk, we highlight the scientific
goals of Solar Orbiter, address the synergy between this joint ESA/NASA
mission and other new space and ground-based observatories, and present
the mission's development status.
Title: Understanding the usage of the Helioviewer Project clients
and services
Authors: Ireland, J.; Zahniy, S.; Mueller, D.; Nicula, B.; Verstringe,
F.; Bourgoignie, B.; Buchlin, E.; Alingery, P.
Bibcode: 2017AGUFMSH51C2507I
Altcode:
The Helioviewer Project enables visual exploration of the Sun
and the inner heliosphere for everyone, everywhere via intuitive
interfaces and novel technology. The project mainly develops two
clients, helioviewer.org and JHelioviewer, and the server-side
capabilities accessed via those clients. Images from many different
ground and space-based sources are currently available from multiple
servers. Solar and heliospheric feature and event information,
magnetic field extrapolations and important time-series can also be
browsed and visualized using Helioviewer Project clients. Users of the
Helioviewer Project have made over two million movies and many millions
of screenshots since detailed (and anonymous) logging of Helioviewer
Project usage was implemented in February 2011. These usage logs are
analyzed to give a detailed breakdown on user interaction with solar
and heliospheric data via Helioviewer Project clients and services. We
present summary statistics on how our users are using our clients
and services, which data they are interested in, and how they choose
to interact with different data sources. At the poster presentation
we will also be soliciting ideas from the community to improve our
clients and services.
Title: 3D Visualization of Solar Data: Preparing for Solar Orbiter
and Parker Solar Probe
Authors: Mueller, D.; Nicula, B.; Felix, S.; Verstringe, F.;
Bourgoignie, B.; Csillaghy, A.; Berghmans, D.; Jiggens, P.; Ireland,
J.; Fleck, B.
Bibcode: 2017AGUFMSH23D2686M
Altcode:
Solar Orbiter and Parker Solar Probe will focus on exploring the
linkage between the Sun and the heliosphere. These new missions will
collect unique data that will allow us to study, e.g., the coupling
between macroscopic physical processes to those on kinetic scales,
the generation of solar energetic particles and their propagation
into the heliosphere and the origin and acceleration of solar wind
plasma. Combined with the several petabytes of data from NASA's Solar
Dynamics Observatory, the scientific community will soon have access
to multidimensional remote-sensing and complex in-situ observations
from different vantage points, complemented by petabytes of simulation
data. Answering overarching science questions like "How do solar
transients drive heliospheric variability and space weather?" will
only be possible if the community has the necessary tools at hand. In
this contribution, we will present recent progress in visualizing the
Sun and its magnetic field in 3D using the open-source JHelioviewer
framework, which is part of the ESA/NASA Helioviewer Project.
Title: JHelioviewer. Time-dependent 3D visualisation of solar and
heliospheric data
Authors: Müller, D.; Nicula, B.; Felix, S.; Verstringe, F.;
Bourgoignie, B.; Csillaghy, A.; Berghmans, D.; Jiggens, P.;
García-Ortiz, J. P.; Ireland, J.; Zahniy, S.; Fleck, B.
Bibcode: 2017A&A...606A..10M
Altcode: 2017arXiv170507628M
Context. Solar observatories are providing the world-wide community
with a wealth of data, covering wide time ranges (e.g. Solar and
Heliospheric Observatory, SOHO), multiple viewpoints (Solar TErrestrial
RElations Observatory, STEREO), and returning large amounts of data
(Solar Dynamics Observatory, SDO). In particular, the large volume of
SDO data presents challenges; the data are available only from a few
repositories, and full-disk, full-cadence data for reasonable durations
of scientific interest are difficult to download, due to their size
and the download rates available to most users. From a scientist's
perspective this poses three problems: accessing, browsing, and finding
interesting data as efficiently as possible.
Aims: To address
these challenges, we have developed JHelioviewer, a visualisation
tool for solar data based on the JPEG 2000 compression standard
and part of the open source ESA/NASA Helioviewer Project. Since the
first release of JHelioviewer in 2009, the scientific functionality
of the software has been extended significantly, and the objective
of this paper is to highlight these improvements.
Methods:
The JPEG 2000 standard offers useful new features that facilitate the
dissemination and analysis of high-resolution image data and offers
a solution to the challenge of efficiently browsing petabyte-scale
image archives. The JHelioviewer software is open source, platform
independent, and extendable via a plug-in architecture.
Results: With JHelioviewer, users can visualise the Sun for any time
period between September 1991 and today; they can perform basic image
processing in real time, track features on the Sun, and interactively
overlay magnetic field extrapolations. The software integrates solar
event data and a timeline display. Once an interesting event has
been identified, science quality data can be accessed for in-depth
analysis. As a first step towards supporting science planning of the
upcoming Solar Orbiter mission, JHelioviewer offers a virtual camera
model that enables users to set the vantage point to the location of
a spacecraft or celestial body at any given time.
Title: Solar Orbiter Status Report
Authors: Gilbert, Holly; St. Cyr, Orville Chris; Mueller, Daniel;
Zouganelis, Yannis; Velli, Marco
Bibcode: 2017SPD....4811004G
Altcode:
With the delivery of the instruments to the spacecraft builder, the
Solar Orbiter mission is in the midst of Integration & Testing
phase at Airbus in Stevenage, U.K. This mission to “Explore the
Sun-Heliosphere Connection” is the first medium-class mission of
ESA’s Cosmic Vision 2015-2025 program and is being jointly implemented
with NASA. The dedicated payload of 10 remote-sensing and in-situ
instruments will orbit the Sun as close as 0.3 A.U. and will provide
measurments from the photosphere into the solar wind. The three-axis
stabilized spacecraft will use Venus gravity assists to increase the
orbital inclination out of the ecliptic to solar latitudes as high as 34
degrees in the extended mission. The science team of Solar Orbiter has
been working closely with the Solar Probe Plus scientists to coordinate
observations between these two highly-complementary missions. This will
be a status report on the mission development; the interested reader
is referred to the recent summary by Müller et al., Solar Physics 285
(2013).
Title: Solar Orbiter Status Report
Authors: Gilbert, Holly; Cyr, Chris S.; Mueller, Daniel; Zouganelis,
Yannis; Velli, Marco
Bibcode: 2017shin.confE.139G
Altcode:
With the delivery of the instruments to the spacecraft builder,
the Solar Orbiter mission is in the midst of Integration &
Testing phase at Airbus in Stevenage, U.K. This mission to "Explore
the Sun-Heliosphere Connection" is the first medium-class mission of
ESA's Cosmic Vision 2015-2025 program and is being jointly implemented
with NASA. The dedicated payload of 10 remote-sensing and in-situ
instruments will orbit the Sun as close as 0.3 A.U. and will provide
measurments from the photosphere into the solar wind. The three-axis
stabilized spacecraft will use Venus gravity assists to increase the
orbital inclination out of the ecliptic to solar latitudes as high as 34
degrees in the extended mission. The science team of Solar Orbiter has
been working closely with the Solar Probe Plus scientists to coordinate
observations between these two highly-complementary missions. This will
be a status report on the mission development; the interested reader
is referred to the recent summary by Müller et al., Solar Physics 285
(2013).
Title: Rapidity profiles from 3+1D Glasma simulations with finite
longitudinal thickness
Authors: Ipp, A.; Mueller, D.
Bibcode: 2017ehep.confE.176I
Altcode: 2017arXiv171001732I; 2017PoS...314E.176I
We present our progress on simulating the Glasma in the early stages
of heavy ion collisions in a non-boost-invariant setting. Our approach
allows us to describe colliding nuclei with finite longitudinal width
by extending the McLerran-Venugopalan model to include a parameter for
the Lorentz-contracted but finite extent of the nucleus in the beam
direction. We determine the rapidity profile of the Glasma energy
density, which shows strong deviations from the boost invariant
result. Both broad and narrow profiles can be produced by varying the
initial conditions. We find reasonable agreement when we compare the
results to rapidity profiles of measured pion multiplicities from RHIC.
Title: JPEG2000 Image Compression on Solar EUV Images
Authors: Fischer, Catherine E.; Müller, Daniel; De Moortel, Ineke
Bibcode: 2017SoPh..292...16F
Altcode: 2017arXiv170201946F
For future solar missions as well as ground-based telescopes,
efficient ways to return and process data have become increasingly
important. Solar Orbiter, which is the next ESA/NASA mission to explore
the Sun and the heliosphere, is a deep-space mission, which implies a
limited telemetry rate that makes efficient onboard data compression
a necessity to achieve the mission science goals. Missions like the
Solar Dynamics Observatory (SDO) and future ground-based telescopes
such as the Daniel K. Inouye Solar Telescope, on the other hand, face
the challenge of making petabyte-sized solar data archives accessible
to the solar community. New image compression standards address
these challenges by implementing efficient and flexible compression
algorithms that can be tailored to user requirements. We analyse solar
images from the Atmospheric Imaging Assembly (AIA) instrument onboard
SDO to study the effect of lossy JPEG2000 (from the Joint Photographic
Experts Group 2000) image compression at different bitrates. To assess
the quality of compressed images, we use the mean structural similarity
(MSSIM) index as well as the widely used peak signal-to-noise ratio
(PSNR) as metrics and compare the two in the context of solar EUV
images. In addition, we perform tests to validate the scientific use
of the lossily compressed images by analysing examples of an on-disc
and off-limb coronal-loop oscillation time-series observed by AIA/SDO.
Title: On stability of the Kasner solution in quadratic gravity
Authors: Toporensky, A.; Müller, D.
Bibcode: 2017GReGr..49....8T
Altcode: 2016arXiv160302851T
We consider the dynamics of a flat anisotropic Universe filled
by a perfect fluid near a cosmological singularity in quadratic
gravity. Two possible regimes are described—the Kasner anisotropic
solution and an isotropic "vacuum radiation" solution which has three
sub cases depending on whether the equation of state parameter w is
bigger, smaller or equals to 1 / 3. Initial conditions for numerical
integrations have been chosen near a General Relativity anisotropic
solution with matter (Jacobs solution). We have found that for such
initial conditions there is a range of values of the coupling constants
so that the resulting cosmological singularity is isotropic.
Title: Cosmic-ray isotope measurements with HELIX
Authors: Coutu, S.; Beatty, J.; Gebhard, M.; Green, N.; Hanna, D.;
Kunkler, B.; Lang, M.; Mognet, I.; Muller, D.; Musser, J.; Nutter,
S.; Park, N.; Schubnell, M.; Tarlé., G.; Tomasch, A.; Visser, G.;
Wakely, S.; Wisher, I.
Bibcode: 2017ICRC...35..226C
Altcode: 2017PoS...301..226C
No abstract at ADS
Title: Solar Wind Core Electrons: Kappa or Maxwellian?
Authors: Walsh, A. P.; Osuna, P.; Toledo Redondo, S.; Zouganelis, Y.;
Masson, A.; De Groof, A.; Mueller, D.; Perrone, D.; Roberts, O. W.;
Taylor, M. G.; Turc, L.
Bibcode: 2016AGUFMSH51D2608W
Altcode:
Solar wind core electrons are typically considered to have a Maxwellian
velocity distribution function. However, most measurements made of
them to date don't have sufficient energy resolution to distinguish
between a Maxwellian and a kappa distribution at low energies. Here
we present a survey of solar wind electron velocity distribution
functions observed by Cluster PEACE in its highest energy resolution
mode, which is sufficient to distinguish between Maxwellian and kappa
distributions for energies below 15eV. Initial results suggest that a
kappa distribution better fits the data than a Maxwellian in all cases;
in the majority of cases the difference in goodness of fit between a
kappa and Maxwellian is small but in some cases, a kappa distribution
fits the data significantly better.
Title: Solar Orbiter Status Update
Authors: Zouganelis, Y.; Mueller, D.; St Cyr, O. C.; Gilbert, H. R.
Bibcode: 2016AGUFMSH53A..02Z
Altcode:
Solar Orbiter, the first mission of ESA's Cosmic Vision 2015-2025
programme, promises to deliver groundbreaking science with previously
unavailable observational capabilities provided by a suite of in-situ
and remote-sensing instruments in a unique orbit. The mission will
address the central question of heliophysics: How does the Sun create
and control the heliosphere? The heliosphere represents a uniquely
accessible domain of space, where fundamental physical processes common
to solar, astrophysical and laboratory plasmas can be studied under
conditions impossible to reproduce on Earth and unfeasible to observe
from astronomical distances. In this talk, we highlight the scientific
goals of Solar Orbiter, address the synergy between this joint ESA/NASA
mission and other new space and ground-based observatories, and present
the mission's development status.
Title: New features of the Helioviewer Project
Authors: Ireland, J.; Zahniy, S.; Nicula, B.; Mueller, D.; Felix,
S.; Verstringe, F.; Bourgoignie, B.
Bibcode: 2016AGUFMSH11A2212I
Altcode:
This year saw the release of major new upgrades to the capabilities
of helioviewer.org and JHelioviewer. The helioviewer.org interface
was completely re-designed, and now provides image and feature/event
time-lines and data download capabilities. JHelioviewer introduced
interactive time-series, the ability to query different servers for
different data, and image reprojection. We introduce the new features
of these software releases and give use cases. We will summarize our
latest usage statistics, and discuss what's coming up next for the
Helioviewer Project. We will also be soliciting bug reports, requests
for new features and comments on the effectiveness of helioviewer.org
and JHelioviewer. What would you like to see next from the Helioviewer
Project?
Title: 20 Years of SOHO
Authors: Fleck, Bernhard; Müller, Daniel
Bibcode: 2016ENews..47c..27F
Altcode:
The Solar and Heliospheric Observatory (SOHO), a joint mission of ESA
and NASA, has provided unparalleled insight into the Sun over the past
20 years - from its interior, through the hot and dynamic atmosphere,
out to the solar wind and its interaction with the interstellar
medium. SOHO also plays a vital role in forecasting potentially
dangerous space weather situations by continuously monitoring solar
storms, and unexpectedly also became the most prolific discoverer of
comets in the history of astronomy.
Title: Optimisation of Solar Orbiter Data Return
Authors: Lakey, D. T.; Tanco, I.; Sánchez Pérez, J. M.; Ravera
Iglesias, G.; Thürey, S.; Müller, D.; Sanchez, L.; Lefort, J.;
Eiblmaier, M. G.
Bibcode: 2016spop.conf.2618L
Altcode:
ESA's Solar Orbiter mission, with NASA participation, scheduled for
launch in 2018 will, after a multi-year cruise phase, enter into an
elliptical orbit around the sun with a perihelion of around 0.3 AU and
an increasing inclination of up to 35° to return images of the solar
polar regions and probe the plasma of the inner heliosphere. It promises
to deliver ground-breaking science with its extensive suite of in-situ
and remote-sensing instruments in a unique orbit. As a deep space
mission, Solar Orbiter has a highly constrained data downlink, which
means that optimising the science data return of the mission within the
constraints is of paramount importance. Data return represents one of
the greatest operational challenges for the mission as data downlink
rates vary dramatically, and irregularly, over the mission due to the
Spacecraft-Earth distance not following the usual periodicity seen
for planet-bound missions. Furthermore, the nature of the baseline
orbit tends to put science generation peaks at different times to the
peaks of data downlink rate. To improve the situation, the Mission
Analysis department at ESA's European Spacecraft Operations Centre
(ESOC) have designed alternative trajectories that optimise the overall
data downlink while retaining the overall orbit configuration to meet
the science objectives. Compared to the baseline trajectory, these new
options can more than double the data return within particular periods
of interest. After launch it will be the responsibility of the Mission
Operations Centre (MOC) and the Science Operations Centre (SOC) to
optimise data return. To this end, both MOC and SOC have independently
created models of data generation versus data return so as to examine
the effects of different parameters. MOC has identified three parameters
which can be modified: duration and method of ranging; use of redundant
storage capacity; and management of the real-time data generated during
the pass itself to avoid duplicating data on the real-time and playback
channels. The combined effect of these optimisations alone results in
an increase of data return of around 20%. SOC considered the generation
of data as well as the return, and examined the detailed on-board mass
memory partitioning. SOC also considered further optimisation of the
time and duration of the downlink passes. As a result SOC expects to
be able to increase data return potential substantially.
Title: Solar Orbiter - Exploring the Sun-Heliosphere Connection
Authors: Zouganelis, Ioannis; Mueller, Daniel; St. Cyr, Chris; Gilbert,
Holly R.
Bibcode: 2016EGUGA..18.7994Z
Altcode:
Solar Orbiter, the first mission of ESA's Cosmic Vision 2015-2025
programme, promises to deliver groundbreaking science with previously
unavailable observational capabilities provided by a suite of in-situ
and remote-sensing instruments in a unique orbit. The mission will
address the central question of heliophysics: How does the Sun create
and control the heliosphere? The heliosphere represents a uniquely
accessible domain of space, where fundamental physical processes
common to solar, astrophysical and laboratory plasmas can be studied
under conditions impossible to reproduce on Earth and unfeasible
to observe from astronomical distances. In this talk, we highlight
the scientific goals of Solar Orbiter, address the synergy between
this joint ESA/NASA mission and other new space- and ground-based
observatories, and present the mission's development status.
Title: Interactive Streaming of Sequences of High-Resolution JPEG
2000 Images
Authors: Sanchez-Hernandez, J. J.; Garcia-Ortiz, J. P.; Gonzalez-Ruiz,
V.; Müller, D.
Bibcode: 2015ITMm...1770595S
Altcode:
The JPEG2000 image coding system was created with the intention of
superseding the original JPEG standard, using a novel wavelet-based
method. The main advantage of JPEG2000 is the flexibility of its
code-stream, which provides new functionality related to the interactive
transmission of images. For this task, JPEG2000 uses the JPIP protocol,
which enables real-time spatial random access while the retrieved image
is progressively displayed (streaming). The standard also foresees
the compression and transmission of sequences of images by repeating
this approach for each image. In this framework, this paper presents
the Continue data-flow control strategy, a JPIP-compliant solution for
the interactive streaming of sequences of images that are transmitted
over time-varying communication channels. In this context, the random
fluctuation of the capacity of the transmission channel over the time
forces the clients to prefetch a minimal amount of the code-stream
of each image of the beginning of the transmitted sequence before
the playback starts, and the server to decide, in real-time, which
amount of the code-stream of each compressed image is going to be
transmitted . The estimated channel capacity is performed by clients
and the rate-control at the server is straightforward, resulting in
a highly scalable image retrieval system. The experiments conducted
in this study demonstrate that the proposed method keeps a constant
playback frame-rate under severe variations of the channel capacity,
even when short prefetch times are used.
Title: Limits on the Multi-TeV Cosmic Ray Electron Flux from CREST
(Cosmic Ray Electron Synchrotron Telescope)
Authors: Musser, J.; Bower, C.; Coutu, S.; Gennaro, J.; Geske,
M.; Müller, D.; Nutter, S.; Park, N.; Schubnell, M.; Tarlé, G.;
Wakely, S.
Bibcode: 2015ICRC...34..415M
Altcode: 2015PoS...236..415M
No abstract at ADS
Title: Prospects for High Energy Light Isotope Measurements on
Balloons
Authors: Wakely, S.; Coutu, S.; Müller, D.; Musser, J.; Nutter, S.;
Park, N. H.; Schubnel, M.; Tarlé, G.
Bibcode: 2015ICRC...34..682W
Altcode: 2015PoS...236..682W
No abstract at ADS
Title: The Helioviewer Project: Solar and Heliospheric Data
Visualization
Authors: Stys, Jeffrey E.; Ireland, Jack; Müller, Daniel
Bibcode: 2015TESS....140304S
Altcode:
Helioviewer.org enables the simultaneous exploration of multiple
heterogeneous solar and heliospheric data sets. The latest iteration
of this open-source web application brings significant visual and
functional enhancements to the user interface. Long overdue from a
usability perspective, these changes also pave the way for significant
new capabilities planned for the future. Emphasis is placed on the
solar imagery, which is now always displayed full-screen. Controls
for selecting image layers, feature and event annotations, and
observation date and time are presented in a light-weight overlay
with individually collapsible sub-sections. Secondary functions such
as movie and screenshot generation, link and image sharing, news and
community videos are now intuitively grouped and kept out of the way
until needed. Tight integration with external services such as the
Virtual Solar Observatory and SDO Cut-out Service allows scientists to
issue precisely defined requests to download science data sets via the
web, SolarSoft/IDL, and SunPy/Python after definining and previewing
them visually. Finally, documentation of the Helioviewer Public API has
been enhanced and expanded, making it simpler to integrate Helioviewer
data into scientific workflows.
Title: B.R.N.O. Contributions #39 Times of minima
Authors: Honkova, K.; Jurysek, J.; Lehky, M.; Smelcer, L.; Masek, M.;
Mazanec, J.; Hanzl, D.; Urbanik, M.; Magris, M.; Vrastak, M.; Walter,
F.; Hladik, B.; Medulka, T.; Bilek, F.; Trnka, J.; Jacobsen, J.;
Benacek, J.; Kuchtak, B.; Audejean, M.; Ogmen, Y.; Zibar, M.; Fatka,
P.; Marchi, F.; Poddany, S.; Quinones, C.; Tapia, L.; Scaggiante, F.;
Zardin, D.; Corfini, G.; Hajek, P.; Lomoz, F.; Mravik, J.; Grnja, J.;
Campos, F.; Caloud, J.; Esseiva, N.; Jaks, S.; Hornik, M.; Filip, J.;
Uhlar, R.; Mina, F.; Artola, R.; Zalazar, J.; Muller, D.; Pintr, P.;
Divisova, L.
Bibcode: 2015OEJV..168....1H
Altcode: 2016arXiv160600369H
This paper presents 1463 times of minima for 455 objects acquired
by 46 members and cooperating observers of the Variable Star and
Exoplanet Section of the Czech Astronomical Society (B.R.N.O. Observing
project). Observations were carried out between October 2013 - September
2014. Some neglected southern eclipsing binaries and newly discovered
stars by the observers of project B.R.N.O. are included in the list.
Title: Effective Gravity and Homogenous Solutions
Authors: Müller, Daniel
Bibcode: 2015mgm..conf.1856M
Altcode:
Near the singularity, gravity should be modified to an effective theory,
in the same sense as with the Euler-Heisenberg electrodynamics. This
effective gravity surmounts to higher derivative theory, and as is well
known, a much more reacher theory concerning the solution space. On the
other hand, as a highly non linear theory, the understanding of this
solution space must go beyond the linearized approach. In this talk we
will present some results previously published by collaborators and
myself, concerning solutions for vacuum spatially homogenous cases
of Bianchi types I and VIIA. These are the anisotropic
generalizations of the cosmological spatially "flat", and "open"
models respectively. The solutions present isotropisation in a weak
sense depending on the initial condition. Also, depending on the
initial condition, singular solutions are obtained.
Title: Future dynamics in theories
Authors: Müller, D.; de Andrade, V. C.; Maia, C.; Rebouças, M. J.;
Teixeira, A. F. F.
Bibcode: 2015EPJC...75...13M
Altcode: 2014arXiv1405.0768M
The gravity theories provide an alternative way to explain the
current cosmic acceleration without invoking a dark energy matter
component used in the cosmological modeling in the framework of general
relativity. However, the freedom in the choice of the functional forms
of gives rise to the problem of the degeneracy among these gravity
theories on theoretical and (or) observational grounds. In this paper
we examine the question as to whether the future dynamics can be used
to break the degeneracy between gravity theories by investigating
the dynamics of spatially homogeneous and isotropic dust flat models
in two gravity theories, namely the well-known gravity and another by
Aviles et al., whose motivation comes from the cosmographic approach to
gravity. We perform a detailed numerical study of the dynamics of these
theories taking into account the recent constraints on the cosmological
parameters made by the Planck Collaboration. We demonstrate that besides
being useful for discriminating between these two gravity theories, the
future dynamics technique can also be used to determine the finite-time
behavior as well as the fate of the Universe in the framework of these
gravity theories. There also emerges from our analysis the result
that one still can have a dust flat FLRW solution with a big rip, if
gravity is governed by . We also show that FLRW dust solutions with
do not necessarily lead to singularities.
Title: The Isotropization Process in the Quadratic Gravity
Authors: Müller, Daniel; Alves, Márcio E. S.; de Araujo, José C. N.
Bibcode: 2014IJMPD..2350019M
Altcode:
It is believed that soon after the Planck era, spacetime should have
a semi-classical nature. Therefore, it is unavoidable to modify
the theory of general relativity or look for alternative theories
of gravitation. An interesting possibility found in the literature
considers two geometric counter-terms to regularize the divergences
of the effective action. These counter-terms are responsible for
a higher-order derivative metric theory of gravitation. In the
present paper, we investigate how isotropization occurs. For this
reason a single solution is chosen throughout this paper. We obtain
perturbatively, by two different methods, that the tensor and scalar
components emerge naturally during the isotropization process. In this
sense our result provides a numerical example to Stelle's well-known
result on classical gravity with higher derivates. Our entire analysis
is restricted to the particular Bianchi type I case.
Title: 3D Visualization of Solar Data: Preparing for Solar Orbiter
and Solar Probe Plus
Authors: Mueller, D.; Felix, S.; Meier, S.; Csillaghy, A.; Nicula,
B.; Verstringe, F.; Bourgoignie, B.; Berghmans, D.; Jiggens, P.
Bibcode: 2014AGUFMSH21B4098M
Altcode:
The next generation of ESA/NASA heliophysics missions, Solar Orbiter
and Solar Probe Plus, will focus on exploring the linkage between the
Sun and the heliosphere. These new missions will collect unique data
that will allow us to study, e.g., the coupling between macroscopic
physical processes to those on kinetic scales, the generation of solar
energetic particles and their propagation into the heliosphere and
the origin and acceleration of solar wind plasma. Since 2010, NASA's
Solar Dynamics Observatory returns 1.4 TB/day of high-resolution
solar images, magnetograms and EUV irradiance data. Within a few
years, the scientific community will thus have access to petabytes of
multidimensional remotesensing and complex in-situ observations
from different vantage points, complemented by petabytes of simulation
data. Answering overarching science questions like "How do solar
transients drive heliospheric variability and space weather?" will only
be possible if the community has the necessary tools at hand. As of
today, there is an obvious lack of capability to both visualize these
data and assimilate them into sophisticated models to advance our
knowledge. A key piece needed to bridge the gap between observables,
derived quantities like magnetic field extrapolations and model output
is a tool to routinely and intuitively visualize large heterogeneous,
multidimensional, timedependent data sets. As of today, the space
science community is lacking the means to do this (i) on a routine
basis, (ii) for complex multidimensional data sets from various
instruments and vantage points and (iii) in an extensible and modular
way that is open for future improvements and interdisciplinary usage. In
this contribution, we will present recent progress in visualizing the
Sun and its magnetic field in 3D using the open-source JHelioviewer
framework, which is part of the ESA/NASA Helioviewer Project. Among
other features, JHelioviewer offers efficient region-of-interest-based
data streaming, metadata and event catalog integration, as well as an
interface to access science-quality data. In addition to its usage by
the solar physics community, JHelioviewer has already been successfully
adapted for application in planetary sciences and medical imaging.
Title: Helioviewer.org: Enhanced Solar & Heliospheric Data
Visualization
Authors: Stys, Jeffrey E.; Ireland, Jack; Hughitt, V. Keith; Mueller,
Daniel
Bibcode: 2014AAS...22421844S
Altcode:
Helioviewer.org enables the simultaneous exploration of multiple
heterogeneous solar data sets. In the latest iteration of this
open-source web application, TRACE and Hinode XRT join SDO, SOHO,
STEREO, PROBA2 SWAP, and Yohkoh SXT as supported data sets, with
significant additions to the availability of data from STEREO. Version
2 of Helioviewer's Public API for scientists and software developers
provides powerful new ways to interact with solar data, complete
with extensive documentation and usage examples. A new data coverage
visualization demystifies the availability of each data set. The
addition of a science data download tool provides a simple way to import
FITS files directly into an IDL or Python analysis environment. Finally,
a prototype timeline feature explores new ways of browsing image data
sets in our viewport as well as interacting with time series data.
Title: The NINJA-2 project: detecting and characterizing gravitational
waveforms modelled using numerical binary black hole simulations
Authors: Aasi, J.; Abbott, B. P.; Abbott, R.; Abbott, T.; Abernathy,
M. R.; Accadia, T.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.;
Addesso, P.; Adhikari, R. X.; Affeldt, C.; Agathos, M.; Aggarwal, N.;
Aguiar, O. D.; Ain, A.; Ajith, P.; Alemic, A.; Allen, B.; Allocca, A.;
Amariutei, D.; Andersen, M.; Anderson, R.; Anderson, S. B.; Anderson,
W. G.; Arai, K.; Araya, M. C.; Arceneaux, C.; Areeda, J.; Aston, S. M.;
Astone, P.; Aufmuth, P.; Aulbert, C.; Austin, L.; Aylott, B. E.; Babak,
S.; Baker, P. T.; Ballardin, G.; Ballmer, S. W.; Barayoga, J. C.;
Barbet, M.; Barish, B. C.; Barker, D.; Barone, F.; Barr, B.; Barsotti,
L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri, R.; Basti,
A.; Batch, J. C.; Bauchrowitz, J.; Bauer, Th S.; Behnke, B.; Bejger,
M.; Beker, M. G.; Belczynski, C.; Bell, A. S.; Bell, C.; Bergmann,
G.; Bersanetti, D.; Bertolini, A.; Betzwieser, J.; Beyersdorf, P. T.;
Bilenko, I. A.; Billingsley, G.; Birch, J.; Biscans, S.; Bitossi, M.;
Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair,
D.; Bloemen, S.; Blom, M.; Bock, O.; Bodiya, T. P.; Boer, M.; Bogaert,
G.; Bogan, C.; Bond, C.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork,
R.; Born, M.; Boschi, V.; Bose, Sukanta; Bosi, L.; Bradaschia, C.;
Brady, P. R.; Braginsky, V. B.; Branchesi, M.; Brau, J. E.; Briant,
T.; Bridges, D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.; Brooks,
A. F.; Brown, D. A.; Brown, D. D.; Brückner, F.; Buchman, S.; Bulik,
T.; Bulten, H. J.; Buonanno, A.; Burman, R.; Buskulic, D.; Buy, C.;
Cadonati, L.; Cagnoli, G.; Calderón Bustillo, J.; Calloni, E.; Camp,
J. B.; Campsie, P.; Cannon, K. C.; Canuel, B.; Cao, J.; Capano, C. D.;
Carbognani, F.; Carbone, L.; Caride, S.; Castiglia, A.; Caudill,
S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Celerier, C.; Cella,
G.; Cepeda, C.; Cesarini, E.; Chakraborty, R.; Chalermsongsak, T.;
Chamberlin, S. J.; Chao, S.; Charlton, P.; Chassande-Mottin, E.;
Chen, X.; Chen, Y.; Chincarini, A.; Chiummo, A.; Cho, H. S.; Chow,
J.; Christensen, N.; Chu, Q.; Chua, S. S. Y.; Chung, S.; Ciani, G.;
Clara, F.; Clark, J. A.; Cleva, F.; Coccia, E.; Cohadon, P. -F.;
Colla, A.; Collette, C.; Colombini, M.; Cominsky, L.; Constancio, M.,
Jr.; Conte, A.; Cook, D.; Corbitt, T. R.; Cordier, M.; Cornish, N.;
Corpuz, A.; Corsi, A.; Costa, C. A.; Coughlin, M. W.; Coughlin, S.;
Coulon, J. -P.; Countryman, S.; Couvares, P.; Coward, D. M.; Cowart,
M.; Coyne, D. C.; Coyne, R.; Craig, K.; Creighton, J. D. E.; Crowder,
S. G.; Cumming, A.; Cunningham, L.; Cuoco, E.; Dahl, K.; Dal Canton,
T.; Damjanic, M.; Danilishin, S. L.; D'Antonio, S.; Danzmann, K.;
Dattilo, V.; Daveloza, H.; Davier, M.; Davies, G. S.; Daw, E. J.;
Day, R.; Dayanga, T.; Debreczeni, G.; Degallaix, J.; Deléglise,
S.; Del Pozzo, W.; Denker, T.; Dent, T.; Dereli, H.; Dergachev, V.;
De Rosa, R.; DeRosa, R. T.; DeSalvo, R.; Dhurandhar, S.; Díaz, M.;
Di Fiore, L.; Di Lieto, A.; Di Palma, I.; Di Virgilio, A.; Donath,
A.; Donovan, F.; Dooley, K. L.; Doravari, S.; Dossa, S.; Douglas, R.;
Downes, T. P.; Drago, M.; Drever, R. W. P.; Driggers, J. C.; Du, Z.;
Dwyer, S.; Eberle, T.; Edo, T.; Edwards, M.; Effler, A.; Eggenstein,
H.; Ehrens, P.; Eichholz, J.; Eikenberry, S. S.; Endrőczi, G.; Essick,
R.; Etzel, T.; Evans, M.; Evans, T.; Factourovich, M.; Fafone, V.;
Fairhurst, S.; Fang, Q.; Farinon, S.; Farr, B.; Farr, W. M.; Favata,
M.; Fehrmann, H.; Fejer, M. M.; Feldbaum, D.; Feroz, F.; Ferrante,
I.; Ferrini, F.; Fidecaro, F.; Finn, L. S.; Fiori, I.; Fisher, R. P.;
Flaminio, R.; Fournier, J. -D.; Franco, S.; Frasca, S.; Frasconi, F.;
Frede, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Fritschel,
P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Gair, J.; Gammaitoni, L.;
Gaonkar, S.; Garufi, F.; Gehrels, N.; Gemme, G.; Genin, E.; Gennai,
A.; Ghosh, S.; Giaime, J. A.; Giardina, K. D.; Giazotto, A.; Gill,
C.; Gleason, J.; Goetz, E.; Goetz, R.; Gondan, L.; González, G.;
Gordon, N.; Gorodetsky, M. L.; Gossan, S.; Goßler, S.; Gouaty, R.;
Gräf, C.; Graff, P. B.; Granata, M.; Grant, A.; Gras, S.; Gray, C.;
Greenhalgh, R. J. S.; Gretarsson, A. M.; Groot, P.; Grote, H.; Grover,
K.; Grunewald, S.; Guidi, G. M.; Guido, C.; Gushwa, K.; Gustafson,
E. K.; Gustafson, R.; Hammer, D.; Hammond, G.; Hanke, M.; Hanks,
J.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.;
Harstad, E. D.; Hart, M.; Hartman, M. T.; Haster, C. -J.; Haughian,
K.; Heidmann, A.; Heintze, M.; Heitmann, H.; Hello, P.; Hemming, G.;
Hendry, M.; Heng, I. S.; Heptonstall, A. W.; Heurs, M.; Hewitson, M.;
Hild, S.; Hoak, D.; Hodge, K. A.; Holt, K.; Hooper, S.; Hopkins, P.;
Hosken, D. J.; Hough, J.; Howell, E. J.; Hu, Y.; Hughey, B.; Husa, S.;
Huttner, S. H.; Huynh, M.; Huynh-Dinh, T.; Ingram, D. R.; Inta, R.;
Isogai, T.; Ivanov, A.; Iyer, B. R.; Izumi, K.; Jacobson, M.; James,
E.; Jang, H.; Jaranowski, P.; Ji, Y.; Jiménez-Forteza, F.; Johnson,
W. W.; Jones, D. I.; Jones, R.; Jonker, R. J. G.; Ju, L.; K, Haris;
Kalmus, P.; Kalogera, V.; Kandhasamy, S.; Kang, G.; Kanner, J. B.;
Karlen, J.; Kasprzack, M.; Katsavounidis, E.; Katzman, W.; Kaufer, H.;
Kawabe, K.; Kawazoe, F.; Kéfélian, F.; Keiser, G. M.; Keitel, D.;
Kelley, D. B.; Kells, W.; Khalaidovski, A.; Khalili, F. Y.; Khazanov,
E. A.; Kim, C.; Kim, K.; Kim, N.; Kim, N. G.; Kim, Y. -M.; King, E. J.;
King, P. J.; Kinzel, D. L.; Kissel, J. S.; Klimenko, S.; Kline, J.;
Koehlenbeck, S.; Kokeyama, K.; Kondrashov, V.; Koranda, S.; Korth,
W. Z.; Kowalska, I.; Kozak, D. B.; Kremin, A.; Kringel, V.; Krishnan,
B.; Królak, A.; Kuehn, G.; Kumar, A.; Kumar, P.; Kumar, R.; Kuo,
L.; Kutynia, A.; Kwee, P.; Landry, M.; Lantz, B.; Larson, S.; Lasky,
P. D.; Lawrie, C.; Lazzarini, A.; Lazzaro, C.; Leaci, P.; Leavey, S.;
Lebigot, E. O.; Lee, C. -H.; Lee, H. K.; Lee, H. M.; Lee, J.; Leonardi,
M.; Leong, J. R.; Le Roux, A.; Leroy, N.; Letendre, N.; Levin, Y.;
Levine, B.; Lewis, J.; Li, T. G. F.; Libbrecht, K.; Libson, A.; Lin,
A. C.; Littenberg, T. B.; Litvine, V.; Lockerbie, N. A.; Lockett,
V.; Lodhia, D.; Loew, K.; Logue, J.; Lombardi, A. L.; Lorenzini, M.;
Loriette, V.; Lormand, M.; Losurdo, G.; Lough, J.; Lubinski, M. J.;
Lück, H.; Luijten, E.; Lundgren, A. P.; Lynch, R.; Ma, Y.; Macarthur,
J.; Macdonald, E. P.; MacDonald, T.; Machenschalk, B.; MacInnis,
M.; Macleod, D. M.; Magana-Sandoval, F.; Mageswaran, M.; Maglione,
C.; Mailand, K.; Majorana, E.; Maksimovic, I.; Malvezzi, V.; Man,
N.; Manca, G. M.; Mandel, I.; Mandic, V.; Mangano, V.; Mangini, N.;
Mantovani, M.; Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.;
Markosyan, A.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Martinelli, L.; Martynov, D.; Marx, J. N.; Mason, K.;
Masserot, A.; Massinger, T. J.; Matichard, F.; Matone, L.; Matzner,
R. A.; Mavalvala, N.; Mazumder, N.; Mazzolo, G.; McCarthy, R.;
McClelland, D. E.; McGuire, S. C.; McIntyre, G.; McIver, J.; McLin,
K.; Meacher, D.; Meadors, G. D.; Mehmet, M.; Meidam, J.; Meinders,
M.; Melatos, A.; Mendell, G.; Mercer, R. A.; Meshkov, S.; Messenger,
C.; Meyers, P.; Miao, H.; Michel, C.; Mikhailov, E. E.; Milano, L.;
Milde, S.; Miller, J.; Minenkov, Y.; Mingarelli, C. M. F.; Mishra, C.;
Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Moe,
B.; Moesta, P.; Mohan, M.; Mohapatra, S. R. P.; Moraru, D.; Moreno, G.;
Morgado, N.; Morriss, S. R.; Mossavi, K.; Mours, B.; Mow-Lowry, C. M.;
Mueller, C. L.; Mueller, G.; Mukherjee, S.; Mullavey, A.; Munch, J.;
Murphy, D.; Murray, P. G.; Mytidis, A.; Nagy, M. F.; Nanda Kumar, D.;
Nardecchia, I.; Naticchioni, L.; Nayak, R. K.; Necula, V.; Nelemans,
G.; Neri, I.; Neri, M.; Newton, G.; Nguyen, T.; Nitz, A.; Nocera,
F.; Nolting, D.; Normandin, M. E. N.; Nuttall, L. K.; Ochsner, E.;
O'Dell, J.; Oelker, E.; Oh, J. J.; Oh, S. H.; Ohme, F.; Oppermann,
P.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.; Ottaway, D. J.;
Ottens, R. S.; Overmier, H.; Owen, B. J.; Padilla, C.; Pai, A.;
Palashov, O.; Palomba, C.; Pan, H.; Pan, Y.; Pankow, C.; Paoletti, F.;
Paoletti, R.; Papa, M. A.; Paris, H.; Pasqualetti, A.; Passaquieti, R.;
Passuello, D.; Pedraza, M.; Penn, S.; Perreca, A.; Phelps, M.; Pichot,
M.; Pickenpack, M.; Piergiovanni, F.; Pierro, V.; Pinard, L.; Pinto,
I. M.; Pitkin, M.; Poeld, J.; Poggiani, R.; Poteomkin, A.; Powell, J.;
Prasad, J.; Premachandra, S.; Prestegard, T.; Price, L. R.; Prijatelj,
M.; Privitera, S.; Prodi, G. A.; Prokhorov, L.; Puncken, O.; Punturo,
M.; Puppo, P.; Qin, J.; Quetschke, V.; Quintero, E.; Quiroga, G.;
Quitzow-James, R.; Raab, F. J.; Rabeling, D. S.; Rácz, I.; Radkins,
H.; Raffai, P.; Raja, S.; Rajalakshmi, G.; Rakhmanov, M.; Ramet, C.;
Ramirez, K.; Rapagnani, P.; Raymond, V.; Re, V.; Read, J.; Reed,
C. M.; Regimbau, T.; Reid, S.; Reitze, D. H.; Rhoades, E.; Ricci,
F.; Riles, K.; Robertson, N. A.; Robinet, F.; Rocchi, A.; Rodruck,
M.; Rolland, L.; Rollins, J. G.; Romano, R.; Romanov, G.; Romie,
J. H.; Rosińska, D.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.;
Salemi, F.; Sammut, L.; Sandberg, V.; Sanders, J. R.; Sannibale, V.;
Santiago-Prieto, I.; Saracco, E.; Sassolas, B.; Sathyaprakash, B. S.;
Saulson, P. R.; Savage, R.; Scheuer, J.; Schilling, R.; Schnabel,
R.; Schofield, R. M. S.; Schreiber, E.; Schuette, D.; Schutz, B. F.;
Scott, J.; Scott, S. M.; Sellers, D.; Sengupta, A. S.; Sentenac, D.;
Sequino, V.; Sergeev, A.; Shaddock, D.; Shah, S.; Shahriar, M. S.;
Shaltev, M.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sidery,
T. L.; Siellez, K.; Siemens, X.; Sigg, D.; Simakov, D.; Singer, A.;
Singer, L.; Singh, R.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M.; Smith, R. J. E.; Smith-Lefebvre, N. D.;
Son, E. J.; Sorazu, B.; Souradeep, T.; Sperandio, L.; Staley, A.;
Stebbins, J.; Steinlechner, J.; Steinlechner, S.; Stephens, B. C.;
Steplewski, S.; Stevenson, S.; Stone, R.; Stops, D.; Strain, K. A.;
Straniero, N.; Strigin, S.; Sturani, R.; Stuver, A. L.; Summerscales,
T. Z.; Susmithan, S.; Sutton, P. J.; Swinkels, B.; Tacca, M.; Talukder,
D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, R.; ter Braack, A. P. M.;
Thirugnanasambandam, M. P.; Thomas, M.; Thomas, P.; Thorne, K. A.;
Thorne, K. S.; Thrane, E.; Tiwari, V.; Tokmakov, K. V.; Tomlinson,
C.; Toncelli, A.; Tonelli, M.; Torre, O.; Torres, C. V.; Torrie,
C. I.; Travasso, F.; Traylor, G.; Tse, M.; Ugolini, D.; Unnikrishnan,
C. S.; Urban, A. L.; Urbanek, K.; Vahlbruch, H.; Vajente, G.; Valdes,
G.; Vallisneri, M.; van den Brand, J. F. J.; Van Den Broeck, C.; van
der Putten, S.; van der Sluys, M. V.; van Heijningen, J.; van Veggel,
A. A.; Vass, S.; Vasúth, M.; Vaulin, R.; Vecchio, A.; Vedovato, G.;
Veitch, J.; Veitch, P. J.; Venkateswara, K.; Verkindt, D.; Verma,
S. S.; Vetrano, F.; Viceré, A.; Vincent-Finley, R.; Vinet, J. -Y.;
Vitale, S.; Vo, T.; Vocca, H.; Vorvick, C.; Vousden, W. D.; Vyachanin,
S. P.; Wade, A.; Wade, L.; Wade, M.; Walker, M.; Wallace, L.; Wang,
M.; Wang, X.; Ward, R. L.; Was, M.; Weaver, B.; Wei, L. -W.; Weinert,
M.; Weinstein, A. J.; Weiss, R.; Welborn, T.; Wen, L.; Wessels, P.;
West, M.; Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.;
White, D. J.; Whiting, B. F.; Wiesner, K.; Wilkinson, C.; Williams, K.;
Williams, L.; Williams, R.; Williams, T.; Williamson, A. R.; Willis,
J. L.; Willke, B.; Wimmer, M.; Winkler, W.; Wipf, C. C.; Wiseman,
A. G.; Wittel, H.; Woan, G.; Worden, J.; Yablon, J.; Yakushin, I.;
Yamamoto, H.; Yancey, C. C.; Yang, H.; Yang, Z.; Yoshida, S.; Yvert,
M.; Zadrożny, A.; Zanolin, M.; Zendri, J. -P.; Zhang, Fan; Zhang, L.;
Zhao, C.; Zhu, X. J.; Zucker, M. E.; Zuraw, S.; Zweizig, J.; Boyle,
M.; Brügmann, B.; Buchman, L. T.; Campanelli, M.; Chu, T.; Etienne,
Z. B.; Hannam, M.; Healy, J.; Hinder, I.; Kidder, L. E.; Laguna, P.;
Liu, Y. T.; London, L.; Lousto, C. O.; Lovelace, G.; MacDonald, I.;
Marronetti, P.; Mösta, P.; Müller, D.; Mundim, B. C.; Nakano, H.;
Paschalidis, V.; Pekowsky, L.; Pollney, D.; Pfeiffer, H. P.; Ponce, M.;
Pürrer, M.; Reifenberger, G.; Reisswig, C.; Santamaría, L.; Scheel,
M. A.; Shapiro, S. L.; Shoemaker, D.; Sopuerta, C. F.; Sperhake, U.;
Szilágyi, B.; Taylor, N. W.; Tichy, W.; Tsatsin, P.; Zlochower, Y.
Bibcode: 2014CQGra..31k5004A
Altcode: 2014arXiv1401.0939T
The Numerical INJection Analysis (NINJA) project is a
collaborative effort between members of the numerical relativity and
gravitational-wave (GW) astrophysics communities. The purpose of NINJA
is to study the ability to detect GWs emitted from merging binary
black holes (BBH) and recover their parameters with next-generation
GW observatories. We report here on the results of the second NINJA
project, NINJA-2, which employs 60 complete BBH hybrid waveforms
consisting of a numerical portion modelling the late inspiral, merger,
and ringdown stitched to a post-Newtonian portion modelling the early
inspiral. In a 'blind injection challenge' similar to that conducted
in recent Laser Interferometer Gravitational Wave Observatory (LIGO)
and Virgo science runs, we added seven hybrid waveforms to two months
of data recoloured to predictions of Advanced LIGO (aLIGO) and Advanced
Virgo (AdV) sensitivity curves during their first observing runs. The
resulting data was analysed by GW detection algorithms and 6 of the
waveforms were recovered with false alarm rates smaller than 1 in
a thousand years. Parameter-estimation algorithms were run on each
of these waveforms to explore the ability to constrain the masses,
component angular momenta and sky position of these waveforms. We find
that the strong degeneracy between the mass ratio and the BHs' angular
momenta will make it difficult to precisely estimate these parameters
with aLIGO and AdV. We also perform a large-scale Monte Carlo study
to assess the ability to recover each of the 60 hybrid waveforms with
early aLIGO and AdV sensitivity curves. Our results predict that
early aLIGO and AdV will have a volume-weighted average sensitive
distance of 300 Mpc (1 Gpc) for 10M⊙ + 10M⊙
(50M⊙ + 50M⊙) BBH coalescences. We demonstrate
that neglecting the component angular momenta in the waveform models
used in matched-filtering will result in a reduction in sensitivity
for systems with large component angular momenta. This reduction is
estimated to be up to ~15% for 50M⊙ + 50M⊙
BBH coalescences with almost maximal angular momenta aligned with the
orbit when using early aLIGO and AdV sensitivity curves.
Title: Solar Orbiter - Exploring the Sun-Heliosphere Connection
Authors: Mueller, Daniel; St Cyr, O. C.; Zouganelis, Yannis; Gilbert,
Holly R.
Bibcode: 2014cosp...40E2193M
Altcode:
Solar Orbiter, the first mission of ESA’s Cosmic Vision 2015-2025
programme, promises to deliver groundbreaking science with previously
unavailable observational capabilities provided by a suite of in-situ
and remote-sensing instruments in a unique orbit. The mission will
address the central question of heliophysics: How does the Sun create
and control the heliosphere? The heliosphere represents a uniquely
accessible domain of space, where fundamental physical processes
common to solar, astrophysical and laboratory plasmas can be studied
under conditions impossible to reproduce on Earth and unfeasible
to observe from astronomical distances. In this talk, we highlight
the scientific goals of Solar Orbiter, address the synergy between
this joint ESA/NASA mission and other new space- and ground-based
observatories, and present the mission’s development status.
Title: Quadratic gravity and cosmological solutions
Authors: Müller, D.
Bibcode: 2014GrCo...20...30M
Altcode:
No abstract at ADS
Title: Interactions of Cosmic Rays in the Atmosphere: Growth Curves
Revisited
Authors: Obermeier, A.; Boyle, P.; Hörandel, J.; Müller, D.
Bibcode: 2013ApJ...778...87O
Altcode: 2013arXiv1309.5739O
Measurements of cosmic-ray abundances on balloons are affected by
interactions in the residual atmosphere above the balloon. Corrections
for such interactions are particularly important for observations
of rare secondary particles such as boron, antiprotons, and
positrons. These corrections either can be calculated if the relevant
cross sections in the atmosphere are known or may be empirically
determined by extrapolation of the "growth curves," i.e., the individual
particle intensities as functions of atmospheric depth. The growth-curve
technique is particularly attractive for long-duration balloon flights
where the periodic daily altitude variations permit rather precise
determinations of the corresponding particle intensity variations. We
determine growth curves for nuclei from boron (Z = 5) to iron (Z =
26) using data from the 2006 Arctic balloon flight of the TRACER
detector for cosmic-ray nuclei, and we compare the growth curves with
predictions from published cross section values. In general, good
agreement is observed. We then study the boron/carbon abundance ratio
and derive a simple and energy-independent correction term for this
ratio. We emphasize that the growth-curve technique can be developed
further to provide highly accurate tests of published interaction
cross section values.
Title: JHelioviewer: Visualization software for solar physics data
Authors: Mueller, Daniel; Dimitoglou, George; Caplins, Benjamin; Garcia
Ortiz, Juan Pablo; Wamsler, Benjamin; Hughitt, Keith; Alexanderian,
Alen; Ireland, Jack; Amadigwe, Desmond; Fleck, Bernhard
Bibcode: 2013ascl.soft08016M
Altcode: 2013ascl.soft08016Y
JHelioview is open source visualization software for solar physics
data. The JHelioviewer client application enables users to browse
petabyte-scale image archives; the JHelioviewer server integrates a
JPIP server, metadata catalog, and an event server. JHelioview uses
the JPEG 2000 image compression standard, which provides efficient
access to petabyte-scale image archives; JHelioviewer also allows
users to locate and manipulate specific data sets.
Title: Effective Gravity and Homogeneous Solutions
Authors: Müller, Daniel
Bibcode: 2013arXiv1307.8438M
Altcode:
Near the singularity, gravity should be modified to an effective theory,
in the same sense as with the Euler-Heisenberg electrodynamics. This
effective gravity surmounts to higher derivative theory, and as is well
known, a much more reacher theory concerning the solution space. On the
other hand, as a highly non linear theory, the understanding of this
solution space must go beyond the linearized approach. In this talk
we will present some results previously published by collaborators
and myself, concerning solutions for vacuum spatially homogenous
cases of Bianchi types $I$ and $VII_A$. These are the anisotropic
generalizations of the cosmological spatially "flat", and "open"
models respectively. The solutions present isotropisation in a weak
sense depending on the initial condition. Also, depending on the
initial condition, singular solutions are obtained.
Title: New Capabilities in Helioviewer Project Clients
Authors: Stys, Jeffrey E.; Ireland, J.; Müller, D.; Hughitt, V. K.
Bibcode: 2013SPD....44..149S
Altcode:
Helioviewer.org enables the simultaneous exploration of multiple
heterogeneous solar data sets. In the latest iteration of this
open-source web application, Yohkoh SXT joins SDO, SOHO, STEREO,
and PROBA2 as a supported data set. A newly enhanced user-interface
expands the utility of Helioviewer.org by adding annotations to the
imagery. Backed by data from the Heliospheric Events Knowledgebase
(HEK), Helioviewer.org can now overlay solar feature and event data
(selectively by type and detection method) through the display of
interactive marker pins, region outlines, data labels, and information
panels. The addition of a size-of-the-Earth indicator provides a
sense of the scale to solar and heliospheric features for education
and public outreach purposes.
Title: Solar Orbiter . Exploring the Sun-Heliosphere Connection
Authors: Müller, D.; Marsden, R. G.; St. Cyr, O. C.; Gilbert, H. R.;
Solar Orbiter Team
Bibcode: 2013SoPh..285...25M
Altcode: 2012SoPh..tmp..193M; 2012arXiv1207.4579M
The heliosphere represents a uniquely accessible domain of space,
where fundamental physical processes common to solar, astrophysical
and laboratory plasmas can be studied under conditions impossible
to reproduce on Earth and unfeasible to observe from astronomical
distances. Solar Orbiter, the first mission of ESA's Cosmic Vision 2015
- 2025 programme, will address the central question of heliophysics:
How does the Sun create and control the heliosphere? In this paper,
we present the scientific goals of the mission and provide an overview
of the mission implementation.
Title: Solar orbiter - Close-up view of the sun
Authors: Marsden, Richard G.; Müller, Daniel; StCyr, O. Chris
Bibcode: 2013AIPC.1539..448M
Altcode:
Solar Orbiter, the first Medium-class mission of ESA's Cosmic
Vision 2015-2025 programme, is designed to study the Sun and inner
heliosphere in greater detail than ever before. At the closest point
on its heliocentric orbit, the Solar Orbiter spacecraft will be about
0.28 AU from the Sun, closer than any other satellite to date. In
addition to providing high-resolution images of the solar surface,
perihelion passes at these distances allow the instruments to track
features on the solar surface for significantly longer than from
Earth orbit. The mission profile also includes a latitude cranking
phase that will enable observations from up to 34° above the solar
equator. The combination of near-Sun and out-of-ecliptic observations
by a suite of complementary remote-sensing and in-situ instruments
makes Solar Orbiter a unique platform for studying the links between
the Sun and inner heliosphere. Planned for launch in January 2017, the
mission will be carried out in collaboration with NASA. In this paper we
present a brief overview of the mission and its scientific objectives,
and examine those areas where Solar Orbiter is expected to make major
contributions with emphasis on close-up and high-latitude observations.
Title: AlGaN/GaN-based variable gain amplifiers for W-band operation
Authors: Diebold, S.; Muller, D.; Schwantuschke, D.; Wagner, S.;
Quay, R.; Zwick, T.; Kallfass, I.
Bibcode: 2013imsd.conf97340D
Altcode:
No abstract at ADS
Title: A 0535+26 in the April 2010 outburst: probing the accretion
regime at work
Authors: Müller, D.; Klochkov, D.; Caballero, I.; Santangelo, A.
Bibcode: 2013A&A...552A..81M
Altcode: 2013arXiv1303.6068M
Context. A number of accreting X-ray pulsars experience spectral
changes, both on the long time scales and on the time scales of the
neutron star spin period. The sources seem to form two distinct
groups that differ by the type of the spectral variations with
flux. Such a bimodality probably reflects two different regimes of
accretion that may result in a particular pulsar depending on its
luminosity - so-called sub- and super-critical regimes.
Aims:
We investigated the behavior of the spectral parameters of the Be/X-ray
binary system A 0535+26, as a function of flux and pulse phase.
Methods: We used the data collected with INTEGRAL and RXTE during the
April 2010 outburst of the source. We analyzed the phase-averaged and
phase-resolved spectra and performed pulse-to-pulse spectral analysis
of the pulsar.
Results: Our analysis reveals variability in
the continuum parameters of the source's pulse-averaged spectrum
with flux. The pulse-averaged cyclotron line energy does not change
with the source luminosity during the outburst, which is consistent
with previous studies. Our pulse-phase resolved and pulse-to-pulse
analyses reveal, however, indications for a positive correlation of
the cyclotron line energy with flux, as well as a flux-dependence of
the continuum parameters. Based on the observed behavior, we argue
that A 0535+26 operates at the sub-critical accretion regime.
Title: Scientific synergy between Solar Orbiter and other new
observatories
Authors: Müller, D.; Marsden, R. G.; St. Cyr, O. C.
Bibcode: 2013MmSAI..84..396M
Altcode:
With previously unavailable observational capabilities provided by a
suite of in-situ and remote-sensing instruments in a unique orbit, the
Solar Orbiter mission promises to deliver ground-breaking science. At
the same time, its challenging 'deep space' trajectory also imposes
constraints, e.g. on the total volume of science data that can be
downlinked per orbit. This contribution highlights the science goals of
Solar Orbiter and addresses the scientific synergy between this joint
ESA/NASA mission and other new space- and ground-based observatories,
which will play a key role in maximizing the science return of Solar
Orbiter.
Title: Future science with Solar Orbiter
Authors: Marsden, Richard; Escoubet, C. Philippe; Mueller, Daniel;
St Cyr, O. C.
Bibcode: 2012cosp...39.1189M
Altcode: 2012cosp.meet.1189M
No abstract at ADS
Title: Record heavy mineral dust outbreaks over Korea
in 2010: Two cases observed with multiwavelength
aerosol/depolarization/Raman-quartz lidar
Authors: Tatarov, B.; Müller, D.; Noh, Y. -M.; Lee, K. -H.; Shin,
D. -H.; Shin, S. -K.; Sugimoto, N.; Seifert, P.; Kim, Y. -J.
Bibcode: 2012GeoRL..3914801T
Altcode:
We report on two strong events of transport of mineral dust from
Central Asia across Korea. The events took place in March and November
2010. The November case is important as fall is not a typical time
for strong dust outbreaks in East Asia. We observed the dust with
a multiwavelength aerosol/depolarization/Raman quartz lidar. The
record PM-10 concentration of nearly 1600 μg/m3 in March
2010 exceeds the record value of 1470 μg/m3 measured in
Seoul in March 2002. The event in November was the strongest case of
dust transport ever observed over Korea in fall. We find up to 360
μg/m3 dust in heights above 250 m which is significantly
different from the ground-based PM-10 observations.
Title: Bianchi V I I A solutions of effective quadratic
gravity
Authors: de Deus, Juliano A.; Müller, Daniel
Bibcode: 2012GReGr..44.1459D
Altcode: 2012GReGr.tmp...57D; 2011arXiv1103.5450D
It is believed that soon after the Planck time, Einstein's general
relativity theory should be corrected to an effective quadratic
theory. Numerical solutions for the anisotropic generalization of the
Friedmann "open" model H 3 for this effective gravity are
given. It must be emphasized that although numeric, these solutions
are exact in the sense that they depend only on the precision of the
machine. The solutions are identified asymptotically in a certain
way. It is found solutions which asymptote de Sitter space, Riemann
flat space and a singularity. The question of isotropisation of an
initially anisotropic Universe is of great importance in the context
of cosmology. Although isotropisation is not directly discussed in
this present work, we show that sufficiently small anisotropies, do
not increase indefinitely according to particular quadratic gravity
theories. It can be understood as weak isotropisation, and we stress
that this result is strongly dependent on initial conditions.
Title: The Boron-to-carbon Abundance Ratio and Galactic Propagation
of Cosmic Radiation
Authors: Obermeier, A.; Boyle, P.; Hörandel, J.; Müller, D.
Bibcode: 2012ApJ...752...69O
Altcode: 2012arXiv1204.6188O
In two long-duration balloon flights in 2003 and 2006, the TRACER
cosmic-ray detector has measured the energy spectra and the absolute
intensities of the cosmic-ray nuclei from boron (Z = 5) to iron (Z =
26) up to very high energies. In particular, the second flight has
led to results on the energy spectrum of the secondary boron nuclei,
and on the boron abundance relative to that of the heavier primary
parent nuclei, commonly quantified as the "B/C abundance ratio." The
energy dependence of this ratio, now available up to about 2 TeV
amu-1, provides a measure for the energy dependence of
cosmic-ray propagation through the Galaxy, and for the shape of the
cosmic-ray source energy spectrum. We use a Leaky-Box approximation of
cosmic-ray propagation to obtain constraints on the relevant parameters
on the basis of the results of TRACER and of other measurements. This
analysis suggests that the source energy spectrum is a relatively soft
power law in energy E -α, with spectral exponent α = 2.37
± 0.12, and that the propagation path length Λ(E) is described by
a power law in energy with exponent δ = 0.53 ± 0.06, but may assume
a constant residual value Λ0 at high energy. The value of
Λ0 is not well constrained but should be less than about
0.8 g cm-2. Finally, we compare the data with numerical
solutions of a diffusive reacceleration model, which also indicates
a soft source spectrum.
Title: The Helioviewer Project: Making Petabytes of Images Available
to Everyone
Authors: Ireland, Jack; Hughitt, V. K.; Mueller, D.
Bibcode: 2012AAS...22032301I
Altcode:
The aim of the Helioviewer Project (supported by ESA and NASA) is to
design services and clients which give users everywhere the capability
to browse and visualize the behavior of the Sun and inner heliosphere
and to give access to the underlying science data. Helioviewer Project
services and clients allow users to explore archives of JPEG2000
files and easily create movies of heliospheric events at arbitrary
times, locations, time-scales and length-scales, using images
from multiple instruments, overlaid using the FITS header information
from the original science data. Images from early 1996 to the present
day are currently available. This presentation will begin with
a short summary of the JPEG2000 standard, which is used to store a
wavelet-compressed version of the original science image data and a full
copy of the FITS header. This reduces storage requirements server-side
when compared to the original science data, but also keeps important
meta-data available for use by browse clients. The JPEG2000 standard
also includes the JPEG2000 Internet Protocol (JPIP), which allows browse
clients to efficiently stream images and dynamically assembled movies
over the web by sending only the wavelet coefficients required to show
the desired portion of the movie. These features enable efficient access
to large archives of large images, such those created by the Advanced
Imaging Assembly. Current use of Helioviewer Project services and
clients will be discussed. Plans for including images from other solar
and heliospheric data-sets will also be discussed. Finally, I will
outline the future integration of Helioviewer Project visualization
capabilities with the data provision services of the Virtual Solar
Observatory (VSO) and the solar phenomena catalog services of the
Heliophysics Event Knowledgebase (HEK), to create more scientifically
useful and integrated data search, browse and acquisition tools.
Title: Helioviewer.org: Solar and Heliospheric Data Visualization
Authors: Hughitt, V. Keith; Ireland, J.; Mueller, D.
Bibcode: 2012AAS...22020707H
Altcode:
Over the past several years, Helioviewer.org has enabled thousands
of users from across the globe to explore the inner heliosphere,
providing access to over ten million images from the SOHO, SDO, and
STEREO missions. Users can explore solar image archives, create movies
on the fly, and interact with other solar and heliospheric services
like the SDO cut-out service and the Virtual Solar Observatory
(VSO). In addition to providing a powerful platform for browsing
heterogeneous sets of solar data, Helioviewer.org also seeks to be
as flexible and extensible as possible, providing access to much
its functionality via a simple Application Programming Interface
(API). The API can be used to create images and movies from data
available on Helioviewer.org, or to embed a simplified version of
Helioviewer.org into another website. Recently the Helioviewer.org API
was used for two such applications developed by outside interests: an
SDO data browser, and a Python library for solar physics data analysis
(SunPy). These applications are discussed and examples of API usage are
provided. Finally, Helioviewer.org is undergoing continual development
with new features being added monthly. Recent changes to the web
application are discussed, along with a preview of things to come.
Title: Bianchi I Solutions of Effective Quadratic Gravity
Authors: Müller, Daniel; de Deus, Juliano A.
Bibcode: 2012IJMPD..2150037M
Altcode: 2012arXiv1203.6882M
It is believed that soon after the Planck time, Einstein's general
relativity theory should be corrected to an effective quadratic
theory. Numerical solutions for the anisotropic generalization of the
Friedmann "flat" model E3 for this effective gravity are
given. It must be emphasized that although numeric, these solutions
are exact in the sense that they depend only on the precision
of the machine. The solutions are identified asymptotically in a
certain sense. It is found solutions which asymptote de Sitter space,
Minkowski space and a singularity. This work is a generalization for
nondiagonal spatial metrics of a previous result obtained by one of
us and a collaborator for Bianchi I spaces.
Title: Analysing X-ray pulsar profiles. Geometry and beam pattern
of 4U 0115+63 and V 0332+53
Authors: Sasaki, M.; Müller, D.; Kraus, U.; Ferrigno, C.; Santangelo,
A.
Bibcode: 2012A&A...540A..35S
Altcode:
Aims: By analysing the asymmetric pulse profiles of the transient
Be/X-ray binaries 4U 0115+63 and V 0332+53 we aim to identify the origin
of the pulsed emission to understand the geometry of the accretion onto
the neutron star.
Methods: We have applied the pulse-profile
decomposition method, which enabled us to find two symmetric pulse
profiles for the two magnetic poles of the neutron star. We derived
beam patterns for different energy bands and luminosity states. This
allowed us to identify the components that are responsible for the
emission. The analysis and the models used for the interpretation of the
results take relativistic light deflection into account.
Results:
We find that the magnetic field of the neutron star is distorted in
both 4U 0115+63 and V 0332+53. The beam patterns are interpreted in
terms of a model for an accretion column that includes the formation
of a halo at the bottom of the accretion column and scattering in
the upper accretion stream.
Conclusions: In both systems,
an accretion column forms while the accretion rate is high. If the
accretion decreases and the sources become fainter, the emission from
the halo and the accretion column disappears. In 4U 0115+63 there seems
to be significant scattering of photons in the still existing accretion
stream even at the end of the outburst. In V 0332+53, the scattering in
the upper stream also disappears at the end and we apparently observe
the emission from the hot spots on the neutron star.
Title: A0535+26 during the 2010 outburst observed with INTEGRAL
and RXTE
Authors: Mueller, D.; Klochkov, D.; Caballero, I.; Staubert, R.;
Santangelo, A.
Bibcode: 2012int..workE..30M
Altcode: 2012PoS...176E..30M
No abstract at ADS
Title: Geodesic motion on closed spaces: Two numerical examples
Authors: Müller, Daniel
Bibcode: 2012PhLA..376..221M
Altcode: 2008arXiv0802.4305M
The geodesic structure is very closely related to the trace of the
Laplace operator, involved in the calculation of the expectation
value of the energy-momentum tensor in Universes with non-trivial
topology. The purpose of this work is to provide concrete numerical
examples of geodesic flows. Two manifolds with genus g=0 are given. In
one the chaotic regions, form sets of negligible or zero measure. In
the second example the geodesic flow shows the presence of measurable
chaotic regions. The approach is “experimental”, numerical, and
there is no attempt to an analytical calculation.
Title: Helioviewer.org: Simple Solar and Heliospheric Data
Visualization
Authors: Hughitt, V. K.; Ireland, J.; Mueller, D.
Bibcode: 2011AGUFMED53B0790H
Altcode:
Helioviewer.org is a free and open-source web application for
exploring solar physics data in a simple and intuitive manner. Over
the past several years, Helioviewer.org has enabled thousands of users
from across the globe to explore the inner heliosphere, providing
access to over ten million images from the SOHO, SDO, and STEREO
missions. While Helioviewer.org has seen a surge in use by the public
in recent months, it is still ultimately a science tool. The newest
version of Helioviewer.org provides access to science-quality data for
all available images through the Virtual Solar Observatory (VSO). In
addition to providing a powerful platform for browsing heterogeneous
sets of solar data, Helioviewer.org also seeks to be as flexible and
extensible as possible, providing access to much of its functionality
via a simple Application Programming Interface (API). Recently,
the Helioviewer.org API was used for two such applications: a
Wordpress plugin, and a Python library for solar physics data analysis
(SunPy). These applications are discussed and examples of API usage are
provided. Finally, Helioviewer.org is undergoing continual development,
with new features being added on a regular basis. Recent updates to
Helioviewer.org are discussed, along with a preview of things to come.
Title: Solar Orbiter: Orbital characteristics and Opportunities for
Multi-Point Observations
Authors: Mueller, D.; Marsden, R. G.; Sanchez Perez, J. M.
Bibcode: 2011AGUFMSH33B2063M
Altcode:
By means of its unique out-of-ecliptic perspective and combined
remote-sensing and in-situ instrumentation, Solar Orbiter will provide
important measurements to address the central question of heliophysics:
How does the Sun create and control the heliosphere? Combining data
from Solar Orbiter with measurements taken by other space missions,
e.g. Solar Probe Plus, and ground-based assets will open up additional
exciting scientific opportunities. To prepare for these investigations,
the orbital characteristics of all observatories involved have to be
understood in detail. In this paper, we describe the three mission
profiles that have been studied for Solar Orbiter and highlight some
of the unique opportunities for multi-point observations.
Title: No apparent accretion mode changes detected in Centaurus X-3
Authors: Müller, D.; Klochkov, D.; Santangelo, A.; Mihara, T.;
Sugizaki, M.
Bibcode: 2011A&A...535A.102M
Altcode: 2011arXiv1111.0438M
Aims: Two distinct spectral states have previously been reported
for Cen X-3 on the basis of RXTE/ASM observations. Intrigued by this
result, we investigated the spectral properties of the source using
the enhanced possibilities of the X-ray data now available with the
aim to clarify and interpret the reported behavior.
Methods: To
check the reported results, we used the same data set and followed the
same analysis procedures as in the work that reported the two spectral
states. Additionally, we repeated the analysis using the enlarged
data sample including the newest RXTE/ASM observations as well as
the data from the MAXI monitor and from the INTEGRAL/JEM-X and ISGRI
instruments.
Results: We were unable to confirm the reported
presence of the two spectral states in Cen X-3 either in the RXTE/ASM
data or in the MAXI or INTEGRAL data. Our analysis shows that the flux
variations in different energy bands are consistent with a spectral
hardness that is constant over the entire time covered by observations.
Title: Energy Spectra of Primary and Secondary Cosmic-Ray Nuclei
Measured with TRACER
Authors: Obermeier, A.; Ave, M.; Boyle, P.; Höppner, Ch.; Hörandel,
J.; Müller, D.
Bibcode: 2011ApJ...742...14O
Altcode: 2011arXiv1108.4838O
The Transition Radiation Array for Cosmic Energetic Radiation (TRACER)
cosmic-ray detector, first flown on long-duration balloon (LDB) in 2003
for observations of the major primary cosmic-ray nuclei from oxygen (Z =
8) to iron (Z = 26), has been upgraded to also measure the energies of
the lighter nuclei, including the secondary species boron (Z = 5). The
instrument was used in another LDB flight in 2006. The properties and
performance of the modified detector system are described, and the
analysis of the data from the 2006 flight is discussed. The energy
spectra of the primary nuclei carbon (Z = 6), oxygen, and iron over
the range from 1 GeV amu-1 to 2 TeV amu-1 are
reported. The data for oxygen and iron are found to be in good agreement
with the results of the previous TRACER flight. The measurement of the
energy spectrum of boron also extends into the TeV amu-1
region. The relative abundances of the primary nuclei, such as carbon,
oxygen, and iron, above ~10 GeV amu-1 are independent of
energy, while the boron abundance, i.e., the B/C abundance ratio,
decreases with energy as expected. However, there is an indication
that the previously reported E -0.6 dependence of the B/C
ratio does not continue to the highest energies.
Title: Measurement of Cosmic-Ray TeV Electrons
Authors: Schubnell, Michael; Anderson, T.; Bower, C.; Coutu, S.;
Gennaro, J.; Geske, M.; Mueller, D.; Musser, J.; Nutter, S.; Park,
N.; Tarle, G.; Wakely, S.
Bibcode: 2011HEAD...12.3616S
Altcode:
The Cosmic Ray Electron Synchrotron Telescope (CREST) high-altitude
balloon experiment is a pathfinding effort to detect for the first
time multi-TeV cosmic-ray electrons. At these energies distant sources
will not contribute to the local electron spectrum due to the strong
energy losses of the electrons and thus TeV observations will reflect
the distribution and abundance of nearby acceleration sites. CREST will
detect electrons indirectly by measuring the characteristic synchrotron
photons generated in the Earth's magnetic field. The instrument consist
of an array of 1024 BaF2 crystals viewed by photomultiplier tubes
surrounded by a hermetic scintillator shield. Since the primary electron
itself need not traverse the payload, an effective detection area is
achieved that is several times the nominal 6.4 m2 instrument. CREST is
scheduled to fly in a long duration circumpolar orbit over Antarctica
during the 2011-12 season.
Title: The Be/X-ray binary A0535+26 during its recent 2009/2010
outbursts
Authors: Caballero, I.; Pottschmidt, K.; Santangelo, A.; Barragan, L.;
Klochkov, D.; Ferrigno, C.; Rodriguez, J.; Kretschmar, P.; Suchy, S.;
Marcu, D. M.; Mueller, D.; Wilms, J.; Kreykenbohm, I.; Rothschild,
R. E.; Staubert, R.; Finger, M. H.; Camero-Arranz, A.; Makishima,
K.; Mihara, T.; Nakajima, M.; Enoto, T.; Iwakiri, W.; Terada, Y.
Bibcode: 2011arXiv1107.3417C
Altcode:
The Be/X-ray binary A0535+26 showed a giant outburst in December 2009
that reached ~5.14 Crab in the 15-50 keV range. Unfortunately, due to
Sun constraints it could not be observed by most X-ray satellites. The
outburst was preceded by four weaker outbursts associated with the
periastron passage of the neutron star. The fourth of them, in August
2009, presented a peculiar double-peaked light curve, with a first peak
lasting about 9 days that reached a (15-50 keV) flux of 440 mCrab. The
flux then decreased to less than 220 mCrab, and increased again
reaching 440 Crab around the periastron. The outburst was monitored
with INTEGRAL, RXTE, and Suzaku TOO observations. One orbital period
(~111 days) after the 2009 giant outburst, a new and unexpectedly bright
outburst took place (~1.4Crab in the 15-50 keV range). It was monitored
with TOO obs ervations with INTEGRAL, RXTE, Suzaku, and Swift. First
results of the spectral and timing analysis of these observations are
presented, with a specific focus on the cyclotron lines present in
the system and its variation with the mass accretion rate.
Title: 11-orbit inspiral of a mass ratio 4:1 black-hole binary
Authors: Sperhake, U.; Brügmann, B.; Müller, D.; Sopuerta, C. F.
Bibcode: 2011CQGra..28m4004S
Altcode:
We analyse an 11-orbit inspiral of a non-spinning black-hole binary
with mass ratio q ≡ M1/M2 = 4. The numerically
obtained gravitational waveforms are compared with post-Newtonian
(PN) predictions including several subdominant multipoles up to
multipolar indices (l = 5, m = 5). We find that (i) numerical and
post-Newtonian predictions of the phase of the (2, 2) mode accumulate
a phase difference of about 0.35 rad at the PN cut-off frequency Mω =
0.1 for the Taylor T1 approximant when numerical and PN waveforms are
matched over a window in the early inspiral phase; (ii) in contrast to
previous studies of equal mass and specific spinning binaries, we find
the Taylor T4 approximant to agree less well with numerical results,
provided the latter are extrapolated to infinite extraction radius;
(iii) extrapolation of gravitational waveforms to infinite extraction
radius is particularly important for subdominant multipoles with l ≠
m; (iv) 3PN terms in post-Newtonian multipole expansions significantly
improve the agreement with numerical predictions for subdominant
multipoles.
Title: Homogeneous Solutions of Quadratic Gravity
Authors: Müller, Daniel
Bibcode: 2011IJMPS...3..111M
Altcode: 2011arXiv1107.3570M; 2011IJMPS..03..111M
It is believed that soon after the Planck time, Einstein's general
relativity theory should be corrected to an effective quadratic
theory. In this work we present the 3 + 1 decomposition for the zero
vorticity case for arbitrary spatially homogenous spaces. We specialize
for the particular Bianchi I diagonal case. The 3- curvature can be
understood as a generalized potential, and the Bianchi I case is a
limiting case where this potential is negligible to the dynamics. The
spirit should be analogous, in some sense to the BKL solution. In this
sense, a better understanding of the Bianchi I case could shed some
light into the general Bianchi case.
Title: Inspiral-Merger-Ringdown Waveforms for Black-Hole Binaries
with Nonprecessing Spins
Authors: Ajith, P.; Hannam, M.; Husa, S.; Chen, Y.; Brügmann,
B.; Dorband, N.; Müller, D.; Ohme, F.; Pollney, D.; Reisswig, C.;
Santamaría, L.; Seiler, J.
Bibcode: 2011PhRvL.106x1101A
Altcode: 2009arXiv0909.2867A
We present the first analytical inspiral-merger-ringdown gravitational
waveforms from binary black holes (BBHs) with nonprecessing spins, that
is based on a description of the late-inspiral, merger and ringdown
in full general relativity. By matching a post-Newtonian description
of the inspiral to a set of numerical-relativity simulations,
we obtain a waveform family with a conveniently small number of
physical parameters. These waveforms will allow us to detect a larger
parameter space of BBH coalescence, including a considerable fraction
of precessing binaries in the comparable-mass regime, thus significantly
improving the expected detection rates.
Title: Searching for TeV cosmic electrons with the CREST experiment
Authors: Coutu, S.; Anderson, T.; Bower, C.; Gennaro, J.; Geske,
M.; Müller, D.; Musser, J.; Nutter, S.; Park, N. H.; Schubnell, M.;
Tarlé, G.; Wakely, S.; Yagi, A.
Bibcode: 2011NuPhS.215..250C
Altcode:
The Cosmic Ray Electron Synchrotron Telescope (CREST) high-altitude
balloon experiment is a pathfinding effort to detect for the first
time multi-TeV cosmic-ray electrons. Such would be the markers
of nearby cosmic accelerators, as energetic electrons from distant
Galactic sources are expected to be depleted by radiative losses during
interstellar transport. Electrons will be detected indirectly by the
characteristic signature of their geomagnetic synchrotron losses,
in the form of a burst of coaligned x-ray photons intersecting the
plane of the instrument. Since the primary electron itself need not
traverse the payload, an effective detection area is achieved that is
several times the nominal 6.4 m2 instrument. The payload is
composed of an array of 1024 BaF2 crystals surrounded by a set of veto
scintillator detectors. A long-duration balloon flight in Antarctica
is planned for the 2011-12 season.
Title: The Helioviewer Project: Solar Data Visualization and
Exploration
Authors: Hughitt, V. Keith; Ireland, J.; Müller, D.; García Ortiz,
J.; Dimitoglou, G.; Fleck, B.
Bibcode: 2011SPD....42.1517H
Altcode: 2011BAAS..43S.1517H
SDO has only been operating a little over a year, but in that short
time it has already transmitted hundreds of terabytes of data, making
it impossible for data providers to maintain a complete archive of
data online. By storing an extremely efficiently compressed subset of
the data, however, the Helioviewer project has been able to maintain a
continuous record of high-quality SDO images starting from soon after
the commissioning phase. The Helioviewer project was not designed
to deal with SDO alone, however, and continues to add support for
new types of data, the most recent of which are STEREO EUVI and
COR1/COR2 images. In addition to adding support for new types of data,
improvements have been made to both the server-side and client-side
products that are part of the project. A new open-source JPEG2000 (JPIP)
streaming server has been developed offering a vastly more flexible and
reliable backend for the Java/OpenGL application JHelioviewer. Meanwhile
the web front-end, Helioviewer.org, has also made great strides both
in improving reliability, and also in adding new features such as the
ability to create and share movies on YouTube. Helioviewer users are
creating nearly two thousand movies a day from the over six million
images that are available to them, and that number continues to grow
each day. We provide an overview of recent progress with the various
Helioviewer Project components and discuss plans for future development.
Title: Accessing SDO Data : The Poster
Authors: Hourcle, Joseph; Addison, K.; Bogart, R.; Chamberlin, P.;
Freeland, S.; Hughitt, V. K.; Ireland, J.; Maddox, M.; Mueller, D.;
Somani, A.; Sommers, J.; Thompson, B.; solar physics data community,
The
Bibcode: 2011SPD....42.2130H
Altcode: 2011BAAS..43S.2130H
As the data from SDO are useful for a variety of purposes, including
solar physics, helioseismology, atmospheric science, space weather
forecasting, education and public outreach, a wide variety of tools
have been development to cater to the different needs of the various
groups. Systems have been developed for pipeline processing, searching,
browsing, subsetting, or simply just moving around large volumes
of data. We present a quick overview of the different systems
that can be used to access SDO data including (J)Helioviewer, the
Heliophysics Event Knowledgebase (HEK), the Virtual Solar Observatory
(VSO), the Integrated Space Weather Analysis System (iSWA), the
Data Record Management System (DRMS), and various websites. We cover
web-based applications, application programming interfaces (APIs),
and IDL command line tools. This poster serves as a supplement
to the oral presentation as a place to distribute information about
the various interfaces and to collect feedback about any unmet needs
for data access.
Title: Isotropisation of Quadratic Gravity: Scalar and Tensor
Components
Authors: Müller, Daniel; Alves, Márcio E. S.; de Araujo, José C. N.
Bibcode: 2011arXiv1103.3439M
Altcode:
It is believed that soon after the Planck era, spacetime should have
a semi-classical nature. Therefore, it is unavoidable to modify
the theory of General Relativity or look for alternative theories
of gravitation. An interesting possibility found in the literature
considers two geometric counter-terms to regularize the divergences of
the effective action. These counter-terms are responsible for a higher
order derivative metric theory of gravitation. In the present letter
we investigate how isotropisation occurs. For this reason a single
solution is chosen throughout this article. We obtain perturbatively,
by two different methods, that the tensor and scalar components emerge
naturally during the isotropisation process. In this sense our result
provides a numerical example to Stelle's well known result on classical
gravity with higher derivates. Our entire analysis is restricted to
the particular Bianchi type $I$ case.
Title: Optical and microphysical properties of fresh biomass burning
aerosol retrieved by Raman lidar, and star-and sun-photometry
Authors: Alados-Arboledas, L.; Müller, D.; Guerrero-Rascado, J. L.;
Navas-Guzmán, F.; Pérez-Ramírez, D.; Olmo, F. J.
Bibcode: 2011GeoRL..38.1807A
Altcode: 2011GeoRL..3801807A
A fresh biomass-burning pollution plume was monitored and characterized
in terms of optical and microphysical properties for the first time
with a combination of Raman lidar and star- and sun-photometers. Such
an instrument combination is highly useful for 24-h monitoring of
pollution events. The observations were made at Granada (37.16°N,
3.6°W), Spain. The fresh smoke particles show a rather pronounced
accumulation mode and features markedly different from those reported
for aged particles. We find lidar ratios around 60-65 sr at 355 nm and
532 nm, and particle effective radii below 0.20 μm. We find low values
of the single-scattering albedo of 0.76-0.9 depending on measurement
wavelength. The numbers are lower than what have been found for aged,
long-range-transported smoke that originated from boreal fires in
Canada and Siberia.
Title: Solar Orbiter: Linking the Sun and Inner Heliosphere
Authors: Marsden, Richard G.; Müller, Daniel
Bibcode: 2011sswh.book..347M
Altcode:
No abstract at ADS
Title: Helioviewer: Simplifying Your Access to SDO Data
Authors: Hughitt, V. K.; Ireland, J.; Mueller, D.; Beck, J.; Lyon,
D.; Dau, A.; Dietert, H.; Nuhn, M.; Dimitoglou, G.; Fleck, B.
Bibcode: 2010AGUFMSH23C1868H
Altcode:
Over the past several years, the Helioviewer Project has evolved
from a simple web application to display images of the sun into a
suite of tools to visualize and interact with heterogeneous types of
solar data. In addition to a modular and scalable back-end server, the
Helioviewer Project now offers multiple browse clients; the original
web application has been upgraded to support high-definition movie
generation and feature and event overlays. For complex image processing
and massive data volumes, there is a stand-alone desktop application,
JHelioviewer. For a quick check of the latest images and events,
there is an iPhone application, hqTouch. The project has expanded from
the original SOHO images to include image data from SDO and event and
feature data from the HEK. We are working on adding additional image
data from other missions as well as spectral and time-series data. We
will discuss the procedure through which interested parties may process
their data for use with Helioviewer, including how to use JP2Gen to
convert FITS files into Helioviewer-compliant JPEG 2000 images, how
to setup a local instance of the Helioviewer server, and how to query
Helioviewer in your own applications using a simple web API.
Title: The Many Ways to Access SDO Data
Authors: Thompson, B. J.; Hourcle, J. A.; Addison, K.; Bogart, R. S.;
Chamberlin, P. C.; Dietert, H.; Freeland, S. L.; Hughitt, V. K.;
Ireland, J.; Mueller, D.; Somani, A.; Sommers, J.
Bibcode: 2010AGUFMSH23C1865T
Altcode:
To solve the issue of dealing with the large volume of data available
from AIA, there are a number of ways to get access to SDO data. With
Helioviewer, the Heliophysics Event Knowledgebase, the Virtual Solar
Observatory, and the PI-provided tools, scientists and other interested
parties have a number of ways to find and obtain data of interest. We
present an overview of the differences between the various systems,
and a flow chart to help determine which one might be of the most
benefit for a given situation.
Title: JHelioviewer: Open-Source Software for Discovery and Image
Access in the Petabyte Age (Invited)
Authors: Mueller, D.; Dimitoglou, G.; Langenberg, M.; Pagel, S.; Dau,
A.; Nuhn, M.; Garcia Ortiz, J. P.; Dietert, H.; Schmidt, L.; Hughitt,
V. K.; Ireland, J.; Fleck, B.
Bibcode: 2010AGUFMSH22A..05M
Altcode:
The unprecedented torrent of data returned by the Solar Dynamics
Observatory is both a blessing and a barrier: a blessing for making
available data with significantly higher spatial and temporal
resolution, but a barrier for scientists to access, browse and
analyze them. With such staggering data volume, the data is bound
to be accessible only from a few repositories and users will have to
deal with data sets effectively immobile and practically difficult to
download. From a scientist's perspective this poses three challenges:
accessing, browsing and finding interesting data while avoiding
the proverbial search for a needle in a haystack. To address
these challenges, we have developed JHelioviewer, an open-source
visualization software that lets users browse large data volumes
both as still images and movies. We did so by deploying an efficient
image encoding, storage, and dissemination solution using the JPEG
2000 standard. This solution enables users to access remote images at
different resolution levels as a single data stream. Users can view,
manipulate, pan, zoom, and overlay JPEG 2000 compressed data quickly,
without severe network bandwidth penalties. Besides viewing data, the
browser provides third-party metadata and event catalog integration
to quickly locate data of interest, as well as an interface to the
Virtual Solar Observatory to download science-quality data. As part of
the Helioviewer Project, JHelioviewer offers intuitive ways to browse
large amounts of heterogeneous data remotely and provides an extensible
and customizable open-source platform for the scientific community.
Title: Mineral quartz concentration measurements of mixed mineral
dust/urban haze pollution plumes over Korea with multiwavelength
aerosol Raman-quartz lidar
Authors: Müller, D.; Mattis, I.; Tatarov, B.; Noh, Y. M.; Shin,
D. H.; Shin, S. K.; Lee, K. H.; Kim, Y. J.; Sugimoto, N.
Bibcode: 2010GeoRL..3720810M
Altcode:
We present a case study of a concentration measurement of mineral quartz
immersed in East Asian urban pollution. We use a novel lidar measurement
technique that uses signals from Raman scattering from quartz at
ultraviolet (360 nm) wavelength. The particle-extinction-related
Ångström exponent (wavelength pair 355/532 nm) varies around 0.7 ±
0.2 , the lidar ratio is 50-55 sr at 532 nm. The numbers indicate that
the pollution plume likely consisted of a mixture of mineral dust with
urban haze. Dust concentrations vary between 8-11 μg/cm3. We
determined Raman quartz concentrations from measurements simultaneously
carried out at 546 nm, which allows us to measure for the first time
the Raman-quartz-related Ångström exponent of mineral dust. Values
are 3-4, whereas we expect a theoretical value of 4. It is unclear if
the lower values follow from retrieval uncertainties or if they are
linked to the internal structure of the quartz grains.
Title: The 16 April 2010 major volcanic ash plume over central Europe:
EARLINET lidar and AERONET photometer observations at Leipzig and
Munich, Germany
Authors: Ansmann, A.; Tesche, M.; Groß, S.; Freudenthaler, V.;
Seifert, P.; Hiebsch, A.; Schmidt, J.; Wandinger, U.; Mattis, I.;
Müller, D.; Wiegner, M.
Bibcode: 2010GeoRL..3713810A
Altcode:
The optically thickest volcanic ash plume ever measured over Germany
was monitored with multiwavelength Raman lidars and Sun photometer
at Leipzig and Munich. When this ash layer, originating from the
Eyjafjoll eruptions in southern Iceland, crossed Leipzig between 2.5
and 6 km height on 16 April 2010, the total 500 nm aerosol optical
depth reached 1.0, and the ash-related optical depth was about
0.7. Volume light-extinction coefficients (40-75-minute mean values)
measured over Leipzig and Munich at 355 and 532 nm reached values
of 400-600 Mm-1 and ash mass concentrations were on the
order of 1000 ± 350 μg/m3 in the center of the main ash
layer. Extinction-to-backscatter ratios ranged from 55 ± 5 sr (Munich)
to 60 ± 5 sr (Leipzig) in the main ash layer, and the particle linear
depolarization ratio was close to 0.35 at both wavelengths. Rather low
photometer-derived Ångström exponents (500-1640 nm wavelength range)
indicated the presence of a significant amount of large ash particles
with diameters >20 μm.
Title: JHelioviewer: Taming The Torrent Of SDO Data
Authors: Mueller, Daniel; Langenberg, M.; Pagel, S.; Schmidt, L.;
Garcia Ortiz, J. P.; Dimitoglou, G.; Hughitt, V. K.; Ireland, J.;
Fleck, B.
Bibcode: 2010AAS...21640224M
Altcode: 2010BAAS...41..877M
Space missions generate an ever-growing amount of data, as impressively
highlighted by the Solar Dynamics Observatory's (SDO) expected return
of 1.4 TByte/day. In order to fully exploit their data, scientists
need to be able to browse and visualize many different data products
spanning a large range of physical length and time scales. So far, the
tools available to the scientific community either require downloading
all potentially relevant data sets beforehand in their entirety or
provide only movies with a fixed resolution and cadence. For SDO,
the former approach is prohibitive due to the shear data volume, while
the latter does not do justice to the high resolution and cadence of
the images. To address this challenge, we have developed JHelioviewer,
a JPEG 2000-based visualization and discovery software for solar image
data. Using the very efficient lossy compression mode of JPEG 2000,
a full-size SDO image can be compressed to 1 MByte at good visual
quality for browsing purposes. JHelioviewer will make the vast amount
of SDO images available to the worldwide community in this format,
which is already being used for all SOHO images. JHelioviewer is
a cross-platform application that offers movie streaming, real-time
frame-by-frame image processing, feature/event overlays and will enable
users to access SDO science data via a VSO interface. JHelioviewer uses
the JPEG 2000 Interactive Protocol (JPIP) and OpenGL. The random code
stream access of JPIP minimizes data transfer by streaming image data in
a region-of-interest and quality-progressive way, while OpenGL enables
rapid hardware-accelerated image processing and rendering. Currently
focused on solar physics data, JHelioviewer can easily be adapted
for use in other areas of space and earth sciences. This poster will
illustrate the new and expanded functionality of JHelioviewer and
highlight the advantages of JPEG 2000 as a new compression standard
for solar image data.
Title: The Helioviewer Project: Browsing, Visualizing and Accessing
Petabytes of Solar Data
Authors: Mueller, Daniel; Hughitt, V. K.; Langenberg, M.; Ireland, J.;
Pagel, S.; Schmidt, L.; Garcia Ortiz, J. P.; Dimitoglou, G.; Fleck, B.
Bibcode: 2010AAS...21640223M
Altcode: 2010BAAS...41..876M
After its successful launch, NASA's Solar Dynamics Observatory
(SDO) will soon return more than 1 Terabyte worth of images per
day. This unprecedented torrent of data will pose an entirely new
set of challenges with respect to data access, data browsing and
searching for interesting data while avoiding the proverbial search
for "a needle in a haystack". In order to fully exploit SDO's wealth
of data and connect it to data from other solar missions like SOHO,
scientists need to be able to interactively browse and visualize many
different data products spanning a large range of physical length and
time scales. So far, all tools available to the scientific community
either require downloading all potentially relevant data sets beforehand
in their entirety or provide only movies with a fixed resolution and
cadence. The Helioviewer project offers a solution to these challenges
by providing a suite of tools that are based on the new JPEG 2000
compression standard and enable scientists and the general public alike
to intuitively browse visualize and access petabytes of image data
remotely: - JHelioviewer, a cross-platform application that offers
movie streaming and real-time processing using the JPEG 2000 Interactive
Protocol (JPIP) and OpenGL, as well as feature/event overlays. -
helioviewer.org, a web-based image and feature/event browser. -
Server-side services to stream movies of arbitrary spatial and temporal
resolution in a region-of-interest and quality-progressive form, a
JPEG 2000 image database and a feature/event server. All the services
can be accessed through well-documented interfaces (APIs). - Code
to convert images into JPEG 2000 format. This presentation will
give an overview of the Helioviewer Project, illustrate new features
and highlight the advantages of JPEG 2000 as a data format for solar
physics that has the potential to revolutionize the way high-resolution
image data are disseminated and analyzed.
Title: Size matters: Influence of multiple scattering on CALIPSO
light-extinction profiling in desert dust
Authors: Wandinger, U.; Tesche, M.; Seifert, P.; Ansmann, A.; Müller,
D.; Althausen, D.
Bibcode: 2010GeoRL..3710801W
Altcode:
We investigate the discrepancies in measurements of light extinction
and extinction-to-backsatter ratio (lidar ratio) of desert dust with
CALIPSO and ground-based lidar systems. Multiwavelength polarization
Raman lidar measurements in the Saharan dust plume performed at
Praia, Cape Verde, 15.0°N, 23.5°W, during SAMUM-2 in June 2008 were
analyzed and compared to results of nearby CALIPSO overflights. The
particle extinction coefficients and thus the optical depth are
underestimated in the CALIPSO products by about 30% compared to Raman
lidar measurements. A pre-defined lidar ratio of 40 sr at 532 nm is
used for mineral dust in the CALIPSO algorithms in agreement with
values of 41 ± 6 sr found from constrained retrievals. However, the
ground-based lidar observations show much larger values of the order
of 55 ± 10 sr. The discrepancies can be explained by the influence of
multiple scattering which is ignored in the CALIPSO retrievals. Based
on recent observations of the size distribution of dust particles from
airborne in-situ observations during SAMUM-1, our model calculations
show that the multiple-scattering-related underestimation of the
extinction coefficient in the CALIPSO lidar signals ranges from
10%-40%. We propose a method to overcome this underestimation.
Title: Solar Mashups: Interacting With, Extending, And Embedding
Helioviewer.org And Jhelioviewer
Authors: Hughitt, V. Keith; Ireland, J.; Müller, D.; Langenberg,
M.; Pagel, S.; Schmidt, L.; Harper, J.; Dimitoglou, G.; Fleck, B.
Bibcode: 2010AAS...21640225H
Altcode: 2010BAAS...41..877H
Helioviewer.org is a JPEG 2000-driven web application for searching
and displaying heterogeneous solar data sets, including both image
and catalog information. Helioviewer.org has been written from the
ground up with extensibility in mind. The result of this effort is a
rich Application Programming Interface (API) from which third-party
applications can interact with Helioviewer.org. In addition to being
able to launch Helioviewer.org with a specified state (by giving
it a time and a set of instruments, wavelengths, etc), it is also
possible to generate composite images and movies, and to search for
catalog data from the Heliophysics Event Knowledgebase (HEK). We are
developing our software so that you will be able to embed instances
of Helioviewer.org in your own web pages, in much the same way that
it is now possible to embed Google Maps (tm) into any webpage. This
will make it very easy to overlay your data with that provided by
the Helioviewer Project. JHelioviewer, Helioviewer.org's Java-based
counterpart, shares many of the same features as Helioviewer.org, but
also offers some new ones when it comes to extensibility, including a
custom plugin architecture that supports custom image filters, overlay
layers, GUI components, and more. Both of the projects are free to
use and completely open-source, and anyone is welcome to contribute
to their development.
Title: TeV electron measurement with CREST experiment
Authors: Park, Nahee; Anderson, T.; Bower, C.; Coutu, S.; Gennaro,
J.; Geske, M.; Muller, D.; Musser, J.; Nutter, S.
Bibcode: 2010cosp...38.2657P
Altcode: 2010cosp.meet.2657P
CREST, the Cosmic Ray Electron Synchrotron Telescope is a balloon-borne
experiment de-signed to measure the spectrum of multi-TeV electrons
by the detection of the x-ray synchrotron photons generated in the
magnetic field of the Earth. Electrons in the TeV range are expected
to reflect the properties of local sources because fluxes from remote
locations are suppressed by radiative losses during propagation. Since
CREST needs to intersect only a portion of the kilometers-long trail
of photons generated by the high-energy electron, the method yields
a larger effective area than the physical size of the detector,
boosting detection areas. The in-strument is composed of an array of
1024 BaF2 crystals and a set of scintillating veto counters. A long
duration balloon flight in Antarctica is currently planned for the
2010-11 season.
Title: The Be/X-ray binary A0535+26 during its recent 2009/2010
outbursts
Authors: Caballero, I.; Pottschmidt, K.; Santangelo, A.; Barragán,
L.; Klochkov, D.; Ferrigno, C.; Rodriguez, J.; Kretschmr, P.; Suchy,
S.; Marcu, D. M.; Müller, D.; Wilms, J.; Kreykenbohm, I.; Rothschild,
R. E.; Staubert, R.; Finger, M. H.; Camero-Arranz, A.; Makishima,
K.; Mihara, T.; Nakajima, M.; Enoto, T.; Iwakiri, W.; Terada, Y.
Bibcode: 2010int..workE..63C
Altcode: 2010PoS...115E..63C
No abstract at ADS
Title: JHelioviewer: Exploring Petabytes of Solar Images
Authors: Mueller, Daniel; Fleck, Bernhard; Dimitoglou, George; Garcia
Ortiz, Juan Pablo; Schmidt, Ludwig; Hughitt, Keith; Ireland, Jack
Bibcode: 2010cosp...38.2880M
Altcode: 2010cosp.meet.2880M
Space missions generate an ever-growing amount of data, as impressively
highlighted by the Solar Dynamics Observatory's (SDO) expected return
of 1.4 TByte/day. In order to fully ex-ploit their data, scientists
need to be able to browse and visualize many different data products
spanning a large range of physical length and time scales. So far, the
tools available to the scientific community either require downloading
all potentially relevant data sets beforehand in their entirety or
provide only movies with a fixed resolution and cadence. For SDO,
the former approach is prohibitive due to the shear data volume,
while the latter does not do justice to the high resolution and
cadence of the images. To address this challenge, we have developed
JHelioviewer, a JPEG 2000-based visualization and discovery software
for solar image data. JHelioviewer makes the vast amount of SDO images
available to the worldwide community, lets users browse more than
14 years worth of images from the Solar and Heliospheric Observatory
(SOHO) and facilitates browsing and analysis of complex time-dependent
data sets from mul-tiple sources in general. The user interface for
JHelioviewer is a multi-platform Java client that communicates with a
remote server via the JPEG 2000 interactive protocol JPIP. The random
code stream access of JPIP minimizes data transfer and can encapsulate
metadata as well as multiple image channels in one data stream. This
presentation will illustrate the features of JHelioviewer and highlight
the advantages of JPEG 2000 as a new data compression standard.
Title: On the Relationship Between Magnetic Field and Mesogranulation
Authors: de Wijn, A. G.; Müller, D.
Bibcode: 2009ASPC..415..211D
Altcode: 2009arXiv0902.1967D
We investigate the relation between Trees of Fragmenting Granules
(TFGs) and the locations of concentrated magnetic flux in
internetwork areas. The former have previously been identified with
mesogranulation. While a relationship has been suggested to exist
between these features, no direct evidence has yet been provided. We
present some preliminary results that show that concentrated magnetic
flux indeed collects on the borders of TFGs.
Title: Solar Orbiter: Exploring the Sun-Heliosphere Connection
Authors: Marsden, R. G.; Mueller, D.
Bibcode: 2009AGUFMSH13B1537M
Altcode:
Understanding the connections and the coupling between the Sun and
the heliosphere is of fundamental importance to addressing one of the
major scientific questions of ESA’s Cosmic Vision 2020 programme:
“How does the Solar System work?” The heliosphere also represents
a uniquely accessible domain of space, where fundamental physical
processes common to solar, astrophysical and laboratory plasmas
can be studied under conditions impossible to reproduce on Earth,
or to study from astronomical distances. The results from missions
such as Helios, Ulysses, Yohkoh, SOHO, TRACE and RHESSI, as well as
the recently launched Hinode and STEREO missions, have formed the
foundation of our understanding of the solar corona, the solar wind,
and the three-dimensional heliosphere. Each of these missions had
a specific focus, being part of an overall strategy of coordinated
solar and heliospheric research. However, an important element of this
strategy has yet to be implemented. None of these missions have been
able to fully explore the interface region where the solar wind is born
and heliospheric structures are formed with sufficient instrumentation
to link solar wind structures back to their source regions at the
Sun. This is the overarching goal of Solar Orbiter. With previously
unavailable observational capabilities provided by the powerful
combination of in-situ and remote sensing instruments, and the unique
inner-heliospheric mission design specifically tailored for the task,
Solar Orbiter will address the central question of heliophysics:
How does the Sun create and control the heliosphere? In this paper,
we will present the detailed science goals of the mission and briefly
review its status.
Title: Helioviewer.org: Browsing Very Large Image Archives Online
Using JPEG 2000
Authors: Hughitt, V. K.; Ireland, J.; Mueller, D.; Dimitoglou, G.;
Garcia Ortiz, J.; Schmidt, L.; Wamsler, B.; Beck, J.; Alexanderian,
A.; Fleck, B.
Bibcode: 2009AGUFMSH51B1279H
Altcode:
As the amount of solar data available to scientists continues to
increase at faster and faster rates, it is important that there exist
simple tools for navigating this data quickly with a minimal amount
of effort. By combining heterogeneous solar physics datatypes such
as full-disk images and coronagraphs, along with feature and event
information, Helioviewer offers a simple and intuitive way to browse
multiple datasets simultaneously. Images are stored in a repository
using the JPEG 2000 format and tiled dynamically upon a client's
request. By tiling images and serving only the portions of the image
requested, it is possible for the client to work with very large
images without having to fetch all of the data at once. In addition
to a focus on intercommunication with other virtual observatories
and browsers (VSO, HEK, etc), Helioviewer will offer a number of
externally-available application programming interfaces (APIs) to
enable easy third party use, adoption and extension. Recent efforts
have resulted in increased performance, dynamic movie generation,
and improved support for mobile web browsers. Future functionality
will include: support for additional data-sources including RHESSI,
SDO, STEREO, and TRACE, a navigable timeline of recorded solar events,
social annotation, and basic client-side image processing.
Title: JHelioviewer: Visualizing Large Sets of Solar Images Using
JPEG 2000
Authors: Muller, D.; Fleck, B.; Dimitoglou, G.; Caplins, B. W.;
Amadigwe, D. E.; García Ortiz, J. P.; Wamsler, B.; Alexanderian,
A.; Hughitt, V. K.; Ireland, J.
Bibcode: 2009CSE....11...38M
Altcode: 2009arXiv0906.1582M
All disciplines that work with image data-from astrophysics to medical
research and historic preservation-increasingly require efficient ways
to browse and inspect large sets of high-resolution images. Based on
the JPEG 2000 image-compression standard, the JHelioviewer solar image
visualization tool lets users browse petabyte-scale image archives as
well as locate and manipulate specific data sets.
Title: A Novel Approach to Discovery and Access to Solar Data in
the Petabyte Age
Authors: Mueller, Daniel; Dimitoglou, G.; Hughitt, V. K.; Ireland,
J.; Wamsler, B.; Fleck, B.
Bibcode: 2009SPD....40.1706M
Altcode:
Space missions generate an ever-growing amount of data, as impressively
highlighted by SDO's expected data rate of 1.4 TByte/day. In order
to fully exploit their data, scientists need to be able to browse
and visualize many different data products spanning a large range
of physical length and time scales. So far, the tools available to
the scientific community either require downloading all potentially
relevant data sets beforehand in their entirety or provide only
movies with a fixed resolution and cadence. To facilitate browsing and
analysis of complex time-dependent data sets from multiple sources,
we are developing JHelioviewer, a JPEG 2000-based visualization and
discovery infrastructure for solar image data. Together with its
web-based counterpart helioviewer.org, JHelioviewer offers intuitive
ways to browse large amounts of heterogeneous data remotely and allows
users to search related event data bases. The user interface for
JHelioviewer is a multi-platform Java client that can both communicate
with a remote server via the JPEG 2000 interactive protocol JPIP
and open local data. The random code stream access of JPIP minimizes
data transfer and can encapsulate meta data as well as multiple image
channels in one data stream. This presentation will illustrate some
of the features of JHelioviewer and the advantages of JPEG 2000 as a
new data compression standard.
Title: Composition and Propagation of Galactic Cosmic-Ray Nuclei at
High Energies
Authors: Obermeier, A.; Ave, M.; Boyle, P.; Marshall, J.; Müller, D.
Bibcode: 2009APS..APR.R8004O
Altcode:
Information on the sources of cosmic rays must be deduced from
observations of composition and energy spectra of the arriving
particles, except for the very highest energies, where anisotropies in
arrival directions may identify specific sources. TRACER, currently the
largest balloon-borne detector, has been designed for direct composition
measurements up to the energy regime where air shower experiments
begin to provide indirect information. A long duration flight of
TRACER from Antarctica (2003) has determined the energy spectra of
primary nuclei (O to Fe) up to several 10^14 eV per particle, and has
led to a self-consistent model for the generation and propagation of
these particles in the Galaxy. For a second flight launched in Sweden
(2006), the instrument was upgraded to allow the lighter elements B,C
and N to be included in the measurement. The analysis of this data
set is ongoing, and preliminary results with emphasis on secondary and
primary abundances will be presented. To further improve the knowledge
of cosmic rays in the multi-TeV energy range, additional exposure time
is needed. Improvements in charge resolution, e.g. by inclusion of an
aerogel Cerenkov counter in TRACER, would allow detailed measurements
of all secondary nuclei, including a determination of the sub-iron
to iron abundance ratio. We will discuss the scientific prospects of
such measurements.
Title: Helioviewer.org: An Open-source Tool for Visualizing Solar Data
Authors: Hughitt, V. Keith; Ireland, J.; Schmiedel, P.; Dimitoglou,
G.; Mueller, D.; Fleck, B.
Bibcode: 2009SPD....40.1502H
Altcode:
As the amount of solar data available to scientists continues to
increase at faster and faster rates, it is important that there exist
simple tools for navigating this data quickly with a minimal amount
of effort. By combining heterogeneous solar physics datatypes such
as full-disk images and coronagraphs, along with feature and event
information, Helioviewer offers a simple and intuitive way to browse
multiple datasets simultaneously. Images are stored in a repository
using the JPEG 2000 format and tiled dynamically upon a client's
request. By tiling images and serving only the portions of the image
requested, it is possible for the client to work with very large
images without having to fetch all of the data at once. Currently,
Helioviewer enables users to browse the entire SOHO data archive,
updated hourly, as well as data feature/event catalog data from
eight different catalogs including active region, flare, coronal
mass ejection, type II radio burst data. In addition to a focus on
intercommunication with other virtual observatories and browsers (VSO,
HEK, etc), Helioviewer will offer a number of externally-available
application programming interfaces (APIs) to enable easy third party
use, adoption and extension. Future functionality will include:
support for additional data-sources including TRACE, SDO and STEREO,
dynamic movie generation, a navigable timeline of recorded solar events,
social annotation, and basic client-side image processing.
Title: Propagation and Source Energy Spectra of Cosmic Ray Nuclei
at High Energies
Authors: Ave, M.; Boyle, P. J.; Höppner, C.; Marshall, J.; Müller, D.
Bibcode: 2009ApJ...697..106A
Altcode: 2008arXiv0810.2972A
A recent measurement of the TRACER instrument on long-duration balloon
has determined the individual energy spectra of the major primary cosmic
ray nuclei from oxygen (Z = 8) to iron (Z = 26). The measurements cover
a large range of energies and extend to energies beyond 1014
eV. We investigate if the data set can be described by a simple but
plausible model for acceleration and propagation of cosmic rays. The
model assumes a power-law energy spectrum at the source with a common
spectral index α for all nuclear species, and an energy-dependent
propagation path length (Λ vprop E -0.6) combined with
an energy-independent residual path length Λ0. We find
that the data can be fitted with a fairly soft source spectrum (α =
2.3-2.4), and with a residual path length Λ0 as high as
0.3 g cm-2. We discuss this model in the context of other
pertinent information, and we determine the relative abundances of
the elements at the cosmic ray source.
Title: The Helioviewer Project: Discovery For Everyone Everywhere
Authors: Ireland, Jack; Hughitt, K.; Müller, D.; Dimitoglou, G.;
Schmiedel, P.; Fleck, B.
Bibcode: 2009SPD....40.1501I
Altcode:
The Helioviewer Project: discovery for everyone everywhere There is
an ever increasing amount of solar and heliospheric data gathered
from multiple sources such as space-based facilities and ground based
observatories. There are also multiple feature and event catalogs
arising from human and computer based detection methods. The Helioviewer
Project is developing a suite of technologies to allow users around the
world to visualize, browse and access these heterogeneous datasets in an
intuitive and highly customizable fashion. Helioviewer technologies
are based on the JPEG2000 file format, an extremely flexible format that
allows for the efficient transfer of data (and meta-data, such as FITS
keywords) between client and server. Rather then having to download an
entire image and then examine the small portion- for example, an active
region - that you are interested in, the JPEG2000 file format lets you
preferentially download only those portions you are interested in. This
dramatically reduces the amount of data transferred, making possible
responsive and flexible scientific discovery applications that can
browse populous archives of large images, such as those from the Solar
Dynamics Observatory. In addition, the Helioviewer Project is
designed to be flexible and extensible to data sources as they become
available. Helioviewer.org (www.helioviewer.org) works seamlessly with
the Virtual Solar Observatory (VSO) whilst an application programming
interface (API) is being developed for interaction with the Solar
Dynamics Observatory Heliophysics Event Knowledgebase. After a
short introduction to the underlying technology, a live demonstration
of the web application www.helioviewer.org will be given. We will also
comment on other client applications (Jhelioviewer, a Java-based browse
tool), and the application of Helioviewer technology to existing and
future solar and heliospheric data and feature/event repositories. This
project is funded by NASA VxO and LWS awards and an ESA science award.
Title: Regional dust model performance during SAMUM 2006
Authors: Haustein, K.; Pérez, C.; Baldasano, J. M.; Müller, D.;
Tesche, M.; Schladitz, A.; Esselborn, M.; Weinzierl, B.; Kandler,
K.; von Hoyningen-Huene, W.
Bibcode: 2009GeoRL..36.3812H
Altcode: 2009GeoRL..3603812H
Traditionally there has been a lack of intensive measurements directly
over dust sources for validating the accuracy of dust models. Utilizing
the valuable and unprecedented SAMUM 2006 field campaign dust dataset
in North Africa, we assess the performance and discuss the limitations
of a state-of-the-art dust regional model to reproduce the complex dust
patterns encountered during the campaign. The DREAM model operational
forecast version during SAMUM 2006 (OPER) and an updated model version
(RESH) are run and compared. RESH reproduces the general Saharan dust
pattern, whereas OPER shows limitations to quantitatively reproduce
dust optical properties over sources and after long range transport
simultaneously. Dust transport in RESH with enhanced number size
bin distribution is proven to be more efficient and adequate. The
modeled vertical extinction coefficient captures fairly well lidar
observations. While particle number size distribution is consistently
reproduced at surface level, we find significant underestimation in
the middle troposphere for large particles. Occasionally, synoptic
scale meteorology remains unsatisfactorily captured leading to errors
in the location and intensity of dust emission and subsequent transport.
Title: Perturbations of Dark Matter Gravity
Authors: Maia, M. D.; Capistrano, A. J. S.; Muller, D.
Bibcode: 2009IJMPD..18.1273M
Altcode: 2009arXiv0909.4759M
Until recently the study of the gravitational field of dark matter
was primarily concerned with its local effects on the motion of
stars in galaxies and galaxy clusters. On the other hand, the WMAP
experiment has shown that the gravitational field produced by dark
matter amplifies the higher acoustic modes of the CMBR power spectrum,
more intensely than the gravitational field of baryons. Such a wide
range of experimental evidences from cosmology to local gravity
suggests the necessity of a comprehensive analysis of the dark matter
gravitational field per se, regardless of any other attributes that
dark matter may eventually possess. In this paper we introduce and
apply Nash's theory of perturbative geometry to the study of the dark
matter gravitational field alone, in a higher-dimensional framework. It
is shown that the dark matter gravitational perturbations in the early
universe can be explained by the extrinsic curvature of the standard
cosmology. Together with the estimated presence of massive neutrinos,
such geometric perturbation is compatible not only with the observed
power spectrum in the WMAP experiment but also with the most recent
data on the accelerated expansion of the universe. It is possible
that the same structure formation exists locally, such as in the cases
of young galaxies or in cluster collisions. In most other cases it
seems to have ceased when the extrinsic curvature becomes negligible,
leading to Einstein's equations in four dimensions. The slow motion
of stars in galaxies and the motion of plasma substructures in nearly
colliding clusters are calculated with the geodesic equation for a
slowly moving object in a gravitational field of arbitrary strength.
Title: Crest - A Balloon-borne Instrument To Measure Cosmic-ray
Electrons Above TeV Energies.
Authors: Schubnell, Michael; Anderson, T.; Bower, C.; Coutu, S.;
Geske, M.; Müller, D.; Musser, J.; Nutter, S.; Park, N.; Tarlé,
G.; Wakely, S.; Yagi, A.
Bibcode: 2009AAS...21347509S
Altcode: 2009BAAS...41R.436S
The observation of high energy (E > 1 TeV) electrons in the cosmic
radiation provides important information on the distribution and
energetics of local cosmic-ray sources. Galactic cosmic-ray electrons
are thought to be shock accelerated in supernova remnants as evident
from observations of non-thermal X-rays and TeV gamma rays. Their
locally observed energy spectrum above 1 TeV is expected to reflect
the distribution and abundance of nearby acceleration sites. However,
the rates at these energies are low and the direct detection would
require unfeasibly large balloons or satellite born detectors. CREST,
a balloon-borne detector array of 1024 BaF2 crystals, overcomes this
hurdle: it will measure the intensity and spectrum of multi-TeV
electrons by detecting synchrotron photons emitted from electrons
passing through the earth's magnetic field. Thus CREST's acceptance
is several times its geometric area providing sensitivity up to about
50 TeV. Following an engineering flight in spring of 2009, CREST will
be flown in a circumpolar orbit on an upcoming Antarctic long-duration
balloon flight. This work is supported by NASA and CSBF.
Title: Future Cosmic-ray Observations On Balloons - Challenges
And Requirements
Authors: Wakely, Scott; Boyle, P.; Muller, D.; Swordy, S.
Bibcode: 2009AAS...21347516W
Altcode: 2009BAAS...41..438W
A number of advanced technologies have now reached maturity
for applications in cosmic-ray research on long-duration balloon
flights. Examples of these include superconducting magnet technology,
precise particle tracking devices, transition radiation detectors,
and a variety of advanced Cherenkov counters, combined with high-speed
and high-volume data readout, processing and storage systems. If
these technologies are incorporated into large-area detector systems,
definitive answers to long-standing questions of astrophysical and
cosmological importance can be expected. We will discuss several
examples: the precise measurement of cosmic-ray positrons and its
potential for dark-matter searches; studies of the Galactic propagation
of cosmic rays through precise observations of secondary nuclei at
the highest energies; and studies of the acceleration process through
the detection of the individual energy spectra of cosmic-ray nuclei
at the highest energies. While initial measurements on some of these
topics have been made in pioneering observations in the past, we will
emphasize the potential for great advances that lie ahead if the most
modern technologies are coupled with the potential of the long-duration
balloon vehicle.
Title: Topologically driven coronal dynamics - a mechanism for
coronal hole jets
Authors: Müller, D. A. N.; Antiochos, S. K.
Bibcode: 2008AnGeo..26.2967M
Altcode:
Bald patches are magnetic topologies in which the magnetic field is
concave up over part of a photospheric polarity inversion line. A
bald patch topology is believed to be the essential ingredient
for filament channels and is often found in extrapolations of the
observed photospheric field. Using an analytic source-surface model to
calculate the magnetic topology of a small bipolar region embedded in
a global magnetic dipole field, we demonstrate that although common
in closed-field regions close to the solar equator, bald patches are
unlikely to occur in the open-field topology of a coronal hole. Our
results give rise to the following question: What happens to a bald
patch topology when the surrounding field lines open up? This would
be the case when a bald patch moves into a coronal hole, or when
a coronal hole forms in an area that encompasses a bald patch. Our
magnetostatic models show that, in this case, the bald patch topology
almost invariably transforms into a null point topology with a spine
and a fan. We argue that the time-dependent evolution of this scenario
will be very dynamic since the change from a bald patch to null point
topology cannot occur via a simple ideal evolution in the corona. We
discuss the implications of these findings for recent Hinode XRT
observations of coronal hole jets and give an outline of planned
time-dependent 3-D MHD simulations to fully assess this scenario.
Title: Solar Orbiter: Status Update
Authors: Müller, D.; Marsden, R. G.
Bibcode: 2008ESPM...12..6.4M
Altcode:
The Solar Orbiter Mission will study the Sun in greater detail
than ever before due the close proximity of the spacecraft as it
orbits the Sun. At its closest point, Solar Orbiter will be about
0.22 AU from the Sun, closer than any other satellite to date. In
addition to providing high-resolution images of the solar surface,
perihelion passes at these distances occur in near co-rotation with
the Sun, allowing the instruments to track features on the surface for
several days. The mission profile also includes a high-latitude phase
that will allow observations from up to 35 degrees above the solar
equator. Multiple Venus gravity assist manoeuvres will be employed
to increase the inclination of the orbital plane. The combination of
near-Sun, quasi-heliosynchronous and high-latitude observations by
remote-sensing and in-situ instruments makes Solar Orbiter a unique
platform for the study of the links between the Sun and the inner
heliosphere. In this paper, we will review the mission goals and
the corresponding mission requirements, together with the technical
challenges, and give an update on recent activities.
Title: Cosmic ray composition at high energies: The TRACER project
Authors: Boyle, P. J.; Gahbauer, F.; Höppner, C.; Hörandel, J.;
Ichimura, M.; Müller, D.; Wolf, A. Romero; TRACER project
Bibcode: 2008AdSpR..42..409B
Altcode:
The TRACER instrument (Transition Radiation Array for Cosmic Energetic
Radiation) is designed to measure the individual energy spectra of
cosmic ray nuclei in long duration balloon flights. The large geometric
factor of TRACER (5 m2 sr) permits statistically significant
measurements at particle energies well beyond 1014 eV. TRACER
identifies individual cosmic ray nuclei with single element resolution,
and measures their energy over a wide range, from about 0.5 to 10,000
GeV/amu. This is accomplished with a gas detector system of 1600
single wire proportional tubes and plastic fiber radiators combined
with plastic scintillators and acrylic Cerenkov counters. A 2-week
flight in Antarctica in December 2003 has led to a measurement of the
nuclear species oxygen to iron up to about 3000 GeV/amu. As an example,
we shall present the energy spectrum and relative abundance for neon
and discuss the implication of this result in the context of current
models of acceleration and propagation of galactic cosmic rays. The
instrument has been refurbished and flown on a second long duration
balloon flight in Summer 2006. For this flight, the dynamic range of
TRACER has been extended to permit inclusion of the lighter elements B,
C, and N in the measurement.
Title: Composition of Primary Cosmic-Ray Nuclei at High Energies
Authors: Ave, M.; Boyle, P. J.; Gahbauer, F.; Höppner, C.; Hörandel,
J. R.; Ichimura, M.; Müller, D.; Romero-Wolf, A.
Bibcode: 2008ApJ...678..262A
Altcode: 2008arXiv0801.0582A
The TRACER instrument (Transition Radiation Array for Cosmic Energetic
Radiation) has been developed for direct measurements of the heavier
primary cosmic-ray nuclei at high energies. The instrument had a
successful long-duration balloon flight in Antarctica in 2003. The
detector system and measurement process are described, details of the
data analysis are discussed, and the individual energy spectra of the
elements O, Ne, Mg, Si, S, Ar, Ca, and Fe (nuclear charge Z = 8-26)
are presented. The large geometric factor of TRACER and the use of a
transition radiation detector make it possible to determine the spectra
up to energies in excess of 1014 eV per particle. A power-law
fit to the individual energy spectra above 20 GeV amu-1
exhibits nearly the same spectral index (2.65 +/- 0.05) for all
elements, without noticeable dependence on the elemental charge Z.
Title: A Mechanism for Coronal Hole Jets
Authors: Mueller, D. A. N.; Antiochos, S. K.
Bibcode: 2008arXiv0804.3995M
Altcode:
Bald patches are magnetic topologies in which the magnetic field is
concave up over part of a photospheric polarity inversion line. A
bald patch topology is believed to be the essential ingredient
for filament channels and is often found in extrapolations of the
observed photospheric field. Using an analytic source-surface model to
calculate the magnetic topology of a small bipolar region embedded in
a global magnetic dipole field, we demonstrate that although common
in closed-field regions close to the solar equator, bald patches are
unlikely to occur in the open-field topology of a coronal hole. Our
results give rise to the following question: What happens to a bald
patch topology when the surrounding field lines open up? This would
be the case when a bald patch moves into a coronal hole, or when
a coronal hole forms in an area that encompasses a bald patch. Our
magnetostatic models show that, in this case, the bald patch topology
almost invariably transforms into a null point topology with a spine
and a fan. We argue that the time-dependent evolution of this scenario
will be very dynamic since the change from a bald patch to null point
topology cannot occur via a simple ideal evolution in the corona. We
discuss the implications of these findings for recent Hinode XRT
observations of coronal hole jets and give an outline of planned
time-dependent 3D MHD simulations to fully assess this scenario.
Title: The Cosmic Ray Electron Synchrotron Telescope (CREST)
Experiment
Authors: Schubnell, M.; Bower, C.; Coutu, S.; Müller, D.; Musser,
J.; Nutter, S.; Tarlé, G.; Wakely, S.; Yagi, A.
Bibcode: 2008ICRC....2..305S
Altcode: 2008ICRC...30b.305S
CREST is a balloon-borne detector array of barium fluoride crystal
scintillators which will measure the intensity and spectrum of multi-TeV
electrons in the Cosmic Rays. By detecting the synchrotron photons
emitted from electrons passing through the earth's magnetic field,
CREST's acceptance is several times its geometric area. We present
background measurement results from a small array prototype flight
(CREST-I) and describe the full instrument (CREST-II) which is scheduled
for an Antarctic Long Duration Balloon flight in late 2009.
Title: The TRACER Project: Instrument Concept, Balloon Flights,
and Analysis Procedures
Authors: Müller, D.; Boyle, P. J; Gahbauer, F.; Höppner, C.;
Hörandel, J.; Ichimura, M.; Müller, D.; Romero-Wolf, A.
Bibcode: 2008ICRC....2...83M
Altcode: 2008ICRC...30b..83M
Accurate measurements of the composition and energy spectra of
cosmic rays beyond the TeV energy region have been an experimental
challenge for years. TRACER ("Transition Radiation Array for Cosmic
Energetic Radiation"), is currently the largest cosmic-ray detector
for direct measurements, and has been developed for long-duration
balloon flights. The instrument is unconventional in that it uses
only electromagnetic processes, such as measurements of ionization
energy loss, Cherenkov light, and transition radiation, to make
precision measurements that span more than four decades in energy,
from 1 GeV/nucleon to energies beyond 10 TeV/nucleon. In its first
long-duration balloon flight from Antarctica in December 2003, TRACER
has measured the energy spectra of the primary galactic cosmic-ray
nuclei from oxygen (Z = 8) to iron (Z = 26). For a second LDB flight
from Sweden in July 2006, the instrument was modified and upgraded
in order to include the important light nuclei from boron (Z = 5)
to nitrogen (Z = 7). We shall discuss the performance of TRACER in
these two flights, review the response of the individual detector
components, and the techniques employed in the data analysis. We will
discuss the resolution of TRACER both in charge and in energy, and
review the statistical and systematic uncertainties of the measurements.
Title: Synchrotron radiation from primary cosmic ray electrons:
Monte Carlo studies of event topographies and potential backgrounds
at balloon altitudes
Authors: Nutter, S.; Bower, C. R.; Coutu, S.; Muller, D.; Musser,
J.; Schubnell, M.; Tarle, G.; Wakely, S. P.; Yagi, A.
Bibcode: 2008ICRC....2..309N
Altcode: 2008ICRC...30b.309N
The balloon-borne Cosmic Ray Electron Synchrotron Telescope (CREST)
experiment will measure the flux of cosmic ray electrons at energies
greater than 2 TeV by detecting the x-ray component of the synchrotron
radiation emitted as the electrons traverse the Earth’s magnetic
field. This method enhances the instrument acceptance to several times
its geometric area. A Monte Carlo simulation of electrons traversing
the atmosphere was performed using GEANT4 in order to calculate the
acceptance of CREST, characterize synchrotron radiation patterns at
balloon altitudes, and search for potential backgrounds due to clusters
of x-ray photons within atmospheric showers. The study results influence
the design of CREST and potential future instruments using a similar
detection technique.
Title: The Flight Electronics System for the Cosmic Ray Electron
Synchrotron Telescope (CREST) Experiment
Authors: Tarle, G.; Ameel, J.; Ball, R.; Bower, C.; Coutu, S.; Gephard,
M.; Muller, D.; Musser, J.; Nutter, S.; Schubnell, M.; Smith, C.;
Wakely, S.; Yagi, A.
Bibcode: 2008ICRC....2..313T
Altcode: 2008ICRC...30b.313T
The balloon-borne Cosmic Ray Electron Synchrotron Telescope (CREST)
experiment will employ a novel distributed electronics system to
collect timing and pulse height information from 1024 BaF2 crystal
detectors and 42 PMTs in its anticoincidence shield. The timing of
single photoelectron triggers from the PMTs in the crystal array is
recorded to an accuracy of 1 ns least count. Wide dynamic range pulse
height information from two dynodes on each PMT is recorded when
two or more crystals receive single photoelectron triggers. Timing
and pulse height information from the anticoincidence shield is
recorded only when received within a preset time window of crystal
array triggers. Integral Cockroft-Walton high voltage power supplies,
potted within the PMTs are individually set by a digitally addressable
control and monitoring system. Extensive use of FPGAs and CPLDs enable
high-speed synchronous operation and low power consumption with a
flexible distributed and modular architecture.
Title: Propagation of High-Energy Cosmic Rays through the Galaxy:
Discussion and Interpretation of TRACER Results
Authors: Ave, M.; Boyle, P. J.; Höppner, C.; Hörandel, J.; Ichimura,
M.; Müller, D.
Bibcode: 2008ICRC....2..215A
Altcode: 2008ICRC...30b.215A
The long-duration balloon flights of TRACER have provided new
measurements of the intensities and energy spectra of the arriving
cosmic-ray nuclei with 5 ≤ Z ≤ 26 at high energies. In order to
determine the particle composition and energy spectra at the cosmic-ray
sources, changes occurring during the interstellar propagation of
cosmic rays must be known. We use a simple propagation model with
energy-dependent pathlength and derive constraints on the propagation
parameters from a self-consistent fit to the measured energy spectra. We
use the model to obtain the relative abundances of the cosmic ray
nuclei at the acceleration site and compare these with the "universal"
abundance scale.
Title: Cosmic Ray Energy Spectra of Primary Nuclei from Oxygen to
Iron: Results from the TRACER 2003 LDB Flight
Authors: Boyle, P. J.; Ave, M.; Höppner, C.; Hörandel, J.; Ichimura,
M.; Müller, D.; Romero-Wolf, A.
Bibcode: 2008ICRC....2...87B
Altcode: 2008ICRC...30b..87B
The first long-duration balloon flight of TRACER in 2003 provided
high-quality measurements of the primary cosmic-ray nuclei over
the range oxygen (Z = 8) to iron (Z = 26). The analysis of these
measurements is now complete, and we will present the individual energy
spectra and absolute intensities of the nuclei O, Ne, Mg, Si, S, Ca, A,
and Fe. The spectra cover the energy range from 1 GeV/nucleon to more
than 10 TeV/nucleon, or in terms of total energy, to several 1014 eV
per particle. We shall compare our results with those of other recent
observations in space and on balloons. We notice, in general, good
agreement with these data for those regions where overlap exists. We
also shall compare our data with information that has recently been
inferred from air shower observations.
Title: Fine Structure of the Net Circular Polarization in a Sunspot
Penumbra
Authors: Tritschler, A.; Müller, D. A. N.; Schlichenmaier, R.;
Hagenaar, H. J.
Bibcode: 2007ApJ...671L..85T
Altcode: 2007arXiv0710.4545T
We present novel evidence for fine structure observed in the
net circular polarization (NCP) of a sunspot penumbra based on
spectropolarimetric measurements utilizing the Zeeman-sensitive Fe
I 630.2 nm line. For the first time we detect filamentary organized
fine structure of the NCP on spatial scales that are similar to the
inhomogeneities found in the penumbral flow field. We also observe an
additional property of the visible NCP, a zero-crossing of the NCP
in the outer parts of the center-side penumbra, which has not been
recognized before. In order to interpret the observations we solve the
radiative transfer equations for polarized light in a model penumbra
with embedded magnetic flux tubes. We demonstrate that the observed
zero-crossing of the NCP can be explained by an increased magnetic
field strength inside magnetic flux tubes in the outer penumbra combined
with a decreased magnetic field strength in the background field. Our
results strongly support the concept of the uncombed penumbra.
Title: Flux Tubes as the Origin of Net Circular Polarization in
Sunspot Penumbrae
Authors: Borrero, J. M.; Bellot Rubio, L. R.; Müller, D. A. N.
Bibcode: 2007ApJ...666L.133B
Altcode: 2007arXiv0707.4145B
We employ a three-dimensional magnetohydrostatic model of a
horizontal flux tube, embedded in a magnetic surrounding atmosphere,
to successfully reproduce the azimuthal and center-to-limb variations
of the net circular polarization observed in sunspot penumbrae. This
success is partly due to the realistic modeling of the interaction
between the flux tube and the surrounding magnetic field.
Title: A Mechanism for Coronal Hole Jets
Authors: Mueller, Daniel; Antiochos, S. K.
Bibcode: 2007AAS...210.9117M
Altcode: 2007BAAS...39..206M
Bald patches are magnetic topologies in which the magnetic field is
concave up over part of a photospheric polarity inversion line. A
bald patch topology is believed to be the essential ingredient
for filament channels and is often found in extrapolations of the
observed photospheric field. We demonstrate that although common in
closed field regions, bald patches are unlikely to occur in the open
field topology of a coronal hole. We use an analytic source-surface
model to calculate the magnetic topology of a small "active region"
dipole embedded in a central magnetic dipole field. While bald patches
readily occur in closed-field regions, we show that there is only
a highly limited parameter range for them to form in open-field regions. Furthermore, the inclusion of a finite gas pressure and
solar wind is likely to destroy even this limited parameter range for
the existence of bald patches in coronal holes. Our results give rise
to the following question: What happens to a bald patch topology when
the surrounding field lines open up? This would be the case when a bald
patch moves into a coronal hole, or when a coronal hole forms in an
area that encompasses a bald patch. Our magnetostatic models show that,
in this case, the bald patch topology almost invariably transforms
into a null point topology with a spine and a fan. We argue that the
time-dependent evolution of this scenario will be very dynamic since
the change from a bald patch to null point topology cannot occur
via a simple ideal evolution in the corona. We discuss the implications
of these findings for recent Hinode XRT observations of coronal hole
jets and give an outline of planned time-dependent 3D MHD simulations
to fully assess this scenario. This work was supported in part
by NASA and ONR.
Title: Cosmic ray composition at high energies: Results from the
TRACER project
Authors: Boyle, P. J.; Ave, M.; Gahbauer, F.; Hoeppner, C.; Hoerandel,
J.; Ichimura, M.; Mueller, D.; Romero-Wolf, A.
Bibcode: 2007astro.ph..3707B
Altcode:
The TRACER instrument Transition Radiation Array for Cosmic Energetic
Radiation is designed to measure the individual energy spectra of
cosmic-ray nuclei in long-duration balloon flights The large geometric
factor of TRACER 5 m 2 sr permits statistically significant measurements
at particle energies well beyond 10 14 eV TRACER identifies individual
cosmic-ray nuclei with single-element resolution and measures their
energy over a very wide range from about 0 5 to 10 000 GeV nucleon
This is accomplished with a gas detector system of 1600 single-wire
proportional tubes and plastic fiber radiators that measure specific
ionization and transition radiation signals combined with plastic
scintillators and acrylic Cherenkov counters A two-week flight in
Antarctica in December 2003 has led to a measurement of the nuclear
species oxygen to iron O Ne Mg Si S Ar Ca and Fe up to about 3 000 GeV
nucleon We shall present the energy spectra and relative abundances
for these elements and discuss the implication of the results in
the context of current models of acceleration and propagation of
galactic cosmic rays The instrument has been refurbished for a second
long-duration flight in the Northern hemisphere scheduled for summer
2006 For this flight the dynamic range of TRACER has been extended to
permit inclusion of the lighter elements B C and N in the measurement.
Title: Multiwavelength Raman lidar observations of particle
growth during long-range transport of forest-fire smoke in the
free troposphere
Authors: Müller, D.; Mattis, I.; Ansmann, A.; Wandinger, U.; Ritter,
C.; Kaiser, D.
Bibcode: 2007GeoRL..34.5803M
Altcode:
We present particle effective radii and Ångström exponents of aged
free-tropospheric forest-fire smoke. The particle plumes were observed
with different multiwavelength Raman lidars downwind of the fires that
burned in boreal areas of the northern hemisphere. We find an increase
of particle size, respectively decrease of the Ångström exponent with
transport time which was more than two weeks in some of the investigated
cases. Mean effective radii were as large as 0.4 μm. Mean Ångström
exponents were as low as 0.04 for the wavelength pair at 355/532 nm. A
fit curve that describes particle growth with time is derived. Particle
growth levels off after approximately ten days of transport time.
Title: Casimir effect in E3 closed spaces
Authors: Lima, Mariana P.; Müller, Daniel
Bibcode: 2007CQGra..24..897L
Altcode: 2006gr.qc.....5112L
As it is well known the topology of space is not totally determined
by Einstein's equations. It is considered a massless scalar quantum
field in a static Euclidean space of dimension 3. The expectation value
for the energy density in all compact orientable Euclidean 3-spaces
are obtained in this work as a finite summation of Epstein type zeta
functions. The Casimir energy density for these particular manifolds
is independent of the type of coupling with curvature. A numerical
plot of the result inside each Dirichlet region is obtained.
Title: Disentangling The Magnetic Field Structure Of Sunspots -
Stereoscopic Polarimetry With Solar Orbiter
Authors: Müller, D. A. N.,; Schlichenmaier, R.; Fleck, B.; Fritz, G.
Bibcode: 2007ESASP.641E..32M
Altcode:
Sunspots exhibit complex, highly structured magnetic fields and
flows. Disentangling the atmospheric structure of sunspots is a
great challenge, and can only be achieved by the combination of
spectropolarimetry at high spatial resoultion and detailed modeling
efforts. We use a generalized 3D the embeds magnetic flux tuber in
a stratified atmosphere and calculates the emerging polarization
of spectrail lines for arbitrary viewing angles. The resulting
polarization maps are a very efficient tool to distinguish between
different atmospheric scenarios and determine the 3D structure of the
magnetic field and the flow field. In this contribution, we present
synthetic maps of the net circular polarication (NCP) as a function of
the heliocentric angle for different spectral lines of interest. Among
these are the Fe I 617.3 nm line which would be observed by the VIM
instrument abard Solar Orbiter and the Fe I 630.2 nm line which will
be observed by Hinode (formerly known as Solar-B).
Title: On the inhomogeneities of the sunspot penumbra
Authors: Schlichenmaier, R.; Müller, D. A. N.; Beck, C.
Bibcode: 2007msfa.conf..233S
Altcode: 2007astro.ph..3021S
The penumbra is ideally suited to challenge our understanding
of magnetohydrodynamics. The energy transport takes place as
magnetoconvection in inclined magnetic fields under the effect of
strong radiative cooling at the surface. The relevant processes
happen at small spatial scales. In this contribution we describe
and elaborate on these small-scale inhomogeneities of a sunspot
penumbra. We describe the penumbral properties inferred from imaging,
spectroscopic and spectropolarimetric data, and discuss the question
of how these observations can be understood in terms of proposed models
and theoretical concepts.
Title: The multi-component field topology of sunspot penumbrae. A
diagnostic tool for spectropolarimetric measurements
Authors: Müller, D. A. N.; Schlichenmaier, R.; Fritz, G.; Beck, C.
Bibcode: 2006A&A...460..925M
Altcode: 2006astro.ph..9632M
Context: .Sunspot penumbrae harbor highly structured magnetic fields
and flows. The moving flux tube model offers an explanation for several
observed phenomena, e.g. the Evershed effect and bright penumbral
grains.
Aims: .A wealth of information can be extracted from
spectropolarimetric observations. In order to deduce the structure of
the magnetic field in sunspot penumbrae, detailed forward modeling is
necessary. On the one hand, it gives insight into the sensitivity of
various spectral lines to different physical scenarios. On the other
hand, it is a very useful tool to guide inversion techniques. In this
work, we present a generalized 3D geometrical model that embeds an
arbitrarily shaped flux tube in a stratified magnetized atmosphere.
Methods: .The new semi-analytical geometric model serves as a
frontend for a polarized radiative transfer code. The advantage of
this model is that it preserves the discontinuities of the physical
parameters across the flux tube boundaries. This is important for the
detailed shape of the emerging Stokes Profiles and the resulting net
circular polarization (NCP).
Results: .(a) The inclination of
downflows in the outer penumbra must be shallower than approximately
15° (b) observing the limb-side NCP of sunspots in the Fe I 1564.8
nm line offers a promising way to identify a reduced magnetic field
strength in flow channels; (c) the choice of the background atmosphere
can significantly influence the shape of the Stokes profiles, but does
not change the global characteristics of the resulting NCP curves for
the tested atmospheric models.
Title: About Starobinsky inflation
Authors: Müller, Daniel; Vitenti, Sandro D. P.
Bibcode: 2006PhRvD..74h3516M
Altcode: 2006gr.qc.....6018M
It is believed that soon after the Planck era, space-time should
have a semiclassical nature. According to this, the escape from the
general relativity theory is unavoidable. Two geometric counterterms
are needed to regularize the divergences which come from the expected
value. These counterterms are responsible for a higher derivative metric
gravitation. Starobinsky’s idea was that these higher derivatives
could mimic a cosmological constant. In this work numerical solutions
are considered for general Bianchi I anisotropic space-times in this
higher derivative theory. The approach is “experimental” in the
sense that there is no attempt for an analytical investigation of
the results. It is shown that for zero cosmological constant Λ=0,
there are sets of initial conditions which form basins of attraction
that asymptote Minkowski space. The complement of this set of
initial conditions form basins which are attracted to some singular
solutions. It is also shown, for a cosmological constant Λ>0, that
there are basins of attraction to a specific de Sitter solution. This
result is consistent with Starobinsky’s initial idea. The complement
of this set also forms basins that are attracted to some type of
singular solution. Because the singularity is characterized by curvature
scalars, it must be stressed that the basin structure obtained is a
topological invariant, i.e., coordinate independent.
Title: Strong particle light absorption over the Pearl River Delta
(south China) and Beijing (north China) determined from combined
Raman lidar and Sun photometer observations
Authors: Müller, D.; Tesche, M.; Eichler, H.; Engelmann, R.;
Althausen, D.; Ansmann, A.; Cheng, Y. F.; Zhang, Y. H.; Hu, M.
Bibcode: 2006GeoRL..3320811M
Altcode:
Particle size and absorption properties have been determined from
combined one-wavelength Raman lidar and Sun photometer measurements
in the Pearl River Delta (South China) in October 2004, and in Beijing
(North China) in January 2005. Particle effective radius varied around
0.24 μm in the south of China. Aerosols were strongly light absorbing
throughout the continental haze layers. The mean imaginary part was
around 0.02i and the single-scattering albedo was as low as 0.75 at
532 nm wavelength. Similar aerosol properties were found over Beijing.
Title: Numerical Bianchi typeI solutions in semiclassical gravitation
Authors: Vitenti, Sandro D. P.; Müller, Daniel
Bibcode: 2006PhRvD..74f3508V
Altcode: 2006gr.qc.....4127V
It is believed that soon after the Planck era, spacetime should
have a semiclassical nature. In this context we consider quantum
fields propagating in a classical gravitational field and study
the backreaction of these fields, using the expected value of the
energy-momentum tensor as source of the gravitational field. According
to this theory, the escape from general relativity theory is
unavoidable. Two geometric counter-term are needed to regularize
the divergences which come from the expected value. There is a
parameter associated to each counter-term and in this work we found
numerical solutions of this theory to particular initial conditions,
for general Bianchi Type I spaces. We show that even though there
are spurious solutions some of them can be considered physical. These
physical solutions include de Sitter and Minkowski that are obtained
asymptotically.
Title: Net Circular Polarization of Sunspot Penumbrae- A Versatile
Tool for Diagnosing Magnetic Field Structure
Authors: Müller, D. A. N.; Schlichenmaier, R.; Fritz, G.; Beck, C.
Bibcode: 2006ESASP.617E..72M
Altcode: 2006soho...17E..72M
No abstract at ADS
Title: Net Circular Polarization Of Sunspot Penumbrae - A Versatile
Model For Diagnosing Magnetic Field Structure
Authors: Mueller, Daniel; Schlichenmaier, R.; Fritz, G.; Beck, C.
Bibcode: 2006SPD....37.0707M
Altcode: 2006BAAS...38..229M
Sunspot penumbrae harbor highly structured magnetic fields and
flows. The moving flux tube model offers an explanation for several
observed phenomena, e.g. the Evershed effect and bright penumbral
grains. In this work, we present a generalized 3D model that embeds an
arbitrarily shaped flux tube in a stratified magnetized atmosphere. The
new model is a versatile tool to calculate the spectral signature of
flux tubes in the penumbra and especially make predictions about the
flow speed and tube inclination from observed maps of the net circular
polarization (NCP). As a first result, we find that the inclination
of downflows in the outer penumbra must be shallower than approx. 15°.
Title: 10 years of SOHO
Authors: Fleck, Bernhard; Müller, Daniel; Haugan, Stein; Sánchez
Duarte, Luis; Siili, Tero; Gurman, Joseph B.
Bibcode: 2006ESABu.126...24F
Altcode:
Since its launch on 2 December 1995, SOHO has revolutionised
our understanding of the Sun. It has provided the first images of
structures and flows below the Sun's surface and of activity on the
far side. SOHO has revealed the Sun's extremely dynamic atmosphere,
provided evidence for the transfer of magnetic energy from the surface
the outer solar atmosphere, the corona, through a "magnetic carpet",
and identified the source regions of the fast solar wind. It has
revolutionised our understanding of solar-terrestrial relations and
dramatically improved our space weather-forecasting by its continuous
stream of images covering the atmosphere, extended corona and far
side. The findings are documented in an impressive number of scientific
publications: over 2500 papers in refereed journals since launch,
representing the work of over 2300 individual scientists. At the
same time, SOHO's easily accessible, spectacular data and fundamental
scientific results have captured the imagination of the space science
community and the general public alike. As a byproduct of the efforts
to provide real-time data to the public, amateurs now dominate SOHO's
discovery of over 1100 Sungrazing comets.
Title: Searching for high energy cosmic ray electrons using the
Earth's magnetic field.
Authors: Nutter, S.; Bower, C.; Coutu, S.; Duvernois, M.; Martell,
A.; Muller, D.; Musser, J.; Schubnell, M.; Tarle, G.; Yagi, A.
Bibcode: 2006APS..APR.P7001N
Altcode:
The Cosmic Ray Electron Synchrotron Telescope (CREST) instrument is
a balloon payload designed to measure the flux of primary cosmic ray
electrons at energies greater than 2 TeV. Because electrons at these
energies lose energy rapidly during propagation through the interstellar
medium, their detection would indicate the existence of sources
which are within a few kiloparsecs. In order to obtain the needed
large exposure time and aperture of the detector, we use an approach
that depends on the detection of synchrotron photons emitted when the
electrons travel through the earth's magnetic field. Such photons have
energies in the x-ray and gamma-ray region, hence CREST incorporates
an array of inorganic scintillators. Since the primary electrons
do not need to pass through the detector, the effective detection
area is much larger than the actual detector array size. To verify
the technique and to determine background count rates, a prototype
array of BGO and BaF2 crystals was flown on high altitude balloon from
Ft. Sumner, N.M. in autumn 2005. The full detector system is currently
under construction. It will consist of a 1600 crystal array, and will
be carried on Long-Duration Balloons on circumpolar trajectory.
Title: Casimir Effect in Compact Universes
Authors: Müller, Daniel
Bibcode: 2006tmgm.meet.1668M
Altcode: 2004gr.qc.....3086M; 2005tmgm.meet.1668M
The Casimir effect in compact hyperbolic Universes was numerically
obtained in previous publications. In this talk, I expose these results.
Title: Cosmic ray composition at high energies: Results from the
TRACER project
Authors: Ave, M.; Boyle, P. J.; Gahbauer, F.; Höppner, C.; Hörandel,
J.; Ichimura, M.; Müller, D.; Romero-Wolf, A.
Bibcode: 2006cosp...36.2517A
Altcode: 2006cosp.meet.2517A
The TRACER instrument Transition Radiation Array for Cosmic Energetic
Radiation is designed to measure the individual energy spectra of
cosmic-ray nuclei in long-duration balloon flights The large geometric
factor of TRACER 5 m 2 sr permits statistically significant measurements
at particle energies well beyond 10 14 eV TRACER identifies individual
cosmic-ray nuclei with single-element resolution and measures their
energy over a very wide range from about 0 5 to 10 000 GeV nucleon
This is accomplished with a gas detector system of 1600 single-wire
proportional tubes and plastic fiber radiators that measure specific
ionization and transition radiation signals combined with plastic
scintillators and acrylic Cherenkov counters A two-week flight in
Antarctica in December 2003 has led to a measurement of the nuclear
species oxygen to iron O Ne Mg Si S Ar Ca and Fe up to about 3 000 GeV
nucleon We shall present the energy spectra and relative abundances
for these elements and discuss the implication of the results in
the context of current models of acceleration and propagation of
galactic cosmic rays The instrument has been refurbished for a second
long-duration flight in the Northern hemisphere scheduled for summer
2006 For this flight the dynamic range of TRACER has been extended to
permit inclusion of the lighter elements B C and N in the measurement
Title: a Multi-Wavelength View on Coronal Rain
Authors: Müller, D. A. N.; de Groof, A.; de Pontieu, B.; Hansteen,
V. H.
Bibcode: 2005ESASP.600E..30M
Altcode: 2005dysu.confE..30M; 2005ESPM...11...30M
No abstract at ADS
Title: Multiwavelength Analysis of Downflows Along AN Off-Limb Loop
Authors: de Groof, A.; Müller, D. A. N.; Poedts, S.
Bibcode: 2005ESASP.600E..29D
Altcode: 2005ESPM...11...29D; 2005dysu.confE..29D
No abstract at ADS
Title: Downflows Along AN Off-Limb Loop Seen both in 30.4NM and Hα
Authors: de Groof, A.; Müller, D. A. N.; Poedts, S.
Bibcode: 2005ESASP.596E..36D
Altcode: 2005ccmf.confE..36D
No abstract at ADS
Title: a Multi-Wavelength View on Coronal Rain
Authors: Müller, D. A. N.; de Groof, A.; de Pontieu, B.; Hansteen,
V. H.
Bibcode: 2005ESASP.596E..37M
Altcode: 2005ccmf.confE..37M
No abstract at ADS
Title: Detailed comparison of downflows seen both in EIT 30.4 nm
and Big Bear Hα movies
Authors: de Groof, A.; Bastiaensen, C.; Müller, D. A. N.; Berghmans,
D.; Poedts, S.
Bibcode: 2005A&A...443..319D
Altcode:
An EIT shutterless campaign was conducted on 11 July 2001 and provided
120 high-cadence (68 s) 30.4 nm images of the north-eastern quarter
of the Sun. Systematic intensity variations are seen which appear
to propagate along an off-disk loop-like structure. In this paper we
study the nature of these intensity variations by confronting the EIT
observations studied in De Groof et al. (2004, A&A, 415, 1141)
with simultaneous Hα images from Big Bear Solar Observatory. With
the goal to carefully co-register the two image sets, we introduce a
technique designed to compare data of two different instruments. The
image series are first co-aligned and later overplotted in order to
visualize and compare the behaviour of the propagating disturbances
in both data sets. Since the same intensity variations are seen in
the EIT 30.4 nm and in the Hα images, we confirm the interpretation
of De Groof et al. (2004, A&A, 415, 1141) that we are observing
downflows of relatively cool plasma. The origin of the downflows is
explained by numerical simulations of "catastrophic cooling" in a
coronal loop which is heated predominantly at its footpoints.
Title: The power spectrum of the circular noise
Authors: Müller, Daniel
Bibcode: 2005GReGr..37.1905M
Altcode: 2005gr.qc.....9126M
The circular noise is important in connection to Mach's principle, and
also as a possible probe of the Unruh effect. In this letter the power
spectrum of the detector following the Trocheries-Takeno motion in the
Minkowski vacuum is analytically obtained in the form of an infinite
series. A mean distribution function and corresponding energy density
are obtained for this particular detected noise. The analogous of a
non constant temperature distribution is obtained. And in the end,
a brief discussion about the equilibrium configuration is given.
Title: High-speed coronal rain
Authors: Müller, D. A. N.; De Groof, A.; Hansteen, V. H.; Peter, H.
Bibcode: 2005A&A...436.1067M
Altcode:
At high spatial and temporal resolution, coronal loops are observed to
have a highly dynamic nature. Recent observations with SOHO and TRACE
frequently show localized brightenings "raining" down towards the solar
surface. What is the origin of these features? Here we present for
the first time a comparison of observed intensity enhancements from an
EIT shutterless campaign with non-equilibrium ionization simulations
of coronal loops in order to reveal the physical processes governing
fast flows and localized brightenings. We show that catastrophic cooling
around the loop apex as a consequence of footpoint-concentrated heating
offers a simple explanation for these observations. An advantage of
this model is that no external driving mechanism is necessary as the
dynamics result entirely from the non-linear character of the problem.
Title: A Survey of Unidentified EGRET Sources at Very High Energies
Authors: Fegan, S. J.; Badran, H. M.; Bond, I. H.; Boyle, P. J.;
Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Catanese, M.;
Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.;
Duke, C.; Falcone, A.; Fegan, D. J.; Finley, J. P.; Fortson, L. F.;
Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.;
Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan,
D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.;
Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.;
Lang, M. J.; Le Bohec, S.; Lessard, R. W.; Linton, E.; Lloyd-Evans, J.;
Milovanovic, A.; McEnery, J.; Moriarty, P.; Mukherjee, R.; Muller,
D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.;
Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.;
Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.;
Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker,
G.; Weekes, T. C.; Zweerink, J.
Bibcode: 2005ApJ...624..638F
Altcode:
The Whipple Observatory 10 m γ-ray telescope has been used to survey
the error boxes of EGRET unidentified sources in an attempt to find
counterparts at energies of 350 GeV and above. Twenty-one unidentified
sources detected by EGRET (more than 10% of the total number) have
been included in this survey. In no case is a statistically significant
signal found in the EGRET error box, which implies that, at least for
this sample, the γ-ray spectra of these sources steepen between 100
MeV and 350 GeV. For each EGRET source location, we list candidate
associations and derive upper limits on the integral γ-ray flux above
350 GeV.
Title: Spectrum of Very High Energy Gamma-Rays from the blazar 1ES
1959+650 during Flaring Activity in 2002
Authors: Daniel, M. K.; Badran, H. M.; Bond, I. H.; Boyle, P. J.;
Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Catanese, M.;
Celik, O.; Cogan, P.; Cui, W.; D'Vali, M.; de la Calle Perez, I.; Duke,
C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson,
L. F.; Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube,
J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan,
D.; Humensky, T. B.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman,
M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.;
Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans,
J.; Milovanovic, A.; Moriarty, P.; Müller, D.; Nagai, T.; Nolan,
S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn,
J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.;
Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Vassiliev,
V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J.
Bibcode: 2005ApJ...621..181D
Altcode: 2005astro.ph..3085D
The blazar 1ES 1959+650 was observed in a flaring state with the Whipple
10 m Imaging Atmospheric Cerenkov Telescope in 2002 May. A spectral
analysis has been carried out on the data from that time period,
and the resulting very high energy gamma-ray spectrum (E>=316
GeV) can be well fitted by a power law of differential spectral index
α=2.78+/-0.12stat+/-0.21sys. On 2002 June 4, the
source flared dramatically in the gamma-ray range without any coincident
increase in the X-ray emission, providing the first unambiguous
example of an ``orphan'' gamma-ray flare from a blazar. The gamma-ray
spectrum for these data can also be described by a simple power-law
fit with α=2.82+/-0.15stat+/-0.30sys. There is
no compelling evidence for spectral variability or for any cutoff to
the spectrum.
Title: Measurements with TRACER: Discussion of Results and Future
Prospects
Authors: Mueller, D.; Ave, M.; Boyle, P. J.; Gahbauer, F.; Höppner,
C.; Hörandel, J.; Ichimura, M.; Romero-Wolf, A.; Wakely, S.
Bibcode: 2005ICRC....3...89M
Altcode: 2005ICRC...29c..89M
No abstract at ADS
Title: Antarctic Balloon Flight and Data Analysis of TRACER
Authors: Romero-Wolf, A.; Ave, M.; Boyle, P.; Gahbauer, F.; Höppner,
C.; Ichimura, M.; Müller, D.; Wakely, S.
Bibcode: 2005ICRC....3...97R
Altcode: 2005ICRC...29c..97R
No abstract at ADS
Title: The Response of the TRACER Detector: Design, Calibrations
and Measurements
Authors: Höppner, C.; Ave, M.; Boyle, P.; Gahbauer, F.; Hörandel,
J.; Ichimura, M.; Müller, D.; Romero-Wolf, A.; Wakely, S.
Bibcode: 2005ICRC....3...73H
Altcode: 2005ICRC...29c..73H
No abstract at ADS
Title: Energy Spectra of Heavy Cosmic Ray Nuclei from 0.5 GeV/amu
to 10,000 GeV/amu
Authors: Boyle, P. J.; Ave, M.; Gahbauer, F.; Höppner, C.; Hörandel,
J.; Ichimura, M.; Müller, D.; Romero-Wolf, A.; Wakely, S.
Bibcode: 2005ICRC....3...65B
Altcode: 2005ICRC...29c..65B
No abstract at ADS
Title: New Measurement of the Cosmic-Ray Positron Fraction from 5
to 15GeV
Authors: Beatty, J. J.; Bhattacharyya, A.; Bower, C.; Coutu, S.;
Duvernois, M. A.; McKee, S.; Minnick, S. A.; Müller, D.; Musser,
J.; Nutter, S.; Labrador, A. W.; Schubnell, M.; Swordy, S.; Tarlé,
G.; Tomasch, A.
Bibcode: 2004PhRvL..93x1102B
Altcode: 2004astro.ph.12230B
We present a new measurement of the cosmic-ray positron fraction at
energies between 5 and 15GeV with the balloon-borne HEAT-pbar instrument
in the spring of 2000. The data presented here are compatible with
our previous measurements, obtained with a different instrument. The
combined data from the three HEAT flights indicate a small positron
flux of nonstandard origin above 5GeV. We compare the new measurement
with earlier data obtained with the HEAT-e± instrument,
during the opposite epoch of the solar cycle, and conclude that our
measurements do not support predictions of charge sign dependent solar
modulation of the positron abundance at 5GeV.
Title: Thermal Instability as the Origin of High Speed Coronal Rain
Authors: Müller, D. A. N.; de Groof, A.; Hansteen, V. H.; Peter, H.
Bibcode: 2004ESASP.575..291M
Altcode: 2004soho...15..291M
No abstract at ADS
Title: New measurement of the altitude dependence of the atmospheric
muon intensity
Authors: Beatty, J. J.; Coutu, S.; Minnick, S. A.; Bhattacharyya, A.;
Bower, C. R.; Musser, J. A.; McKee, S. P.; Schubnell, M.; Tarlé,
G.; Tomasch, A. D.; Labrador, A. W.; Müller, D.; Swordy, S. P.;
Duvernois, M. A.; Nutter, S. L.
Bibcode: 2004PhRvD..70i2005B
Altcode: 2004astro.ph.10552B
We present a new measurement of atmospheric muons made during an ascent
of the High Energy Antimatter Telescope balloon experiment. The
muon charge ratio μ+/μ- as a function
of atmospheric depth in the momentum interval 0.3 0.9GeV/c is
presented. The differential μ- intensities in the 0.3
50GeV/c range and for atmospheric depths between 4 960 g/cm2
are also presented. We compare these results with other measurements
and model predictions. We find that our charge ratio is ∼1.1 for
all atmospheric depths and is consistent, within errors, with other
measurements and the model predictions. We find that our measured
μ- intensities are also consistent with other measurements,
and with the model predictions, except at shallow atmospheric depths.
Title: A Search for TeV Gamma-Ray Emission from High-peaked
Flat-Spectrum Radio Quasars Using the Whipple Air Cerenkov Telescope
Authors: Falcone, A. D.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.;
Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.;
D'Vali, M.; de la Calle Perez, I.; Duke, C.; Fegan, D. J.; Fegan,
S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.;
Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.;
Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Kenny,
G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.;
Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton,
E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.;
Nagai, T.; Nolan, S.; Ong, R.; Pallassini, R.; Petry, D.; Pizlo,
F.; Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.;
Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy,
S. P.; Syson, A.; Tyler, K.; Vassiliev, V. V.; Wakely, S. P.; Walker,
G.; Weekes, T. C.; Zweerink, J.
Bibcode: 2004ApJ...613..710F
Altcode: 2004astro.ph..8365F
Blazars have traditionally been separated into two broad categories
based on their optical emission characteristics. Blazars with faint
or no emission lines are referred to as BL Lacertae objects (BL Lacs),
and blazars with prominent, broad emission lines are commonly referred
to as flat-spectrum radio quasars (FSRQs). The spectral energy
distribution of FSRQs has generally been thought of as being more
akin to the low-peaked BL Lacs, which exhibit a peak in the infrared
region of the spectrum, as opposed to high-peaked BL Lacs (HBLs),
which exhibit a peak in UV/X-ray region of the spectrum. All blazars
that are currently confirmed as sources of TeV emission fall into the
HBL category. Recent surveys have found several FSRQs that exhibit
spectral properties, particularly the synchrotron peak frequency,
similar to HBLs. These objects are potential sources of TeV emission
according to several models of blazar jet emission and the evolution
of blazars. Measurements of TeV flux or flux upper limits could
impact existing theories explaining the links between different blazar
types and could have a significant impact on our understanding of the
nature of objects that are capable of TeV emission. In particular,
the presence (or absence) of TeV emission from FSRQs could confirm
(or cast doubt on) recent evolutionary models that expect intermediate
objects in a transitional state between FSRQ and BL Lac. The Whipple
10 m imaging air Cerenkov gamma-ray telescope is well suited for TeV
gamma-ray observations. Using the Whipple telescope, we have taken data
on a small selection of nearby (z<0.1 in most cases) high-peaked
FSRQs. Although one of the objects, B2 0321+33, showed marginal evidence
of flaring, no significant emission was detected. The implications of
this paucity of emission and the derived upper limits are discussed.
Title: Dynamics of solar coronal loops. II. Catastrophic cooling
and high-speed downflows
Authors: Müller, D. A. N.; Peter, H.; Hansteen, V. H.
Bibcode: 2004A&A...424..289M
Altcode: 2004astro.ph..5538M
This work addresses the problem of plasma condensation and
``catastrophic cooling'' in solar coronal loops. We have carried out
numerical calculations of coronal loops and find several classes of
time-dependent solutions (static, periodic, irregular), depending on
the spatial distribution of a temporally constant energy deposition
in the loop. Dynamic loops exhibit recurrent plasma condensations,
accompanied by high-speed downflows and transient brightenings of
transition region lines, in good agreement with features observed with
TRACE. Furthermore, these results also offer an explanation for the
recent EIT observations of \cite{DeGroof+al2004AA} of moving bright
blobs in large coronal loops. In contrast to earlier models, we suggest
that the process of catastrophic cooling is not initiated by a drastic
decrease of the total loop heating but rather results from a loss
of equilibrium at the loop apex as a natural consequence of heating
concentrated at the footpoints of the loop, but constant in time.
Title: Measuring TeV Cosmic-Ray Electrons with CREST
Authors: Schubnell, M.; Bower, C.; Coutu, S.; DuVernois, M.; McKee,
S.; Muller, D.; Musser, J.; Nutter, S.; Swordy, S.; Tarle, G.; Tomasch,
A.; Yagi, A.
Bibcode: 2004HEAD....8.2304S
Altcode: 2004BAAS...36Q.948S
There is strong indirect evidence for the supernova shock acceleration
of galactic cosmic-ray electrons through observations of non-thermal
X-rays and TeV gamma rays from supernova remnants (SNRs). Current and
past electron detectors, typically flown by high altitude balloons,
have been limited in their ability to study high energy electrons
in the local cosmic-ray flux by their short exposure times and
small apertures. To date, no measurements have been made at energies
greater than 2 TeV. Yet the detection of high-energy electrons would
be extremely significant, yielding information about the spatial
distribution of nearby cosmic ray sources. High-energy electrons lose
energy rapidly during propagation in the Galaxy through synchrotron
and inverse Compton processes and thus TeV electrons reaching the
solar system have to originate at distances < 1 kpc, leaving
few known supernova remnants from which these particles could
originate. The spectral shape of high-energy electrons should,
therefore, be strongly affected by the number of nearby sources,
and their distance distribution. Conversely, if no such features
in the high-energy electron spectrum are observed it will call into
question our understanding of cosmic ray sources and propagation. The
balloon-borne Cosmic Ray Electron Synchrotron Telescope (CREST) will
detect high-energy electrons by measuring the X-ray synchrotron photons
generated by these electrons in the Earth's magnetic field. This
technique results in a substantial increase in the acceptance and
sensitivity of the apparatus compared to the traditional direct
detection of electrons. The instrument will consist of a 2m x 2m array
of BGO crystals. Simulation studies indicate that with an ultra-long
duration (100 day) flight, as many as 250 such electrons will be
detected with energies greater than 2 TeV, with an expected background
of only 1 event. A prototype instrument is currently being developed
and will be flown in 2005 on a conventional balloon. The full CREST
instrument will be flown in 2007 in Antarctica. This work is supported
by a grant from the National Aeronautics and Space Administration.
Title: Observation of M87 at 400 GeV with the Whipple 10 Meter
Telescope
Authors: Le Bohec, S.; Badran, H. M.; Bond, I. H.; Boyle, P. J.;
Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Catanese, M.;
Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.;
Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.;
Fortson, L. F.; Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders,
G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.;
Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman,
M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.;
Krennrich, F.; Lang, M. J.; Linton, E.; Lloyd-Evans, J.; Milovanovic,
A.; Moriarty, P.; Müller, D.; Nagai, T.; Nolan, S.; Ong, R. A.;
Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.;
Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter,
M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.;
Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J.
Bibcode: 2004ApJ...610..156L
Altcode:
We present results from observations taken with the Whipple 10 m
very high energy γ-ray telescope with maximal sensitivity at 400 GeV
during 39 hr between 2000 and 2003 in the direction of the giant radio
galaxy M87. Using the entire data set, we derive a 99% confidence level
upper limit on the flux of γ-ray emission above 400 GeV from M87 to
be <=6.9×10-12 cm-2 s-1. This
suggests variability at the 90% confidence level when compared to the
flux measured by the HEGRA collaboration in 1999 if the differential
spectrum is steeper than a power law of index 3.75. Our search for a
correlation between the Rossi X-Ray Timing Explorer all-sky monitor
observation and a potential γ-ray signal is inconclusive.
Title: TeV Gamma-Ray Observations of the Galactic Center
Authors: Kosack, K.; Badran, H. M.; Bond, I. H.; Boyle, P. J.;
Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Celik, O.;
Connaughton, V.; Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez,
I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.;
Fortson, L. F.; Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders,
G. H.; Grube, J.; Gutierrez, K.; Hall, J.; Hall, T. A.; Hanna, D.;
Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny,
G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Krawczynski,
H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans,
J.; Milovanovic, A.; McEnery, J.; Moriarty, P.; Muller, D.; Nagai,
T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney,
B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.;
Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson,
A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.;
Zweerink, J.
Bibcode: 2004ApJ...608L..97K
Altcode: 2004astro.ph..3422K
We report a possible detection of TeV gamma rays from the Galactic
center by the Whipple 10 m gamma-ray telescope. Twenty-six hours of data
were taken over an extended period from 1995 through 2003 resulting
in a total significance of 3.7 σ. The measured excess corresponds
to an integral flux of 1.6×10-8+/-0.5×10-8
(stat)+/-0.3×10-8 (sys) photons m-2
s-1 above an energy of 2.8 TeV, roughly 40% of the flux from
the Crab Nebula at this energy. The 95% confidence region has an angular
extent of about 15' and includes the position of Sgr A*. The detection
is consistent with a point source and shows no evidence of variability.
Title: A New Measurement of the Intensities of the Heavy Primary
Cosmic-Ray Nuclei around 1 TeV amu-1
Authors: Gahbauer, F.; Hermann, G.; Hörandel, J. R.; Müller, D.;
Radu, A. A.
Bibcode: 2004ApJ...607..333G
Altcode:
We describe a new measurement of the intensities of the heavy primary
cosmic-ray nuclei O, Ne, Mg, Si, and Fe from 10 GeV amu-1
to energies beyond 1 TeV amu-1. The measurement was conducted
in 1999 during a 1 day test flight of the Transition Radiation Array for
Cosmic Energetic Radiation (TRACER), a new cosmic-ray telescope designed
for long-duration balloon flights. TRACER uses an array of thin-walled
single-wire proportional tubes to determine the particle Lorentz factor
from measurements of specific ionization and transition radiation. The
nuclear charge is obtained with plastic scintillators, and low-energy
background is identified with an acrylic Cerenkov counter. The results
of this observation are consistent with previous measurements in this
energy region. The current statistical limitations should be greatly
improved with the planned long-duration exposure of TRACER.
Title: VERITAS: the Very Energetic Radiation Imaging Telescope
Array System
Authors: Krennrich, F.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.;
Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.;
D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.;
Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell,
S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.;
Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan,
M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.;
Kosack, K.; Krawczynski, H.; Lang, M. J.; LeBohec, S.; Linton, E.;
Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Müller, D.; Nagai,
T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney,
B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.;
Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson,
A.; Vassiliev, V. V.; Walker, G.; Wakely, S. P.; Weekes, T. C.;
Zweerink, J.
Bibcode: 2004NewAR..48..345K
Altcode:
The Very Energetic Radiation Imaging Telescope Array System (VERITAS)
is the major next generation imaging atmospheric Cherenkov γ-ray
telescope in the western hemisphere and will be located in southern
Arizona nearby Kitt Peak National Observatory. The VERITAS observatory
will provide unprecedented sensitivity to photon energies between 50
GeV and 50 TeV. The first stage is an array of four telescopes to be
fully operational in early 2006, with an expansion to seven telescopes
envisioned for 2008. The construction of a prototype telescope is
underway, for which first light is expected in Fall 2003. The technical
concept is outlined and a progress report is given.
Title: Energy Spectra and Charge Ratios of Atmospheric Muons
Authors: Minnick, S. A.; Beach, A. S.; Beatty, J. J.; Bhattacharyya,
A.; Bower, C. R.; Coutu, S.; Duvernois, M. A.; Labrador, A. W.;
McKee, S. P.; Muller, D.; Musser, J. A.; Nutter, S. L.; Schubnell,
M.; Swordy, S. P.; Tarle, G.; Tomasch, A. D.
Bibcode: 2004APS..OSS.B9001M
Altcode:
We present a new measurement of atmospheric muons made during an
ascent of the High Energy Antimatter Telescope balloon experiment. The
muon charge ratio μ^+/μ^- as a function of atmospheric depth in the
momentum interval 0.3--0.9 GeV/c is presented. The differential μ^-
fluxes in the 0.3--50 GeV/c range and for atmospheric depths between
4--960 g/cm^2 are also presented. We compare these results with other
measurements and model predictions.
Title: Constraints on the Very High Energy Emission from BL Lacertae
Objects
Authors: Horan, D.; Badran, H. M.; Bond, I. H.; Boyle, P. J.; Bradbury,
S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Catanese, M.; Celik, O.;
Cui, W.; Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.;
Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson,
L. F.; Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders, G. H.;
Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder,
J.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.;
Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.;
Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic,
A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.;
Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.;
Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter,
M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.;
Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J.
Bibcode: 2004ApJ...603...51H
Altcode: 2003astro.ph.11397H
We present results from observations of 29 BL Lacertae objects, taken
with the Whipple Observatory 10 m gamma-ray telescope between 1995 and
2000. The observed objects are mostly at low redshift (z<0.2), but
observations of objects of up to z=0.444 are also reported. Five of the
objects are EGRET sources and two are unconfirmed TeV sources. Three of
the confirmed sources of extragalactic TeV gamma rays were originally
observed as part of this survey and have been reported elsewhere. No
significant excesses are detected from any of the other objects
observed, on timescales of days, months, or years. We report 99.9%
confidence level flux upper limits for the objects for each observing
season. The flux upper limits are typically 20% of the Crab flux,
although for some sources, limits as sensitive as 6% of the Crab
flux were derived. The results are consistent with the synchrotron
self-Compton model predictions considered in this work.
Title: Thermal non-equilibrium in coronal loops: A road to complex
evolution
Authors: Müller, Daniel; de Groof, A.; Hansteen, V. H.; Peter, H.
Bibcode: 2004IAUS..223..289M
Altcode: 2005IAUS..223..289M
At high spatial and temporal resolution, coronal loops are observed to
have a highly dynamic nature. Recent observations with SOHO and TRACE
frequently show localized brightening "raining" down towards the solar
surface. What is the origin of these features? Here we present for
the first time a comparison of observed intensity enhancements from an
EIT shutterless campaign with non-equilibrium ionization simulations
of coronal loops in order to reveal the physical processes governing
fast flows and localized brightening. We show that catastrophic cooling
around the loop apex as a consequence of footpoint-concentrated heating
offers a simple explanation for these observations. An advantage of
this model is that no external driving mechanism is necessary as the
dynamics result entirely from the non-linear character of the system.
Title: Catastrophic Cooling and High-Speed Downflows in Solar
Coronal Loops
Authors: Müller, D.; Peter, H.; Hansteen, V.
Bibcode: 2004IAUS..219..765M
Altcode: 2003IAUS..219E..48M
We report numerical simulations of the condensation of plasma in
short solar coronal loops which has several interesting physical
consequences. Firstly we propose a connection between small cool loops
which presumably constitute the solar transition region and prominences
in the sense that the same physical mechanism governs their dynamics
namely the onset of instability and runaway cooling due to strong
radiative losses. Secondly we show that the temporal evolution of
these loop models exhibit a cyclic pattern of chromospheric evaporation
condensation formation motion of the condensation region to either side
of the loop and finally loop reheating with a period of 4000 - 6000
s for a loop of 10 Mm length. Thirdly we have synthesized transition
region lines from these simulations which show strong periodic intensity
variations making condensation processes in loops a candidate to
account for the observed temporal variability of these lines.
Title: Plasma Condensation in Solar Coronal Loops: II. "Catastrophic
Cooling" and High-Speed Downflows
Authors: Müller, D. A. N.; Peter, H.; Hansteen, V. H.
Bibcode: 2004ESASP.547..199M
Altcode: 2004soho...13..199M
The second part of this work focuses on the application of the
concept of plasma condensation to large coronal loops. In contrast
to the short loops analyzed in Müller et al. (2003a), these models
can more easily be compared to SOHO and TRACE observations. From our
numerical calculations of coronal loops we find several classes of
time-dependent solutions (static, periodic, irregular), depending on
the spatial dependence of a temporally constant energy deposition
in the loop. One of these classes is in remarkably close agreement
with the features observed with TRACE, described by Schrijver (2001):
Emission in C IV (154.8 nm), developing initially near the loop tops,
cool plasma sliding down on both sides of the loop, downflow velocities
of up to 100 km/s, and a downward acceleration which is substantially
reduced with respect to the solar surface gravity. Furthermore, these
results also offer an explanation for the observations of De Groof
et al. (2003a,b). In contrast to earlier models, we suggest that the
process of catastrophic cooling does not have to be initiated by a
drastic decrease of the loop heating. It can also result from a loss
of equilibrium at the loop apex which is a natural consequence if the
loop is heated predominantly at the footpoints, but constant in time.
Title: Catastrophic cooling in solar coronal loops : thermal
instability as a road to complex evolution
Authors: Müller, Daniel
Bibcode: 2004PhDT.......315M
Altcode:
No abstract at ADS
Title: Plasma Condensation in Solar Coronal Loops -- I. Basic
Processes
Authors: Müller, D. A. N.; Hansteen, V. H.; Peter, H.
Bibcode: 2004ESASP.547..285M
Altcode: 2004soho...13..285M
In the first part of this work, we report numerical calculations
of the condensation of plasma in short coronal loops, which has
several interesting physical consequences. We propose a connection
between small, cool loops, which presumably constitute the solar
transition region, and prominences in the sense that the same physical
mechanism governs their dynamics, namely the onset of instability
and runaway cooling due to strong radiative losses. We show that the
temporal evolution of these loop models exhibits a cyclic pattern of
chromospheric evaporation, condensation, motion of the condensation
region to either side of the loop, and finally loop reheating with
a period of 4000 - 8000 s for a loop of 10 Mm length. Furthermore,
we have synthesized transition region lines from these calculations
which show strong periodic intensity variations, making condensation
in loops a candidate to account for observed transient brightenings of
solar transition region lines. Remarkably, all these dynamic processes
take place for a heating function which is constant in time and has a
simple exponential height dependence. In the second part of this work
(Müller et al., 2003b), we apply this concept to large coronal loops.
Title: The deconvolution of the energy spectrum for the TRACER
experiment
Authors: Radu, A. A.; Müller, D.; Gahbauer, F.
Bibcode: 2004rac..conf..205R
Altcode:
TRACER (Transition Radiation Array for Cosmic Energetic Radiation) is
a large area detector built at the University of Chicago for direct
measurements of heavy cosmic ray nuclei up to about 10 TeV/amu. The
deconvolution of the energy spectra for different nuclei, from the
data collected by TRACER, is one component of our data analysis
efforts. Two methods used to estimate the spectra will be discussed
and the deconvoluted spectrum for iron will be presented.
Title: Search for High-Energy Gamma Rays from an X-Ray-selected
Blazar Sample
Authors: de la Calle Pérez, I.; Bond, I. H.; Boyle, P. J.; Bradbury,
S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Celik, O.; Cui, W.;
Dowdall, C.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.;
Finley, J. P.; Fortson, L.; Gaidos, J. A.; Gibbs, K.; Gammell,
S.; Hall, J.; Hall, T. A.; Hillas, A. M.; Holder, J.; Horan,
D.; Jordan, M.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.;
Kosack, K.; Krawczynski, H.; Krennrich, F.; LeBohec, S.; Linton,
E. T.; Lloyd-Evans, J.; Moriarty, P.; Müller, D.; Nagai, T. N.;
Ong, R. A.; Page, M.; Pallassini, R.; Petry, D.; Power-Mooney, B.;
Quinn, J.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter,
M.; Sembroski, G. H.; Swordy, S. P.; Vassiliev, V. V.; Wakely, S. P.;
Walker, G.; Weekes, T. C.
Bibcode: 2003ApJ...599..909D
Altcode: 2003astro.ph..9063D; 2003astro.ph..9063P
Our understanding of blazars has been greatly increased in recent years
by extensive multiwavelength observations, particularly in the radio,
X-ray, and gamma-ray regions. Over the past decade the Whipple 10
m telescope has contributed to this with the detection of five BL
Lacertae objects at very high gamma-ray energies. The combination
of multiwavelength data has shown that blazars follow a well-defined
sequence in terms of their broadband spectral properties. Together with
providing constraints on emission models, this information has yielded
a means by which potential sources of TeV emission may be identified
and predictions made as to their possible gamma-ray flux. We have
used the Whipple telescope to search for TeV gamma-ray emission from
eight objects selected from a list of such candidates. No evidence
has been found for very high energy emission from the objects in our
sample, and upper limits have been derived for the mean gamma-ray
flux above 390 GeV. These flux upper limits are compared with the
model predictions, and the implications of our results for future
observations are discussed.
Title: Dynamics of solar coronal loops. I. Condensation in cool
loops and its effect on transition region lines
Authors: Müller, D. A. N.; Hansteen, V. H.; Peter, H.
Bibcode: 2003A&A...411..605M
Altcode:
We report numerical calculations of the condensation of plasma
in short coronal loops, which have several interesting physical
consequences. Firstly, we propose a connection between small, cool
loops (T < 106 K), which constitute one of the basic
components of the solar transition region, and prominences, in the
sense that the same physical mechanism governs their dynamics: Namely
the onset of instability and runaway cooling due to strong radiative
losses. Secondly, we show that the temporal evolution of these
loop models exhibits a cyclic pattern of chromospheric evaporation,
condensation, motion of the condensation region to either side of the
loop, and finally loop reheating with a period of 4000-8000 s for a loop
of 10 Mm length. Thirdly, we have synthesized transition region lines
from these calculations which show strong periodic intensity variations,
making condensation in loops a candidate to account for observed
transient brightenings of solar transition region lines. Remarkably,
all these dynamic processes take place for a heating function which
is constant in time and has a simple exponential height dependence.
Title: The VERITAS Prototype
Authors: Wakely, S. P.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.;
Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.; D'Vali, M.; de la
Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.;
Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.; Gibbs, K.;
Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.;
Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny,
G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.;
Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.;
Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai,
T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney,
B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.;
Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson,
A.; Vassiliev, V. V.; Walker, G.; Weekes, T. C.; Zweerink, J.
Bibcode: 2003ICRC....5.2803W
Altcode: 2003ICRC...28.2803W
We give an up date on the status of the prototype telescope of the
Very Energetic Radiation Imaging telescope Array System (VERITAS), a
next-generation ˇ atmospheric imaging Cerenkov array currently under
construction in southern Arizona. VERITAS will feature significant
improvements over previous instruments, including better energy
resolution, lower energy threshold, improved an-
Title: Dynamics of Coronal loops: "Catastrophic Cooling" and
High-speed Downflows
Authors: Müller, D. A. N.; Hansteen, V. H.; Peter, H.
Bibcode: 2003ANS...324...13M
Altcode: 2003ANS...324..B09M
No abstract at ADS
Title: Measurement of the Cosmic-Ray Antiproton Energy Spectrum
with HEAT-pbar
Authors: Beach, A. S.; Beatty, J. J.; Bhattacharyya, A.; Bower, C. R.;
Coutu, S.; Duvernois, M. A.; Labrador, A. W.; McKee, S. P.; Minnick,
S. A.; Müller, D.; Musser, J. A.; Nutter, S.; Schubnell, M.; Swordy,
S. P.; Tarlé, G.; Tomasch, A. D.
Bibcode: 2003ICRC....4.1789B
Altcode: 2003ICRC...28.1789B; 2003ICRC....4.1789S
The absolute intensities of cosmic-ray antiprotons have been measured
in the energy range between 4.5 and 50 GeV. The data were obtained
by the HEAT-pbar instrument, a balloon borne superconducting magnet
spectrometer with precise rigidity and multiple energy loss measurement
capability. The instrument was flown in the Spring 2000 from Ft. Sumner,
NM, at an average atmospheric depth of 7.2 g /cm2 . Here we briefly
describe the instrument and the measurement and outline the analysis
of the data which is still ongoing at this time. We will present the
result of our analysis and discuss the implications for cosmic-ray
propagation models at the conference.
Title: Energy Spectra and Charge Ratios of Atmospheric Muons
Authors: Minnick, S. A.; Beach, A. S.; Beatty, J. J.; Bhattacharyya,
A.; Bower, C. R.; Coutu, S.; Duvernois, M. A.; Labrador, A. W.; McKee,
S. P.; Mueller, D.; Musser, J. A.; Nutter, S. L.; Schnubnell, M.;
Swordy, S. P.; Tarle, G.; Tomasch, A. D.
Bibcode: 2003ICRC....3.1191M
Altcode: 2003ICRC...28.1191M
We present a new measurement of atmospheric muons made during an
ascent of the High Energy Antimatter telescope balloon experiment. The
muon charge ratio µ+ /µ- as a function of atmospheric depth in the
momentum interval 0.3-0.9 GeV/c is presented. The differential µ-
fluxes in the 0.3-50 GeV/c range and for atmospheric depths between
4-960 g/cm2 are also presented. We compare these results with other
measurements and model predictions.
Title: Transition Radiation Detectors for Cosmic Rays near the Knee
Authors: Wakely, S. P.; Gahbauer, F. H.; Hoerandel, J. R.; Mueller,
D.; Plewnia, S.
Bibcode: 2003ICRC....4.2237W
Altcode: 2003ICRC...28.2237W
Precise observations of the energy spectra and relative abundances of
cosmic-ray nuclei require instruments that exhibit individual charge
resolution and a calibrated energy response. If energies up to ∼ 1015
eV are to be covered, the low intensity of the heavier nuclei (Z ² 3)
also mandates detector areas of several square meters. X-ray transition
radiation detectors (TRDs) appear to provide the only practical means
of fulfilling all of these requirements for balloon or space-b orne
instruments. However, for measurements up to the cosmic-ray "knee",
care must be taken that the energy response of the TRD does not
saturate for Lorentz factors less than ∼ 105 . We have designed
detectors to meet this goal, and have successfully tested prototypes at
an accelerator beam at CERN. We shall present and discuss the results
of these measurements.
Title: Observation of M87 with the Whipple 10m Telescope
Authors: LeBohec, S.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.;
Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.;
D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.;
Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell,
S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.;
Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan,
M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.;
Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Linton, E.;
Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai,
T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney,
B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.;
Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson,
A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.;
Zweerink, J.
Bibcode: 2003ICRC....5.2627L
Altcode: 2003astro.ph..5582L; 2003ICRC...28.2627L
The Whipple 10-m telescope was used to observe M87 since 2000. No
significant gamma-ray signal was found and upper limits compared to
the HEGRA detection suggest the source may be variable. We found weak
evidence for a correlation with the X-ray activity in 2000-2001 but
this tendency did not persist in 2002-2003.
Title: VHE Observations of BL Lacertae Objects: 1995-2000
Authors: Horan, D.; Catanese, M. A.; Bond, I. H.; Boyle, P. J.;
Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.;
Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.;
Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.;
Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall,
T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Jarvis, A.; Jordan, M.;
Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack,
K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton,
E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai,
T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney,
B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.;
Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson,
A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.;
Zweerink, J.
Bibcode: 2003ICRC....5.2567H
Altcode: 2003ICRC...28.2567H
The results of observations of 29 BL Lacertae objects taken with the
Whipple Observatory 10 m gamma-ray telescope between 1995 and 2000
are presented.
Title: Whipple Observations of 1ES1959+650: An Update
Authors: Holder, J.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.;
Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.;
D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.;
Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell,
S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.;
Hanna, D.; Hillas, A. M.; Horan, D.; Jarvis, A.; Jordan, M.; Kenny,
G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.;
Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.;
Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai,
T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney,
B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.;
Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson,
A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.;
Zweerink, J.
Bibcode: 2003ICRC....5.2619H
Altcode: 2003astro.ph..5577H; 2003ICRC...28.2619H
Strong flares of TeV gamma-ray emission up to a level of ∼ 5 Crab
were ˇ detected by the Whipple 10 m atmospheric Cerenkov telescope
from the BL Lacertae object 1ES1959+650 during May July 2002. We report
here the results of follow up observations during 2002 2003.
Title: Search for a WIMP Annihilation Signature in the Core of the
Globular Cluster M15
Authors: LeBohec, S.; Baltz, E. A.; Bond, I. H.; Boyle, P. J.;
Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.;
Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.;
Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos,
J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.;
Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis,
A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.;
Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.;
Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller,
D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.;
Power-Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.;
Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy,
S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes,
T. C.; Zweerink, J.
Bibcode: 2003ICRC....4.2521L
Altcode: 2003ICRC...28.2521L; 2003astro.ph..5581L
The Whipple 10m Very High Energy gamma-ray telescope has been used to
search for indications of WIMP annihilation in the direction of the
globular cluster M15. The upper limits derived constrain the amount
of super-symmetric dark matter that may reside in globular clusters.
Title: Condensation in Cool Coronal Loops and its Effect on Transition
Region Lines
Authors: Müller, D. A. N.; Hansteen, V. H.; Peter, H.
Bibcode: 2003ANS...324..108M
Altcode: 2003ANS...324..P14M
No abstract at ADS
Title: Whipple Telescope Observations of Potential TeV Gamma-Ray
Sources Found by the Tibet Air Shower Array
Authors: Walker, G.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.;
Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.;
D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.;
Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.;
Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna,
D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.;
Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack,
K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton,
E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai,
T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney,
B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.;
Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson,
A.; Vassiliev, V. V.; Wakely, S. P.; Weekes, T. C.; Zweerink, J.
Bibcode: 2003ICRC....5.2563W
Altcode: 2003ICRC...28.2563W
An all-sky survey performed with the Tibet Air Shower Array (Tib et AS)
has found a number of potential point sources of TeV gamma rays. If they
are steady sources, the implied Tibet AS fluxes should be visible with
strong significance to the Whipple 10-m gamma-ray telescope (E >
400 GeV) with only a short (5 hour) exposure. We have observed four
candidate directions from the Tibet-I I HD dataset for ∼5 hours each
with the Whipple telescope. In addition, we observed a new candidate
direction from the Tibet-I I I Phase 1 dataset for 7.5 hours. We have
found no corresponding excesses at the flux levels implied, and we
have set upper limits for each candidate.
Title: Energy Spectra and Relative Abundances of Heavy Cosmic-Ray
Nuclei around 1 TeV/Nucleon
Authors: Muller, D.; Gahbauer, F.; Hermann, G.; Hoerandel, J.; Radu,
A. A.
Bibcode: 2003ICRC....4.1873M
Altcode: 2003ICRC...28.1873M
We describe a measurement of the intensities of heavy primary cosmicray
nuclei with the Transition Radiation Array for Cosmic Energetic
Radiation (TRACER) up to energies around a few TeV/nucleon. Absolute
cosmic-ray fluxes are presented for O, Ne, Mg, Si, and Fe obtained
during a one-day test flight from Ft. Sumner, NM in preparation for a
20-day circum-p olar balloon flight. The results of TRACER are largely
consistent with previous observations in this energy range. Introduction
Direct measurements of the elemental composition and energy spectra
of cosmic-ray nuclei at high energies, beyond a TeV/nucleon, and
approaching the cosmic-ray knee above total energies of 1015 eV, are
expected to provide a sensitive test of the current paradigm that
all cosmic rays are generated with the same energy spectrum at the
source, up to a maximum rigidity around 1014 V for shock acceleration
in supernova remnants, and that their propagation pathlength through
the galaxy decreases with increasing energy. However, new observational
data are slow in coming because the low particle intensity necessitates
long exposures of very large-area instruments. With this need in mind,
TRACER was constructed for a long-duration balloon flight. A successful
30-hour test flight was conducted from Ft. Sumner, NM, in September
1999. A subsequent long-duration balloon flight along the Northern Polar
circle could not be accomplished due to lack of required international
agreements. The instrument is currently scheduled for a long-duration
flight in Antarctica in 2003/4. This report will present and discuss
results obtained with the 1999 test flight. The Instrument Figure 1
shows the detector arrangement. The main elements are (a) plas-
Title: Hourly Spectral Variability of Mrk 421
Authors: Krennrich, F.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.;
Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.;
D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.;
Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell, S.;
Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna,
D.; Hillas, A. M.; Holder, J.; Horan, D.; Jarvis, A.; Jordan, M.;
Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack,
K.; Krawczynski, H.; Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans,
J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.;
Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.;
Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.;
Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson, A.; Vassiliev,
V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J.
Bibcode: 2003ICRC....5.2603K
Altcode: 2003ICRC...28.2603K; 2003astro.ph..5419K
Mrk 421 is the first TeV blazar found to exhibit significant spectral
variability during strong flaring activity, showing hardening of the
TeV spectrum in high emission states. Mrk 421 is also known to exhibit
flux variability on time scales as short as 15 minutes. In this paper
we present studies of hourly spectral variability of Mrk 421 in 2001
using data from the Whipple Observatory 10 m gamma-ray telescope.
Title: Precise Identification of Heavy Cosmic-Ray Nuclei: The Role
of Delta Rays
Authors: Gahbauer, F.; Hermann, G.; Hörandel, J.; Müller, D.; Radu,
A. A.
Bibcode: 2003ICRC....4.2245G
Altcode: 2003ICRC...28.2245G; 2003ICRC....4.2245M
Relativistic δ rays may lead to detector response functions, both
in charge and energy, which are different from those expected for
unaccompanied particles. These effects are particularly noticable for
cosmic ray nuclei with large charge number, Z . We shall demonstrate
some of these features with balloon-b orne data obtained with the
TRACER instrument, and compare the measurement with Monte Carlo
calculations. Our results illustrate how δ -ray effects can lead to
false charge assignments or acceptance efficiencies if not properly
taken into account, but also how they can be helpful in extending the
energy response of some of the counter elements.
Title: Observations of Starburst Galaxies
Authors: Nagai, T.; Vassiliev, V. V.; Bond, I. H.; Boyle, P. J.;
Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.;
Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.;
Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos,
J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.;
Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Jarvis, A.; Jordan,
M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.;
Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.;
Linton, E.; Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller,
D.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney,
B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.;
Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson,
A.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J.
Bibcode: 2003ICRC....5.2635N
Altcode: 2003ICRC...28.2635N
The search for TeV gamma-ray radiation from starburst galaxies (SBGs)
has been conducted by the Whipple 10-m gamma-ray telescope from
January 2001 to March 2003. The regions with high star formation rates
(SFRs) observed in SBGs are frequently accompanied by high density
clouds of interstellar matter (ISM). This seems to create nearly
perfect conditions for generating diffuse gamma-ray radiation as high
energy cosmic rays interact with the ISM. If the current paradigm that
supernovae are the origin of high energy cosmic rays is valid, then star
forming regions rich in type Ib/c, I I supernovae may become the lab
oratories to test the hypothesis. Using the Whipple telescope we have
conducted a survey of several plausible SBGs selected based on their
distance, density of gas clouds, age of star forming regions, SFRs,
and magnetic fields, as well as the presence of radio flux and X-ray
point sources. We discuss the selection criteria based on gamma-ray
flux estimates, as well as the results of a novel spectrum dependent
analysis (to be reported during presentation) of SBG observations for
which a total exposure of 10-30 hours per source have been accumulated.
Title: Intensive TeV Gamma-Ray and X-Ray Observations of the Blazar
Mrk 421 in December 2002 and January 2003
Authors: Rebillot, P. F.; Hughes, S. B.; Bond, I. H.; Boyle, P. J.;
Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.;
Daniel, M.; D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone,
A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.;
Gaidos, J.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.;
Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan,
D.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.;
Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.;
Lang, M. J.; LeBohec, S.; Linton, E.; Lloyd-Evans, J.; Milovanovic,
A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.;
Pallassini, R.; Petry, D.; Power-Mooney, B.; Quinn, J.; Quinn, M.;
Ragan, K.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski,
G.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker,
G.; Weekes, T. C.; Zweerink, J.
Bibcode: 2003ICRC....5.2599R
Altcode: 2003ICRC...28.2599R; 2003astro.ph..5583R
We report on observations of Markarian 421 made with the Whipple 10m
ˇ erenkov telescope and the RXTE satellite during a multi-wavelength
campaign C in December 2002 and January 2003, initiated by a Whipple
target of opportunity. The observations revealed several flares with
flux levels between 1 and 2 times the flux of the Crab Nebula. We
will discuss the temporal properties, including evidence of X-ray/TeV
gamma-ray flux correlation.
Title: Observations of H1426+428 from 1999 to 2002 with the Whipple
Observatory 10 m Telescope
Authors: Horan, D.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.;
Buckley, J. H.; Carter-Lewis, D.; Celik, O.; Cui, W.; Daniel, M.;
D'Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.;
Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J.; Gammell,
S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.;
Hanna, D.; Hillas, A. M.; Holder, J.; Jarvis, A.; Jordan, M.; Kenny,
G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.;
Krawczynski, H.; Krennrich, F.; Lang, M. J.; LeBohec, S.; Linton, E.;
Lloyd-Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai,
T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power-Mooney,
B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.;
Rose, H. J.; Schroedter, M.; Sembroski, G.; Swordy, S. P.; Syson,
A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.;
Zweerink, J.
Bibcode: 2003ICRC....5.2647H
Altcode: 2003ICRC...28.2647H; 2003astro.ph..5579H
The BL Lacertae object H1426+428 is the most distant, confirmed
source of TeV gamma rays. At a redshift of 0.129, its detection at TeV
energies has important implications for estimating the density of the
extragalactic infra-red background radiation. H1426+428 was observed
extensively during the 2001/2002 observing season with the Whipple 10
m gamma-ray telescope. The results of these observations are presented
here and are combined with the results of previous observations made
between 1999 and 2001 at Whipple.
Title: Antimatter Measurements with Heat and the Dark Matter
Connection
Authors: Coutu, S.; Beach, A. S.; Beatty, J. J.; Minnick, S.; Labrador,
A.; Müller, D.; Swordy, S.; Bower, C.; Musser, J.; McKee, S.;
Schubnell, M.; Tarlé, G.; Tomasch, A.; Duvernois, M. A.; Nutter, S. L.
Bibcode: 2003idm..conf..483C
Altcode:
The High Energy Antimatter Telescope is a magnet spectrometer
complemented by an array of particle detectors, flown on high
altitude balloons. With it, we have measured the positron content
of the cosmic-ray flux at energies between 1 and 50 GeV, and the
antiproton content from 4 to 50 GeV. We have found both antiparticle
species to be substantially in agreement with models of secondary
antimatter production in interstellar collisions of hadronic cosmic
rays. The positron measurements however seem to consistently indicate
the possibility of a small primary antimatter component. Just such
a contribution has been predicted to result from the annihilation of
dark matter particles in the galactic halo. The HEAT measurements are
described here, and their connection with SUSY dark matter is explored.
Title: The energy spectrum of cosmic-ray protons and helium near
100 GeV
Authors: Diehl, E.; Ellithorpe, D.; Müller, D.; Swordy, S. P.
Bibcode: 2003APh....18..487D
Altcode:
A large ring-imaging Čerenkov telescope (RICH-II) was flown on a high
altitude balloon from Fort Sumner, New Mexico, USA in October 1997. This
instrument is designed to determine the energy spectra of light
cosmic-ray nuclei over the energy range 30-150 GeV/n through a precise
measurement of the angle of Čerenkov emission from each particle. We
give details about the design and performance of the instrument and
present results on the absolute intensity of cosmic-ray protons and
helium nuclei. The observed ratio of proton to helium intensities does
not change significantly over this energy range. We also find that the
abundances of protons and helium nuclei at 100 GeV/n at the cosmic-ray
source relative to elemental galactic abundances are much smaller than
those of other elements with comparable first ionization potential.
Title: Search for TeV Emissions from Pulsars in Binary Systems
Authors: Hall, T. A.; Bond, I. H.; Bradbury, S. M.; Buckley,
J. H.; Carson, M. J.; Carter-Lewis, D. A.; Catanese, M.; Dunlea, S.;
D'Vali, M.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Gaidos, J. A.;
Gillanders, G. H.; Hillas, A. M.; Horan, D.; Kertzman, M.; Kieda,
D.; Kildea, J.; Knapp, J.; Krennrich, F.; Lang, M. J.; LeBohec, S.;
Lessard, R.; Lloyd-Evans, J.; McKernan, B.; Moriarty, P.; Muller, D.;
Ong, R.; Quinn, J.; Reynolds, P. T.; Rose, H. J.; Sembroski, G. H.;
Swordy, S. P.; Vassiliev, V. V.; Weekes, T. C.
Bibcode: 2003ApJ...583..853H
Altcode:
A survey of binary systems containing pulsars was conducted, with
the intention of detecting Galactic sources of very high energy
γ-ray emission. Observations were carried out with the Whipple
10 m imaging atmospheric Cerenkov telescope. Standard analysis
techniques were applied to these sources to search for steady,
unpulsed emission. Periodic tests were also performed to search for
emission correlated with both the orbital and spin phases, where
appropriate. Analyses indicate that the binaries in this study do
not emit detectable levels of very high energy photons within the
sensitivity of our instrument. The flux upper limits presented here
fail to seriously constrain emission models.
Title: Detection of TeV Gamma Rays from the BL Lacertae Object 1ES
1959+650 with the Whipple 10 Meter Telescope
Authors: Holder, J.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.;
Buckley, J. H.; Carter-Lewis, D. A.; Cui, W.; Dowdall, C.; Duke,
C.; de la Calle Perez, I.; Falcone, A.; Fegan, D. J.; Fegan, S. J.;
Finley, J. P.; Fortson, L.; Gaidos, J. A.; Gibbs, K.; Gammell, S.;
Hall, J.; Hall, T. A.; Hillas, A. M.; Horan, D.; Jordan, M.; Kertzman,
M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.;
Krennrich, F.; LeBohec, S.; Linton, E. T.; Lloyd-Evans, J.; Moriarty,
P.; Müller, D.; Nagai, T. N.; Ong, R.; Page, M.; Pallassini, R.;
Petry, D.; Power-Mooney, B.; Quinn, J.; Rebillot, P.; Reynolds,
P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.;
Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.
Bibcode: 2003ApJ...583L...9H
Altcode: 2002astro.ph.12170H
We present the first strong detection of very high energy γ-rays
from the close (z=0.048) X-ray-selected BL Lacertae object 1ES
1959+650. Observations were made with the Whipple 10 m telescope
on Mount Hopkins, Arizona, using the atmospheric Cerenkov imaging
technique. The flux between 2002 May and July was highly variable,
with a mean of 0.64+/-0.03 times the steady flux from the Crab Nebula
and reaching a maximum of 5 crab, with variability on timescales as
short as 7 hr.
Title: Recent Results from the VERITAS Collaboration
Authors: Krennrich, F.; Bond, I. H.; Bradbury, S. M.; Buckley, J. H.;
Carter-Lewis, D. A.; Cui, W.; de la Calle Perez, I.; Falcone, A.;
Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Gaidos, J. A.; Gibbs, K.;
Gillanders, G. H.; Hall, T. A.; Hillas, A. M.; Holder, J.; Horan, D.;
Jordan, M.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack,
K.; Lang, M. J.; LeBohec, S.; Moriarty, P.; Muller, D.; Ong, R. A.;
Pallassini, R.; Petry, D.; Quinn, J.; Reynolds, P. T.; Rose, H. J.;
Sembroski, G. H.; Swordy, S. P.; Vassiliev, V. V.; Wakely, S. P.;
Weekes, T. C.
Bibcode: 2002astro.ph.12269K
Altcode:
A decade after the discovery of TeV gamma-rays from the blazar Mrk 421
(Punch et al. 1992), the list of TeV blazars has increased to five
BL Lac objects: Mrk 421 (Punch et al. 1992; Petry et al. 1996; Piron
et al. 2001), Mrk 501 (Quinn et al. 1996; Aharonian et al. 1999;
Djannati-Atai et al. 1999), 1ES2344+514 (Catanese et al. 1998),
H1426+428 (Horan et al. 2000, 2002; Aharonian et al. 2002; Djannati-Atai
et al. 2002) and 1ES1959+650 (Nishiyama et al. 1999; Konopelko et
al. 2002; Holder et al. 2002). In this paper we report results from
recent observations of Mrk 421, H1426+428 and 1ES1959+650 using the
Whipple Observatory 10 m telescope.
Title: The TeV Spectrum of H1426+428
Authors: Petry, D.; Bond, I. H.; Bradbury, S. M.; Buckley, J. H.;
Carter-Lewis, D. A.; Cui, W.; Duke, C.; de la Calle Perez, I.; Falcone,
A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Gaidos, J. A.; Gibbs,
K.; Gammell, S.; Hall, J.; Hall, T. A.; Hillas, A. M.; Holder, J.;
Horan, D.; Jordan, M.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp,
J.; Kosack, K.; Krennrich, F.; LeBohec, S.; Moriarty, P.; Müller,
D.; Nagai, T. N.; Ong, R.; Page, M.; Pallassini, R.; Power-Mooney, B.;
Quinn, J.; Reay, N. W.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.;
Sembroski, G. H.; Sidwell, R.; Stanton, N.; Swordy, S. P.; Vassiliev,
V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.
Bibcode: 2002ApJ...580..104P
Altcode: 2002astro.ph..7506P
The BL Lac object H1426+428 was recently detected as a high-energy
γ-ray source by the VERITAS collaboration (Horan et al.). We have
reanalyzed the 2001 portion of the data used in the detection
in order to examine the spectrum of H1426+428 above 250 GeV. We
find that the time-averaged spectrum agrees with a power law
of the shape(dF/dE)(E)=10-7.31+/-0.15stat+/-
0.16systE-3.50+/-0.35stat+/-
0.05systm-2s-1TeV-
1.The statistical evidence from our data for emission above
2.5 TeV is 2.6 σ. At the 95% confidence level, the integral flux
of H1426+428 above 2.5 TeV is larger than 3% of the corresponding
flux from the Crab Nebula. The spectrum is consistent with the
(noncontemporaneous) measurement by Aharonian et al. both in shape
and in normalization. Below 800 GeV, the data clearly favor a spectrum
steeper than that of any other TeV blazar observed so far, indicating
a difference in the processes involved either at the source or in the
intervening space.
Title: Casimir energy in multiply connected static hyperbolic
universes
Authors: Müller, Daniel; Fagundes, Helio V.; Opher, Reuven
Bibcode: 2002PhRvD..66h3507M
Altcode: 2002gr.qc.....9103M
We generalize a previously obtained result for the case of a few other
static hyperbolic universes with manifolds of nontrivial topology as
spatial sections.
Title: Spectral signature of magnetic flux tubes in sunspot penumbrae
Authors: Müller, D. A. N.; Schlichenmaier, R.; Steiner, O.; Stix, M.
Bibcode: 2002A&A...393..305M
Altcode:
We study the polarization of spectral lines in the penumbra by
integrating the radiative transfer equation of polarized light for a
three-dimensional model atmosphere of a sunspot. In this model, the
Evershed flow is confined to magnetic flux tubes which are embedded
in a static background atmosphere, in accordance with the moving tube
model of Schlichenmaier et al. (\cite{Schlichenmaier1998apjl},b). The
gradients and/or discontinuities in the fluid velocity and the
magnetic field at the flux tube boundaries give rise to asymmetric
Stokes profiles. We concentrate on the Stokes-V profiles and study the
net circular polarization (NCP) of two photospheric spectral lines of
neutral iron, Fe I 630.25 nm and Fe I 1564.8 nm. The different behavior
of these two lines, which are exemplary for atomic spectral lines with
a large Landé factor and significantly different wavelength, is based
on the difference in excitation potential of the corresponding atomic
transitions and the fact that the wavelength dependence of the Doppler
shift is linear, while that of the Zeeman splitting is quadratic. We
find that the azimuthal variation of the NCP, N(psi, is a predominantly
antisymmetric function of psi with respect to the line connecting
disk center and spot center (line-of-symmetry) for the infrared line
of Fe I 1564.8 nm, while the variation is predominantly symmetric for
Fe I 630.25 nm. We show that the antisymmetric variation is caused
by anomalous dispersion (Faraday pulsation) and the discontinuity
in the azimuthal angle of the magnetic field, which is due to the
relative inclination between flux tube and background field. We
then compute synthetic NCP maps of a sunspot and compare them with
observational results. Finally, the center-to-limb variation of the
NCP, N(theta ), of these spectral lines is investigated. We show
that the location of the zero-crossing point of N(theta ) on the
center side of the line-of-symmetry represents a diagnostic tool to
determine the inclination angle of the Evershed flow: A vanishing NCP
on the center-side of the line-of-symmetry is an indirect evidence of
downflows in the penumbra.
Title: The composition of cosmic rays at the knee
Authors: Swordy, S. P.; Fortson, L. F.; Hinton, J.; Hörandel, J.;
Knapp, J.; Pryke, C. L.; Shibata, T.; Wakely, S. P.; Cao, Z.; Cherry,
M. L.; Coutu, S.; Cronin, J.; Engel, R.; Fowler, J. W.; Kampert,
K. -H.; Kettler, J.; Kieda, D. B.; Matthews, J.; Minnick, S. A.;
Moiseev, A.; Muller, D.; Roth, M.; Sill, A.; Spiczak, G.
Bibcode: 2002APh....18..129S
Altcode: 2002astro.ph..2159S
The observation of a small change in spectral slope, or 'knee'
in the fluxes of cosmic rays near energies 10 15 eV has
caused much speculation since its discovery over 40 years ago. The
origin of this feature remains unknown. A small workshop to review
some modern experimental measurements of this region was held at the
Adler Planetarium in Chicago, USA in June 2000. This paper summarizes
the results presented at this workshop and the discussion of their
interpretation in the context of hadronic models of atmospheric air
showers.
Title: Discovery of Spectral Variability of Markarian 421 at TeV
Energies
Authors: Krennrich, F.; Bond, I. H.; Bradbury, S. M.; Buckley, J. H.;
Carter-Lewis, D. A.; Cui, W.; de la Calle Perez, I.; Fegan, D. J.;
Fegan, S. J.; Finley, J. P.; Gaidos, J. A.; Gibbs, K.; Gillanders,
G. H.; Hall, T. A.; Hillas, A. M.; Holder, J.; Horan, D.; Jordan,
M.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Lang,
M. J.; LeBohec, S.; Moriarty, P.; Müller, D.; Ong, R. A.; Pallassini,
R.; Petry, D.; Quinn, J.; Reay, N. W.; Reynolds, P. T.; Rose, H. J.;
Sembroski, G. H.; Sidwell, R.; Stanton, N.; Swordy, S. P.; Vassiliev,
V. V.; Wakely, S. P.; Weekes, T. C.
Bibcode: 2002ApJ...575L...9K
Altcode: 2002astro.ph..7184K
The detection of spectral variability of the γ-ray blazar Mrk 421 at
TeV energies is reported. Observations with the Whipple Observatory
10 m γ-ray telescope taken in 2000/2001 revealed exceptionally strong
and long-lasting flaring activity. Flaring levels of 0.4-13 times that
of the Crab Nebula flux provided sufficient statistics for a detailed
study of the energy spectrum between 380 GeV and 8.2 TeV as a function
of the flux level. These spectra are well described by a power law with
an exponential cutoff: dN/dE~E-αe-E/E0
m-2 s-1 TeV-1. There is no evidence for
variation in the cutoff energy with flux, and all spectra are consistent
with an average value for the cutoff energy of 4.3 TeV. The spectral
index varies between 1.89+/-0.04stat+/-0.05syst in
a high flux state and 2.72+/-0.11stat+/-0.05syst
in a low state. The correlation between spectral index and flux is tight
when averaging over the total 2000/2001 data set. Spectral measurements
of Mrk 421 from previous years (1995/1996 and 1999) by the Whipple
collaboration are consistent with this flux-spectral index correlation,
which suggests that this may be a constant or a long-term property of
the source. If a similar flux-spectral index correlation were found for
other γ-ray blazars, this universal property could help disentangle
the intrinsic emission mechanism from external absorption effects.
Title: Net circular polarization of sunspot penumbrae - symmetry
breaking by anomalous dispersion
Authors: Müller, D. A. N.; Schlichenmaier, R.; Steiner, O.; Stix, M.
Bibcode: 2002ESASP.508..141M
Altcode: 2002soho...11..141M
We examine the polarization of spectral lines in the penumbra of
sunspots by solving the radiative transfer equation of polarized
light for a three-dimensional axially symmetric model atmosphere
of a sunspot. The Evershed flow is confined to horizontal magnetic
flux tubes obtained from MHD calculations. These are embedded in
an inclined background magnetic field. In this work, we concentrate
on the Stokes-V profiles and examine the net circular polarization
(NCP), N = ∫V(λ)dλ, of two photospheric spectral lines of neutral
iron, Fe I 630.25 nm and Fe I 1564.8 nm. Analyzing spectra at a fixed
distance from the spot center, we find that the azimuthal variation
of N, N(ψ), is an antisymmetric function of ψ w.r.t. to the line
connecting disk center and spot center for Fe I 1564.8 nm, while
the variation is predominantly symmetric for Fe I 630.25 nm. We show
that the antisymmetric variation is caused by anomalous dispersion
(rotation of the polarization vector in a magnetized plasma). The
different inclination angles lead to a discontinuity in the azimuth
of the magnetic field along the line-of-sight. We show that this
discontinuity together with the effect of anomalous dispersion produced
an antisymmetric component in N(ψ) which outweighs the symmetric
component from the discontinuity for Fe I 1564.8 nm, while it is
negligible for Fe I 630.25 nm. We finally compute synthetic NCP maps of
a sunspot which offer an explanation for recent observational results.
Title: Detection of the BL Lacertae Object H1426+428 at TeV Gamma-Ray
Energies
Authors: Horan, D.; Badran, H. M.; Bond, I. H.; Bradbury, S. M.;
Buckley, J. H.; Carson, M. J.; Carter-Lewis, D. A.; Catanese, M.;
Cui, W.; Dunlea, S.; Das, D.; de la Calle Perez, I.; D'Vali, M.;
Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Gaidos, J. A.; Gibbs, K.;
Gillanders, G. H.; Hall, T. A.; Hillas, A. M.; Holder, J.; Jordan, M.;
Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krennrich,
F.; Lang, M. J.; LeBohec, S.; Lessard, R.; Lloyd-Evans, J.; McKernan,
B.; Moriarty, P.; Muller, D.; Ong, R.; Pallassini, R.; Petry, D.;
Quinn, J.; Reay, N. W.; Reynolds, P. T.; Rose, H. J.; Sembroski,
G. H.; Sidwell, R.; Stanton, N.; Swordy, S. P.; Vassiliev, V. V.;
Wakely, S. P.; Weekes, T. C.
Bibcode: 2002ApJ...571..753H
Altcode: 2002astro.ph..2185H
A very high energy γ-ray signal has been detected at the 5.5 σ
level from H1426+428, an X-ray-selected BL Lacertae object at a
redshift of 0.129. The object was monitored from 1995 to 1998 with
the Whipple 10 m imaging atmospheric Cerenkov telescope as part of a
general blazar survey; the results of these observations, although
not statistically significant, were consistently positive. X-ray
observations of H1426+428 during 1999 with the BeppoSAX instrument
revealed that the peak of its synchrotron spectrum occurs at greater
than 100 keV, leading to the prediction of observable TeV emission
from this object. H1426+428 was monitored extensively at the Whipple
Observatory during the 1999, 2000, and 2001 observing seasons. The
strongest TeV signals were detected in 2000 and 2001. During 2001,
an integral flux of 2.04+/-0.35×10-11 cm-2
s-1 above 280 GeV was recorded from H1426+428. The detection
of H1426+428 supports the idea that, as also seen in Mrk 501 and 1ES
2344+514, BL Lacertae objects with extremely high synchrotron peak
frequencies produce γ-rays in the TeV range.
Title: VERITAS: the Very Energetic Radiation Imaging Telescope
Array System
Authors: Weekes, T. C.; Badran, H.; Biller, S. D.; Bond, I.; Bradbury,
S.; Buckley, J.; Carter-Lewis, D.; Catanese, M.; Criswell, S.; Cui,
W.; Dowkontt, P.; Duke, C.; Fegan, D. J.; Finley, J.; Fortson, L.;
Gaidos, J.; Gillanders, G. H.; Grindlay, J.; Hall, T. A.; Harris,
K.; Hillas, A. M.; Kaaret, P.; Kertzman, M.; Kieda, D.; Krennrich,
F.; Lang, M. J.; LeBohec, S.; Lessard, R.; Lloyd-Evans, J.; Knapp,
J.; McKernan, B.; McEnery, J.; Moriarty, P.; Muller, D.; Ogden, P.;
Ong, R.; Petry, D.; Quinn, J.; Reay, N. W.; Reynolds, P. T.; Rose,
J.; Salamon, M.; Sembroski, G.; Sidwell, R.; Slane, P.; Stanton, N.;
Swordy, S. P.; Vassiliev, V. V.; Wakely, S. P.
Bibcode: 2002APh....17..221W
Altcode: 2001astro.ph..8478W
The Very Energetic Radiation Imaging Telescope Array System
(VERITAS) represents an important step forward in the study of extreme
astrophysical processes in the universe. It combines the power of the
atmospheric Cherenkov imaging technique using a large optical reflector
with the power of stereoscopic observatories using arrays of separated
telescopes looking at the same shower. The seven identical telescopes in
VERITAS, each of aperture 10 m, will be deployed in a filled hexagonal
pattern of side 80 m; each telescope will have a camera consisting of
499 pixels with a field of view of 3.5°. VERITAS will substantially
increase the catalog of very high energy ( E>100 GeV) γ-ray sources
and greatly improve measurements of established sources.
Title: Cosmic ray composition near the knee: the TRACER project and
prospects for future developments
Authors: Muller, D.
Bibcode: 2002cosp...34E1436M
Altcode: 2002cosp.meetE1436M
Precise measurements of the elemental composition of cosmic rays up
to energies around the spectral knee above 10E15 eV are of critical
importance for the understanding of the acceleration and galactic
confinement of cosmic rays. Such measurements require detectors
with very large exposure factors above the atmosphere, as may be
achieved with transition radiation detectors for the nuclei heavier
than protons and helium. We shall describe the TRACER instrument
("Transition Radiation Array for Cosmic Energetic Radiation") that
has been developed for measurements in circumpolar, long-duration
balloon flights. We shall discuss the performance of TRACER, based
on accelerator calibrations and on a one-day test flight on balloon,
and we shall report on the planned long-duration flights. Finally,
we will review the potential of the transition radiation technique
for the development of future LDB and ULDB payloads.
Title: Casimir Energy Density in Closed Hyperbolic Universes
Authors: Müller, Daniel; Fagundes, Helio V.
Bibcode: 2002IJMPA..17.4385M
Altcode: 2002gr.qc.....5050M
The original Casimir effect results from the difference in the vacuum
energies of the electromagnetic field, between that in a region of
space with boundary conditions and that in the same region without
boundary conditions. In this paper we develop the theory of a similar
situation, involving a scalar field in spacetimes with closed spatial
sections of negative curvature.
Title: Net circular polarization of sunspot penumbrae. Symmetry
breaking through anomalous dispersion
Authors: Schlichenmaier, R.; Müller, D. A. N.; Steiner, O.; Stix, M.
Bibcode: 2002A&A...381L..77S
Altcode:
The net circular polarization, N, is used as a measure for the
asymmetry of Stokes-V profiles: Nequiv int V(lambda ) d lambda ,
integrated over an absorption line. Exemplary for Fe I 630.2 nm and
Fe I 1564.8 nm, we synthesize penumbral V-profiles that stem from a
model atmosphere in which the Evershed flow is confined to horizontal
flux tubes which are embedded in a magnetic field that has the same
magnetic field strength as the flow channel, but is less inclined
w.r.t. the surface normal. At the two points where a line-of-sight
enters and leaves the flow channel, discontinuities in the inclination,
gamma , the velocity v, and the azimuth, phi , of the magnetic field
vector w.r.t. the plane perpendicular to the line-of-sight produce
V-asymmetries. Assuming an axially symmetric penumbra, we investigate
the azimuthal dependence N(psi ) for a mid-penumbral radius. We find:
(1) Without including anomalous dispersion, N(psi ) is symmetric
w.r.t. the line that connects disk center to the center of the spot. (2)
Including anomalous dispersion, this symmetry is broken. We demonstrate
that this is due to the difference in azimuth, triangle phi (psi ),
between the flow channel and the background that varies along the
penumbral circle. For Fe I 630.2 nm this effect is found to be of
minor relevance leading to essentially symmetric N-maps, whereas strong
asymmetries are predicted for Fe I 1564.8 nm. Our results provide an
explanation for recent observational findings.
Title: Measurement of the Cosmic-Ray Antiproton-to-Proton Abundance
Ratio between 4 and 50 GeV
Authors: Beach, A. S.; Beatty, J. J.; Bhattacharyya, A.; Bower, C.;
Coutu, S.; Duvernois, M. A.; Labrador, A. W.; McKee, S.; Minnick,
S. A.; Müller, D.; Musser, J.; Nutter, S.; Schubnell, M.; Swordy,
S.; Tarlé, G.; Tomasch, A.
Bibcode: 2001PhRvL..87A1101B
Altcode: 2001astro.ph.11094B
We present a new measurement of the antiproton-to-proton abundance
ratio, p¯/p, in the cosmic radiation. The HEAT-pbar instrument, a
balloon borne magnet spectrometer with precise rigidity and multiple
energy loss measurement capability, was flown successfully in Spring
2000, at an average atmospheric depth of 7.2 g/cm2. A total
of 71 antiprotons were identified above the vertical geomagnetic cutoff
rigidity of 4.2 GV. The highest measured proton energy was 81 GeV. We
find that the p¯/p abundance ratio agrees with that expected from
a purely secondary origin of antiprotons produced by primary protons
with a standard soft energy spectrum.
Title: Time-slice diagrams of solar granulation
Authors: Müller, D. A. N.; Steiner, O.; Schlichenmaier, R.; Brandt,
P. N.
Bibcode: 2001SoPh..203..211M
Altcode:
From a series of 1400 white-light images of solar granulation spanning
a time period of 8.2 hours, skeletal plots of time-slice diagrams are
derived showing intergranular lane positions as a function of time. The
diagrams permit to automatically track, classify, and relate 42 186
granules. Recurrently fragmenting granules are found that survive
by means of their descendants for more than 3 hours. Such long-lived
active granules tend to have a mean spatial distance along the slice
of about 10 Mm. This distance decreases with decreasing minimal
required lifetime. Since active granules are expected to generate a
steadily divergent flow over a long period of time, it is suggested
to identify them as a source of the mesogranular flow. Deficiencies
of the time-slice analysis are discussed. The relative frequency of
different types of granules and the granule decay time as derived
from the time-slice diagrams are compared with corresponding results
of previous works.
Title: Cosmic Rays Beyond the Knee
Authors: Müller, D.
Bibcode: 2001SSRv...99..105M
Altcode:
We briefly review the available data on cosmic rays beyond the
`knee', i.e., over the energy range from 10^15 to more than 10^20
eV. We discuss the observational status of the field, review some
of the current attempts to explain the origin of these particles,
and briefly survey the prospects of future measurements.
Title: KEY MEASUREMENTS IN THE FUTURE - Working Group Report
Authors: Müller, D.; Connel, J. J.; Decourchelle, A.; Mewaldt, R.;
Reynolds, S.; Strong, A.; Völk, H.; Wiedenbeck, M.
Bibcode: 2001SSRv...99..353M
Altcode:
The experimental basis of cosmic-ray astrophysics consists of
detailed measurements of the cosmic-ray intensity arriving near
earth, of observations of photons in all wavelength bands generated
by cosmic ray interactions in the interstellar medium or in the
cosmic-ray sources, and of laboratory studies of high energy particle
interactions. In addition, a large body of astronomical information on
the composition of stellar atmospheres and of the interstellar medium,
including interstellar dust grains, is required to bring cosmic-ray
data into context with subjects such as nucleosynthesis and evolution
of the galaxy. This report will summarize some of these observational
questions, will discuss specific experimental needs in current research,
and will review some of the key measurements that can be expected for
the near future. This review will neither be complete nor attempt
to establish observational priorities. However, it will illustrate
the variety of observational activities that are required to achieve
progress.
Title: Cutoff in the TeV Energy Spectrum of Markarian 421 during
Strong Flares in 2001
Authors: Krennrich, F.; Badran, H. M.; Bond, I. H.; Bradbury, S. M.;
Buckley, J. H.; Carter-Lewis, D. A.; Catanese, M.; Cui, W.; Dunlea,
S.; Das, D.; de la Calle Perez, I.; Fegan, D. J.; Fegan, S. J.;
Finley, J. P.; Gaidos, J. A.; Gibbs, K.; Gillanders, G. H.; Hall,
T. A.; Hillas, A. M.; Holder, J.; Horan, D.; Jordan, M.; Kertzman, M.;
Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Lang, M. J.; LeBohec,
S.; McKernan, B.; Moriarty, P.; Müller, D.; Ong, R.; Pallassini,
R.; Petry, D.; Quinn, J.; Reay, N. W.; Reynolds, P. T.; Rose, H. J.;
Sembroski, G. H.; Sidwell, R.; Stanton, N.; Swordy, S. P.; Vassiliev,
V. V.; Wakely, S. P.; Weekes, T. C.
Bibcode: 2001ApJ...560L..45K
Altcode: 2001astro.ph..7113K
Exceptionally strong and long-lasting flaring activity of the blazar
Mrk 421 occurred between 2001 January and March. Based on the excellent
signal-to-noise ratio of the data, we derive the energy spectrum between
260 GeV and 17 TeV with unprecedented statistical precision. The
spectrum is not well described by a simple power law even with a
curvature term. Instead, the data can be described by a power law with
exponential cutoff: dN/dE~E-2.14+/-0.03state-
E/E0 m-2 s-1 TeV-1
with E0=4.3+/-0.3stat TeV. Mrk 421 is the second
γ-ray blazar that unambiguously exhibits an absorption-like feature
in its spectral energy distribution at 3-6 TeV.
Title: Miniaturized atomic force microscope for planetary exploration
Authors: Gautsch, S.; Staufer, U.; Akiyama, T.; Hidber, H. R.; Tonin,
A.; Howald, L.; Müller, D.; Niedermann, P.; de Rooij, N. F.
Bibcode: 2001ESASP.480...11G
Altcode: 2001smt..conf...11G
The Atomic Force Microscope (AFM) has revealed itself as a reliable tool
for characterizing surface topography with nanometer resolution. In
principle, a sharp tip mounted on a cantilever is brought into close
proximity of the sample surface. The forces acting between the sample
and the tip slightly deflect the cantilever. Scanning across the
surface while recording this deflection provides a topographic image
of the sample. As in most space experiments, performing microscopy
measurements on a planetary mission requires a good trade-off between
the experiment's weight and size and the quality and relevance of the
measured data. A plain optical setup with acceptable size and weight
for a space launch will provide images with limited resolution. Thus,
atomic force microscopy with a well designed instrument can be
complementary to an optical setup for increasing image resolution
and getting higher scientific throughput. At the first glance, high
sensitivity and required interaction between the instrument and the
operator render the AFM unsuitable for planetary missions. However,
micro-fabrication technology combined with innovative design ideas
allowed us to build an error tolerant system with functionality for
addressing the above mentioned challenges.
Title: Cosmic-Ray Electrons and Positrons from 1 to 100 GeV:
Measurements with HEAT and Their Interpretation
Authors: DuVernois, M. A.; Barwick, S. W.; Beatty, J. J.;
Bhattacharyya, A.; Bower, C. R.; Chaput, C. J.; Coutu, S.; de Nolfo,
G. A.; Lowder, D. M.; McKee, S.; Müller, D.; Musser, J. A.; Nutter,
S. L.; Schneider, E.; Swordy, S. P.; Tarlé, G.; Tomasch, A. D.;
Torbet, E.
Bibcode: 2001ApJ...559..296D
Altcode:
Measurements of the energy spectra of negative electrons and positrons
have been performed with the High-Energy Antimatter Telescope (HEAT)
in two balloon flights-1994 May from Fort Sumner, NM, and 1995 August
from Lynn Lake, Manitoba. We present the combined data set from these
two flights, covering the energy range 1-100 GeV. We compare our data
with results from other groups and discuss the data in the context
of diffusive propagation models. There is some evidence that primary
electrons above 10 GeV and cosmic-ray nuclei exhibit the same energy
spectrum at the source, but that the source spectrum becomes harder at
lower energy. Within the experimental uncertainties, the intensity of
positrons is consistent with a purely secondary origin, due to nuclear
interactions in interstellar space.
Title: Cosmic Ray Nuclei at High Energies: Recent Results from TRACER
and Future Prospects
Authors: Gahbauer, F.; Hermann, G.; Hörandel, J.; Müller, D.;
Swordy, S. P.; Wakely, S. P.
Bibcode: 2001ICRC....5.1612G
Altcode: 2001ICRC...27.1612G
The first balloon flight of the TRACER instrument in 1999 led to a
new measurement of the energy spectra of cosmic ray nuclei from Z=8
to Z=26 at energies from a few GeV/nucleon to several TeV/nucleon. We
will present and discuss the results, compare them with other recent
measurements and examine the implications for current cosmic ray
propagation and acceleration models. Finally, we will comment on
the prospects of planned flights of the TRACER instrument on long
duration balloons, and on the adaptation of the measurement technique
to anticipated space missions.
Title: The Cosmic-Ray Antiproton to Proton Ratio from 5 to 50 GEV
Authors: Musser, J.; Beach, A. S.; Beatty, J. J.; Bhattacharyya, A.;
Bower, C.; Coutu, S.; Duvernois, M. A.; Labrador, A.; McKee, S. P.;
Minnick, S.; Muller, D.; Nutter, S.; Schubnell, M.; Swordy, S.; Tarle,
G.; Tomasch, A.
Bibcode: 2001ICRC....5.1684M
Altcode: 2001ICRC...27.1684M
We present a new measurement of the cosmic-ray p/p abundance ratio as
a function of energy. The data were obtained from a balloon flight
of the HEAT-pbar instrument in the Spring of 2000 from Ft. Sumner,
NM. Our results for the energy-dependent antiproton fraction are
compared with other measurements and recent predictions based on the
observed abundance of secondary light elements in the cosmic rays. Our
data appear to be consistent with a purely secondary production of
antiprotons.
Title: A new Measurement of the Energy Spectra of Cosmic Ray Nuclei
Authors: Hörandel, J. R.; Britton, J. W.; Gahbauer, F.; Hermann,
G.; Müller, D.; Swordy, S. P.; Wakely, S. P.
Bibcode: 2001ICRC....5.1608H
Altcode: 2001ICRC...27.1608H
A new large-area detector system was constructed at the University of
Chicago for direct measurements of heavy cosmic ray nuclei (oxygen
to iron) up to about 10 TeV/nucleon. TRACER ("Transition Radiation
Array for Cosmic Energetic Radiation") uses plastic scintillators to
measure charge and a proportional tube array to measure energy via
specific ionization and transition radiation. While TRACER is designed
for circumglobal long-duration balloon flights, an initial 28-hour
flight was conducted in Autumn 1999 from Ft. Sumner, New Mexico. We
will discuss the performance of the detector and present first data
from the balloon flight.
Title: Positron Measurements with the Heat-Pbar Instrument
Authors: Coutu, S.; Beach, A. S.; Beatty, J. J.; Bhattacharyya, A.;
Bower, C.; Duvernois, M. A.; Labrador, A.; McKee, S. P.; Minnick,
S.; Muller, D.; Musser, J.; Nutter, S.; Schubnell, M.; Swordy, S.;
Tarle, G.; Tomasch, A.
Bibcode: 2001ICRC....5.1687C
Altcode: 2001ICRC...27.1687C
The HEAT-pbar magnet spectrometer, flown on a balloon in Spring 2000,
was designed for measurements of cosmic-ray antiprotons. However,
the use of several particle identification methods also permits
the detection of electrons and positrons with high rejection power
against protons, pions and muons. We present new measurements of the
positron fraction above 5 GeV, which confirm the results of the earlier
HEAT-e± flights, albeit with an independent technique. In particular,
we investigate the region below 10 GeV, which previously had indicated
some structure, possibly suggesting a small primary contribution to
the positron intensity.
Title: Detection of cosmic ray antiprotons with the heat-pbar
instrument
Authors: Nutter, S.; Beach, A. S.; Beatty, J. J.; Bhattacharyya, A.;
Bower, C.; Coutu, S.; Duvernois, M. A.; Labrador, A.; McKee, S. P.;
Minnick, S.; Muller, D.; Musser, J.; Schubnell, M.; Swordy, S.; Tarle,
G.; Tomasch, A.
Bibcode: 2001ICRC....5.1691N
Altcode: 2001ICRC...27.1691N
HEAT-pbar, a balloon instrument to measure the cosmic-ray antiproton
flux from 5 to 50 GeV energy, was flown successfully in spring
2000. The instrument consists of a combination of a superconducting
magnet spectrometer with time-of-flight counters and multiple wire
chambers for measurements of the specific ionization. We review the
instrument performance during flight and discuss how the detector
configuration separates antiprotons from the large flux of electrons,
muons/pions, and protons. After all data analysis cuts, approximately
70 antiprotons were detected.
Title: Absolute Rigidity Spectra of Protons and Helium from 16 to
250 GV
Authors: Duvernois, M. A.; Beatty, J. J.; Bower, C.; Coutu, S.; McKee,
S. P.; Muller, D.; Musser, J.; Nutter, S.; Swordy, S.; Tarle, G.;
Tomasch, A.
Bibcode: 2001ICRC....5.1618D
Altcode: 2001ICRC...27.1618D
The HEAT-e± magnet spectrometer was used in two balloon flights to
measure the intensities of cosmic-ray electrons and positrons. However,
this instrument also collected a large sample of proton and helium
nuclei. We report here the rigidity spectra for these two species
up to about 250 GV, and we compare our results with those of other
recent experiments. Above approximately 50 GV, the rigidity spectrum
of helium appears to be slightly harder than that of protons.
Title: Splash and reentrant albedo observations of electrons and
positrons at a 4.5 GV vertical magnetic cutoff
Authors: Duvernois, M.; Beach, A. S.; Beatty, J. J.; Bhattacharyya,
A.; Bower, C.; Coutu, S.; Labrador, A.; McKee, S. P.; Minnick, S.;
Muller, D.; Musser, J.; Nutter, S.; Schubnell, M.; Swordy, S.; Tarle,
G.; Tomasch, A.
Bibcode: 2001ICRC...10.4003D
Altcode: 2001ICRC...27.4003D
The HEAT-p balloon magnet spectrometer was used to measure the
rigidity spectra of splash and reentrant albedo particles. Although
the primary objective of the HEATp instrument is the measurement of
antiproton abundances at high energy, a large sample of events below
local geomagnetic cutoff was also collected. The top-bottom symmetry of
the detector configuration and the excellent particle identification
required for antiproton measurements allowed for clean measurements
of the upward and downward-going electron and positron albedos. These
measurements are important in understanding the detailed properties and
model dependencies of both the Earth's magnetosphere and of extensive
air showers at small atmospheric depths.
Title: The Design of Precision X-ray Transition Radiation Detectors
for Cosmic Rays
Authors: Wakely, S. P.; Gahbauer, F. H.; Hörandel, J. R.; Müller,
D.; Swordy, S. P.
Bibcode: 2001ICRC....6.2247W
Altcode: 2001ICRC...27.2247W
Precision transition radiation detectors (TRDs) can be an effective
tool for determining the energy spectra of cosmic ray nuclei up to the
energies of the knee. They offer unique measurement capabilities and
embody design principles which are somewhat different from those of the
threshold TRDs used in accelerator experiments. We will discuss some
of the characteristics of these instruments, including the relevant
design principles and the properties which determine their performance.
Title: Casimir energy in a small volume multiply connected static
hyperbolic preinflationary universe
Authors: Müller, Daniel; Fagundes, Helio V.; Opher, Reuven
Bibcode: 2001PhRvD..63l3508M
Altcode: 2001gr.qc.....3014M
A few years ago, Cornish, Spergel and Starkman (CSS) suggested that a
multiply connected ``small'' universe could allow for classical chaotic
mixing as a preinflationary homogenization process. The smaller the
volume, the more important the process. Also, a smaller universe has a
greater probability of being spontaneously created. Previously DeWitt,
Hart and Isham (DHI) calculated the Casimir energy for static multiply
connected flat space-times. Because of the interest in small volume
hyperbolic universes (e.g., CSS), we generalize the DHI calculation
by making a numerical investigation of the Casimir energy for a
conformally coupled, massive scalar field in a static universe, whose
spatial sections are the Weeks manifold, the smallest universe of
negative curvature known. In spite of being a numerical calculation,
our result is in fact exact. It is shown that there is spontaneous
vacuum excitation of low multipolar components.
Title: Cosmic Rays Beyond the Knee
Authors: Müller, D.
Bibcode: 2001agcr.book..105M
Altcode:
No abstract at ADS
Title: Key Measurements in the Future
Authors: Müller, D.; Connel, J. J.; Decourchelle, A.; Mewaldt, R.;
Reynolds, S.; Strong, A.; Völk, H.; Wiedenbeck, M.
Bibcode: 2001agcr.book..353M
Altcode:
No abstract at ADS
Title: Orbits in a Neighboring Dwarf Galaxy According to Modified
Nonrelativistic Dynamics
Authors: Müller, Daniel; Opher, Reuven
Bibcode: 2000ApJ...540...57M
Altcode: 2000astro.ph..4150M
We study the orbits in the modified nonrelativistic dynamics (MOND)
theory within a dwarf galaxy of mass Md~108
Msolar at a distance of ~100 kpc from a neighboring
galaxy of mass Mg=5×1011 Msolar,
such as ours. It is assumed that a second mass m<<Md
is gravitationally bound to Md by a previously calculated
potential for the MOND theory. This potential is obtained for a
free-falling mass Md in a constant external gravitational
acceleration field ∇φg. The numerical technique of
surfaces of section is used to study the stability of the phase-space
orbits in the dwarf galaxy. Equatorial orbits with sufficiently
small eccentricities e<0.65 are found to be stable with respect
to small changes in the initial conditions. (The equatorial plane is
perpendicular to the direction of ∇φg, which is along the
line joining Md and Mg.) For decreasing values
of the conserved component of the angular momentum, in the direction
of ∇φg, equatorial stability is lost.
Title: Polychromatic guide star: feasibility study
Authors: Foy, Renaud; Pique, Jean-Paul; Petit, Alain D.; Chevrou,
Patrick; Michau, Vincent; Grynberg, Gilbert; Migus, Arnold; Ageorges,
Nancy; Bellanger, Veronique; Biraben, Francois; Deron, Ruy; Fews,
Hayden; Foy, Francoise-Claude; Hoegemann, Claudia; Laubscher, Markus;
Mueller, Daniel; D'Orgeville, Celine; Peillet, Olivier; Redfern,
Mike; Schoeck, Matthias; Segonds, Patricia; Soden, Richard; Tallon,
Michel; Thiebaut, Eric; Tokovinin, Andrei A.; Vaillant, Jerome;
Weulersse, Jean-Marc
Bibcode: 2000SPIE.4065..312F
Altcode:
Adaptive optics at astronomical telescopes aims at correcting in
real time the phase corrugations of incoming wavefronts caused by
the turbulent atmosphere, as early proposed by Babcock. Measuring the
phase errors requires a bright source located within the isoplanatic
patch of the program source. The probability that such a reference
source exists is a function of the wavelength, of the required image
quality (Strehl ratio), of the turbulence optical properties, and of
the direction of the observation. It turns out that the sky coverage is
disastrously low in particular in the visible wavelength range where,
unfortunately, the gain in spatial resolution brought by adaptive
optics is the largest. Foy and Labeyrie have proposed to overcome
this difficulty by creating an artificial point source in the sky in
the direction of the observation relying on the backscattered light
due to a laser beam. This laser guide star (hereinafter referred to
as LGS) can be bright enough to allow us to accurately measure the
wavefront phase errors, except for two modes which are the piston
(not relevant in this case) and the tilt. Pilkington has emphasized
that the round trip time of the laser beam to the mesosphere,
where the LGS is most often formed, is significantly shorter than
the typical tilt coherence time; then the inverse-return-of-light
principle causes deflections of the outgoing and the ingoing beams
to cancel. The apparent direction of the LGS is independent of the
tilt. Therefore the tilt cannot be measured only from the LGS. Until
now, the way to overcome this difficulty has been to use a natural
guide star to sense the tilt. Although the tilt is sensed through the
entire telescope pupil, one cannot use a faint source because $APEX
90% of the variance of the phase error is in the tilt. Therefore,
correcting the tilt requires a higher accuracy of the measurements
than for higher orders of the wavefront. Hence current adaptive optics
devices coupled with a LGS face low sky coverage. Several methods have
been proposed to get a partial sky coverage for the tilt. The only
one providing us with a full sky coverage is the polychromatic LGS
(hereafter referred to as PLGS). We present here a progress report of
the R&D program Etoile Laser Polychromatique et Optique Adaptative
(ELP-OA) carried out in France to develop the PLGS concept. After a
short recall of the principles of the PLGS, we will review the goal
of ELP-OA and the steps to get over to bring it into play. We finally
shortly described the effort in Europe to develop the LGS.
Title: Energy spectra, altitude profiles, and charge ratios of
atmospheric muons
Authors: Coutu, S.; Beatty, J. J.; Duvernois, M. A.; Barwick, S. W.;
Schneider, E.; Bhattacharyya, A.; Bower, C. R.; Musser, J. A.;
Labrador, A.; Müller, D.; Swordy, S. P.; Torbet, E.; Chaput, C.;
McKee, S.; Tarlé, G.; Tomasch, A. D.; Nutter, S. L.; Denolfo, G. A.
Bibcode: 2000PhRvD..62c2001C
Altcode: 2000hep.ex....4010C
We present a new measurement of air shower muons made during
atmospheric ascent of the High Energy Antimatter Telescope balloon
experiment. The muon charge ratio μ+/μ- is
presented as a function of atmospheric depth in the momentum interval
0.3-0.9 GeV/c. The differential μ- momentum spectra are
presented between 0.3 and ~50 GeV/c at atmospheric depths between
13 and 960 g/cm2. We compare our measurements with other
recent data and with Monte Carlo calculations of the same type as
those used in predicting atmospheric neutrino fluxes. We find that
our measured μ- fluxes are smaller than the predictions
by as much as 70% at shallow atmospheric depths, by ~20% at the depth
of shower maximum, and are in good agreement with the predictions at
greater depths. We explore the consequences of this on the question
of atmospheric neutrino production.
Title: ELPOA: toward the tilt measurement from a polychromatic laser
guide star
Authors: Foy, Renaud; Pique, Jean-Paul; Petit, Alain D.; Chevrou,
Patrick; Michau, Vincent; Grynberg, Gilbert; Migus, Arnold; Ageorges,
Nancy; Bellanger, Veronique; Biraben, Francois; Deron, Ruy; Fews,
Hayden; Foy, Francoise-Claude; Hoegemann, Claudia; Laubscher, Markus;
Mueller, Daniel; D'Orgeville, Celine; Peillet, Olivier; Redfern,
Mike; Schoeck, Matthias; Segonds, Patricia; Soden, Richard; Tallon,
Michel; Thiebaut, Eric; Tokovinin, Andrei A.; Vaillant, Jerome;
Weulersse, Jean-Marc
Bibcode: 2000SPIE.4007..284F
Altcode:
Adaptive optics at astronomical telescopes aims at correcting in
real time the phase corrugations of incoming wavefronts caused by the
turbulent atmosphere, as early proposed by Babcock. Measuring the phase
errors requires a bright source, which is located within the isoplanatic
patch of the program source. The probability that such a reference
source exists is a function of the wavelength of the observation,
of the required image quality (Strehl ratio), of the turbulence
optical properties, and of the direction of the observation. Several
papers have addressed the problem of the sky coverage as a function
of these parameters (see e.g.: Le Louarn et al). It turns out that
the sky coverage is disastrously low in particular in the short
(visible) wavelength range where, unfortunately, the gain in spatial
resolution brought by adaptive optics is the largest. Foy and Labeyrie
have proposed to overcome this difficulty by creating an artificial
point source in the sky in the direction of the observation relying
on the backscattered light due to a laser beam. This laser guide
star (hereafter referred to as LGS) can be bright enough to allow
us to accurately measure the wavefront phase errors, except for two
modes which are the piston (which is not relevant in this case) and
the tilt. Pilkington has emphasized that the round trip time of the
laser beam to the mesosphere, where the LGS is most often formed, is
significantly shorter than the typical tilt coherence time; then the
inverse-return- of-light principle causes deflections of the outgoing
and the ingoing beams to cancel. The apparent direction of the LGS
is independent of the tilt. Therefore the tilt cannot be measured
only from the LGS. Until now, the way to overcome this difficulty
has been to use a natural guide star to sense the tilt. Although the
tilt is sensed through the entire telescope pupil, one cannot use a
faint source because approximately equals 90% of the variance of the
phase error is in the tilt. Therefore, correcting the tilt requires
a higher accuracy of the measurements than for higher orders of the
wavefront. Hence current adaptive optics devices coupled with a LGS face
low sky coverage. Several methods have been proposed to get a partial
or total sky coverage for the tilt, such as the dual adaptive optics
concept, the elongation perspective method, or the polychromatic LGS
(hereafter referred to as PLGS). We present here a progress report of
the R&D program Etoile Laser Polychromatique et Optique Adaptative
(ELP-OA) carried out in France to develop the PLGS concept. After a
short recall of the principles of the PLGS, we will review the goal
of ELP-OA and the steps to get over to bring it into play.
Title: VERITAS: Very Energetic Radiation Imaging Telescope Array
System
Authors: Bond, F.; Krennrich, S. M.; Bradbury, I. H.; Burckley, A. C.;
Breslin, J. H.; Carter-Lewis, D. A.; Catanese, M.; Dingus, B. L.;
Fegan, D. J.; Finley, J. P.; Gaidos, J.; Hillas, J.; Grindlay, A. M.;
Hermann, G.; Kaaret, P.; Kieda, D.; Knapp, J.; Lebohec, S.; Lessard,
R. W.; Lloyd-Evans, T.; Müller, D.; Ong, R.; Quinn, J.; Rose, H. J.;
Salamon, M.; Sembroski, G. H.; Swordy, S.; Vassiliev, V. V.; Weekes,
T. C.
Bibcode: 2000AIPC..515..515B
Altcode: 2000gtgr.conf..515B
No abstract at ADS
Title: VERITAS: Very energetic radiation imaging telescope array
system
Authors: Krennrich, F.; Bradbury, S. M.; Bond, I. H.; Breslin, A. C.;
Buckley, J. H.; Carter-Lewis, D. A.; Catanese, M.; Dingus, B. L.;
Fegan, D. J.; Finley, J. P.; Gaidos, J.; Grindlay, J.; Hillas, A. M.;
Hermann, G.; Kaaret, P.; Kieda, D.; Knapp, J.; Lebohec, S.; Lessard,
R. W.; Lloyd-Evans, J.; Müller, D.; Ong, R.; Quinn, J.; Rose, H. J.;
Salamon, M.; Sembroski, G. H.; Swordy, S.; Vassiliev, V. V.; Weekes,
T. C.
Bibcode: 2000AIPC..515..515K
Altcode:
The Very Energetic Radiation Imaging Telescope Array System (VERI-TAS)
is a wide energy range (50 GeV-50 TeV) atmospheric Cherenkov detector
and will start operation in 2004. The design is driven by a major
scientific interest in jets of active galactic nuclei, probing the
intergalactic IR fields with TeV γ-ray beams, measuring the high energy
spectrum of γ-ray bursts and galactic sources of cosmic rays. Also
γ-rays signatures of quantum gravity, neutralinos and primordial black
holes constitute the exotic scientific motivations to built a highly
versatile detector that can be operated in various modes. The technical
concept and design of the seven-telescope array system is described. .
Title: Absolute Spectra of Protons and Helium Nuclei from 16-250 GV
Authors: Duvernois, M. A.; Beatty, J. J.; Coutu, S.; de Nolfo, G. A.;
Barwick, S. W.; Schneider, E.; Bhattacharyya, A.; Bower, C. R.;
Musser, J. A.; Chaput, C. J.; McKee, S.; Tarle, G.; Tomasch, A. D.;
Lowder, D. M.; Muller, D.; Swordy, S. P.; Torbet, E.; Nutter, S. L.
Bibcode: 2000APS..APRC16005D
Altcode:
The High-Energy Antimatter Telescope (HEAT) balloon-borne magnet
spectrometer was used to measure the absolute energy and rigidity
spectra of cosmic-ray protons and helium. Although the primary goal
of the HEAT experiment is the measurement of electron and positron
abundances at high energy, a large sample of high energy protons and
helium were also collected. This observation is compared with other
recent balloon experiments (including other magnet spectrometers) and
with theoretical expectations. Some flattening of the helium spectrum
above ~50 GeV is observed, consistent with other measurements and with
some models of non-linear shock acceleration.
Title: The Very Energetic Radiation Imaging Telescope Array System
(VERITAS)
Authors: Weekes, T. C.; Bradbury, S. M.; Bond, I. H.; Breslin, A. C.;
Buckley, J. H.; Carter-Lewis, D. A.; Catanese, M.; Dingus, B. L.;
Fegan, D. J.; Finley, J. P.; Gaidos, J.; Grindlay, J.; Hillas, A. M.;
Hermann, G.; Kaaret, P.; Kieda, D.; Knapp, J.; Krennrich, F.; Lebohec,
S.; Lessard, R. W.; Lloyd-Evans, J.; Müller, D.; Ong, R.; Quinn, J.;
Rose, H. J.; Salamon, M.; Sembroski, G. H.; Swordy, S.; Vassiliev,
V. V.
Bibcode: 2000AIPC..510..637W
Altcode: 2000comp.symp..637W
An overview of the current status and scientific goals of VERITAS,
a proposed hexagonal array of seven 10 m aperture imaging Cherenkov
telescopes, is provided. The selected site is close to Mt. Hopkins,
the site of the Whipple Observatory, in Arizona. Each telescope, of 12
m focal length, will be equipped with a 499 element photomultiplier
camera covering a 3.5 degree field of view. A central station will
initiate the readout of 500 MHz FADCs upon receipt of multiple telescope
triggers. The minimum detectable flux sensitivity will be 0.5% of
the Crab Nebula flux at 200 GeV. VERITAS will operate primarily as
a γ-ray observatory in the 50 GeV to 50 TeV range for the study of
active galaxies, supernova remnants, pulsars and gamma-ray bursts. .
Title: The Energy Spectra and Relative Abundances of Electrons and
Positrons in the Galactic Cosmic Radiation
Authors: Barwick, S. W.; Beatty, J. J.; Bower, C. R.; Chaput, C. J.;
Coutu, S.; de Nolfo, G. A.; DuVernois, M. A.; Ellithorpe, D.; Ficenec,
D.; Knapp, J.; Lowder, D. M.; McKee, S.; Müller, D.; Musser, J. A.;
Nutter, S. L.; Schneider, E.; Swordy, S. P.; Tarlé, G.; Tomasch,
A. D.; Torbet, E.
Bibcode: 1998ApJ...498..779B
Altcode: 1997astro.ph.12324B
Observations of cosmic-ray electrons and positrons have been made with
a new balloon-borne detector, the High-Energy Antimatter Telescope
(HEAT), which was first flown in 1994 May from Fort Sumner, New
Mexico. We describe the instrumental approach and the data analysis
procedures, and we present results from this flight. The measurement
has provided a new determination of the individual energy spectra of
electrons and positrons from 5 GeV to about 50 GeV and of the combined
``all-electron'' intensity (e+ + e-) up to ~100
GeV. The single power-law spectral indices for electrons and positrons
are α = 3.09 +/- 0.08 and 3.3 +/- 0.2, respectively. We find that a
contribution from primary sources to the positron intensity in this
energy region, if it exists, must be quite small.
Title: Cosmic ray electrons and positrons from 1--100 GeV: HEAT
balloon measurements
Authors: Duvernois, M. A.; Beatty, J. J.; Coutu, S.; Barwick,
S. W.; Schneider, E.; Bhattacharyya, A.; Bower, C. R.; Musser, J. A.;
Chaput, C. J.; McKee, S.; Tarlé, G.; Tomasch, A. D.; de Nolfo, G. A.;
Labrador, A.; Müller, D.; Swordy, S. P.; Torbet, E.; Nutter, S. L.
Bibcode: 1998APS..APR..M709D
Altcode:
Observations of the cosmic ray electron and positron energy spectra
have been performed with the balloon-borne ``High-Energy Antimatter
Telescope'' (HEAT) flown in May 1994 from Fort Sumner, NM, and May
1995 from Lynn Lake, Manitoba in Canada. We summarize the instrument
procedures and data analysis, and we present the results, combined from
the two flights. These include determinations of the absolute energy
spectra of electrons and positrons from 1--50 GeV, and the combined
``all-electron'' spectrum (e^++e^-) up to 100 GeV. We discuss the
results in the context of current models of cosmic ray propagation in
the Galaxy and find no strong evidence for contributions to the positron
intensity beyond purely secondary origin from nuclear interactions in
the ISM.
Title: Cosmic ray reentrant electron albedo: High-Energy Antimatter
Telescope balloon measurements from Fort Sumner, New Mexico
Authors: Barwick, S. W.; Beatty, J. J.; Bower, C. R.; Chaput, C. J.;
Coutu, S.; de Nolfo, G. A.; DuVernois, M. A.; Ficenec, D.; Knapp, J.;
Lowder, D. M.; McKee, S.; Müller, D.; Musser, J. A.; Nutter, S. L.;
Schneider, E.; Swordy, S. P.; Tarlé, G.; Tomasch, A. D.; Torbet, E.
Bibcode: 1998JGR...103.4817B
Altcode:
The High-Energy Antimatter Telescope (HEAT) balloon cosmic ray detector
flew from Fort Sumner, New Mexico on May 3-5, 1994. The instrument
measured electron and positron abundances and spectra from ~1 to 100 GeV
at a vertical geomagnetic cutoff rigidity that varied between 4.0 and
4.5 GV. The intensities of electrons and positrons have been measured
as a function of atmospheric depth between 3.8 and 7.4gcm-2
of overburden. At magnetic rigidities below cutoff, the intensity of
downward moving e+/- consists of secondary (spallogenic)
particles and the reentrant (or return) albedo. We determine the
contribution of the reentrant electron albedo and compare it with
earlier measurements and limits at similar geomagnetic cutoff levels. In
the range of 1.0-2.4 GeV, the reentrant albedo component amounts to 40%
of the total electron intensity observed.
Title: Measurements of the Cosmic-Ray Positron Fraction from 1 to
50 GeV
Authors: Barwick, S. W.; Beatty, J. J.; Bhattacharyya, A.; Bower,
C. R.; Chaput, C. J.; Coutu, S.; de Nolfo, G. A.; Knapp, J.;
Lowder, D. M.; McKee, S.; Mueller, D.; Musser, J. A.; Nutter, S. L.;
Schneider, E.; Swordy, S. P.; Tarle, G.; Tomasch, A. D.; Torbet, E.;
HEAT Collaboration
Bibcode: 1997ApJ...482L.191B
Altcode: 1997astro.ph..3192H; 1997astro.ph..3192B
Two measurements of the cosmic-ray positron fraction as a function
of energy have been made using the High-Energy Antimatter Telescope
(HEAT) balloon-borne instrument. The first flight took place from Fort
Sumner, New Mexico, in 1994 and yielded results above the geomagnetic
cutoff energy of 4.5 GeV. The second flight, from Lynn Lake, Manitoba,
in 1995, permitted measurements over a larger energy interval, from
1 to 50 GeV. We present results on the positron fraction based on
data from the Lynn Lake flight and compare these with the previously
published results from the Fort Sumner flight. The results confirm that
the positron fraction does not increase with energy above ~10 GeV,
although a small excess above purely secondary production cannot be
ruled out. At low energies the positron fraction is slightly larger
than that reported from measurements made in the 1960s. This effect
could possibly be a consequence of charge dependence in the level of
solar modulation.
Title: Towards the knee: direct measurements of the cosmic ray
composition with electronic detectors
Authors: Müller, D.; Diehl, E.; Gahbauer, F.; Meyer, P.; Swordy, S.
Bibcode: 1997AdSpR..19..719M
Altcode:
Over a wide range of energies, the cosmic ray composition can be
described with a uniform source spectrum for all components, and by a
propagation pathlength that continually decreases with energy. However,
there are indications that this description may no longer be valid
above ~ 10^13eV/particle, where observational data become scarce. We
discuss how progress can be made in new direct measurements above the
atmosphere over the region 10^13-10^15eV/particle. Most important is
the availability of well calibrated detectors with known charge and
energy resolution and very large sensitive area. For the heavier nuclei
(Z >= 3), these specifications can be met with a new generation of
light weight transition radiation detectors. In balloon flights of a few
days duration these will reach maximum energies of ~ 0.5 x 10^15eV for
oxygen and ~ 2 x 10^15eV for iron nuclei with good statistical accuracy.
Title: The High-Energy Antimatter Telescope (HEAT): An instrument
for the study of cosmic-ray positrons
Authors: Barwick, S. W.; Beatty, J. J.; Bower, C. R.; Chaput, C.;
Coutu, S.; de Nolfo, G.; Ellithorpe, D.; Ficenec, D.; Knapp, J.;
Lowder, D. M.; McKee, S.; Müller, D.; Musser, J. A.; Nutter, S. L.;
Schneider, E.; Swordy, S. P.; Tang, K. K.; Tarlé, G.; Tomasch, A. D.;
Torbet, E.
Bibcode: 1997NIMPA.400...34B
Altcode:
The HEAT (High-Energy Antimatter Telescope) instrument has been
developed for a series of observations in cosmic-ray astrophysics
that require the use of a superconducting magnet spectrometer. This
paper describes the first configuration of HEAT which is optimized
for the detection of cosmic-ray electrons and positrons below 100
GeV. In addition to the spectrometer, a combination of time-of-flight
scintillators, a transition radiation detector, and an electromagnetic
shower counter, provides particle identification, energy measurement,
and powerful discrimination against the large background of protons. The
instrument was successfully flown aboard high-altitude balloons in 1994
and 1995. The design and construction of the spectrometer and of the
detector systems are described, and the performance of the instrument
is demonstrated with data obtained in flight.
Title: A large area RICH photon detector for astrophysics
Authors: Ellithorpe, D.; Diehl, E.; Müller, D.; Swordy, S.
Bibcode: 1997NIMPA.387..150E
Altcode:
We have developed a detector of 1.5 × 1.4 m2 area
which measures individual photons with a spatial resolution of
~1 cm. This device is in the focal plane of a 3 m long gas-filled
Ring Imaging CHerenkov (RICH) instrument designed to make precision
measurements of the velocity of high energy cosmic rays at the top
of the atmosphere. In future applications this type of detector may
be combined with a magnet spectrometer to make mass measurements of
cosmic rays at high energy. The detector is a wire chamber filled with
an ethane/TMAE mixture having fused silica windows. The signals are
collected by 18 432 cathode pads of 1 cm2 area connected
to a VLSI electronic readout system. The quantum efficiency of the
detector in the wavelength region of 180-200 nm is ~12%. We shall
discuss the design and operation of this detector.
Title: Energy Spectra of Electrons and Positrons from 5 to 100 GeV
Authors: Müller, D.; Barwick, S. W.; Beatty, J. J; Bhattacharyya, A.;
Bower, C. R.; Chaput, C. J.; Coutu, S.; de Nolfo, G. A.; Du Vernois,
M. A.; Knapp, J.; Lowder, D. M.; McKee, S.; Musser, J. A.; Nutter,
S. L.; Schneider, E.; Swordy, S. P.; Tarlé, G.; Tomasch, A. D.;
Torbet, E.
Bibcode: 1997ICRC....4..237M
Altcode: 1997ICRC...25d.237M
No abstract at ADS
Title: A New Measurement of the Energy Spectra of Light Nuclei from
20-150 GeV/n
Authors: Diehl, E.; Ellithorpe, D.; Müller, D.; Swordy, S. P.
Bibcode: 1997ICRC....3..405D
Altcode: 1997ICRC...25c.405D
No abstract at ADS
Title: Measurements of the Cosmic Ray Positron Fraction with the
HEAT Spectrometer
Authors: Musser, J.; Barwick, S. W.; Beatty, J. J; Bhattacharyya,
A.; Bower, C. R.; Chaput, C. J.; Coutu, S.; de Nolfo, G. A.; Knapp,
J.; Lowder, D. M.; McKee, S.; Müller, D.; Nutter, S. L.; Schneider,
E.; Swordy, S. P.; Tarlé, G.; Tomasch, A. D.; Torbet, E.
Bibcode: 1997ICRC....4..209M
Altcode: 1997ICRC...25d.209M
No abstract at ADS
Title: Cosmic-Ray Positions: Are there Primary Sources?
Authors: Coutu, S.; Barwick, S. W.; Beatty, J. J; Bhattacharyya,
A.; Bower, C. R.; Chaput, C. J.; de Nolfo, G. A.; Du Vernois, M. A.;
Labrador, A.; McKee, S.; Müller, D.; Nutter, S. L.; Schneider, E.;
Swordy, S. P.; Tarlé, G.; Tomasch, A. D.; Torbet, E.
Bibcode: 1997ICRC....4..213C
Altcode: 1997ICRC...25d.213C
No abstract at ADS
Title: Relative Abundances of Positive and Negative Muons in the
Atmosphere
Authors: Tarlé, G.; Barwick, S. W.; Beatty, J. J.; Bhattacharyya,
A.; Bower, C. R.; Chaput, C. J.; Coutu, S.; de Nolfo, G. A.; Knapp,
J.; Lowder, D. M.; McKee, S.; Müller, D.; Musser, J. A.; Nutter,
S. L.; Schneider, E.; Swordy, S. P.; Tomasch, A. D.; Torbet, E.
Bibcode: 1997ICRC....6..321T
Altcode: 1997ICRC...25f.321T
No abstract at ADS
Title: VERITAS: The Very Energetic Radiation Imaging Telescope
Array System.
Authors: Weekes, T. C.; Akerlof, C.; Biller, S.; Breslin, A. C.;
Catanese, M.; Carter-Lewis, D. A.; Cawley, M. F.; Dingus, B.; Fazio,
G. G.; Fegan, D. J.; Finley, J.; Fishman, G.; Gaidos, J.; Gillanders,
G. H.; Gorham, P.; Grindlay, J. E.; Hillas, A. M.; Huchra, J.; Kaaret,
P.; Kertzman, M.; Kieda, D.; Krennrich, F.; Lamb, R. C.; Lang, M. J.;
Marscher, A. P.; Matz, S.; McKay, T.; Muller, D.; Ong, R.; Purcell,
W.; Rose, H. J.; Sembroski, G.; Seward, F. D.; Slane, P.; Swordy,
S.; Tumer, T.; Ulmer, M.; Urban, M.; Wilkes, B.
Bibcode: 1997ICRC....5..173W
Altcode: 1997ICRC...25e.173W; 1997icrc...25..173W; 1997astro.ph..6143W
A next generation atmospheric Cherenkov observatory is described based
on the Whipple Observatory $\gamma$-ray telescope. A total of nine
such imaging telescopes will be deployed in an array that will permit
the maximum versatility and give high sensitivity in the 50 GeV -
50 TeV band (with maximum sensitivity from 100 GeV to 10 TeV).
Title: Secondary and Re-entrant Albedo Electrons in the Atmosphere
Authors: de Nolfo, G. A.; Barwick, S. W.; Beatty, J. J.; Bhattacharyya,
A.; Bower, C. R.; Coutu, S.; Chaput, C. J.; DuVernois, M. A.; Knapp,
J.; Lowder, D. M.; McKee, S.; Müller, D.; Musser, J. A.; Nutter,
S. L.; Schneider, E.; Swordy, S. P.; Tarle, G.; Tomasch, A. D.;
Torbet, E.
Bibcode: 1997ICRC....2..373D
Altcode: 1997ICRC...25b.373D
No abstract at ADS
Title: A Measurement of the Cosmic Ray Positron Fraction at
Intermediate Energies
Authors: Musser, J.; Bower, C. R.; Barwick, S. W.; Schneider, E.;
Chaput, C.; Coutu, S.; McKee, S.; Nutter, S. L.; Tarle, G.; Tomasch,
A. D.; Knapp, J.; Muller, D.; Swordy, S. P.; Torbet, E.; Tang, K. K.;
Beatty, J. J.; de Nolfo, G.; Lowder, D. M.
Bibcode: 1996APS..MAY..B702M
Altcode:
We present preliminary results of a measurement of the Cosmic Ray
positron fraction obtained from the second balloon flight of the High
Energy Antimatter Telescope (HEAT). The HEAT instrument combines
a magnetic spectrometer with a transition radiation detector,
electromagnetic calorimeter, and time of flight counters. The data
from this flight provides a measurement of the positron fraction over
the energy range 1 < E < 50 GeV, extending the range explored
by the first HEAT flight to lower energies.
Title: A Semi-Analytical Method for the Evaluation of the Power
Spectrum of a Rotating Observer
Authors: Mueller, Daniel
Bibcode: 1995gr.qc....12038M
Altcode:
In this letter we propose a semi-analitical method of evaluation of
the power spectrum of a circular moving Unruh-type detector using
the method of residue and compare the spectrum with the already known
result in the relativistic limit.
Title: Performance of the HEAT spectrometer for cosmic ray electrons
and positrons
Authors: Muller, D.
Bibcode: 1995NIMPA.367...71M
Altcode:
A new detector system for observations of cosmic ray electrons and
positrons has been flown on a high altitude balloon in May 1994. The
instrumentation includes a superconducting magnet and a drift tube
hodoscope for the measurement of particle rigidities, and a combination
of transition radiation detectors, shower counters and a time-of-flight
system for particle identification and energy measurement. We will
discuss the performance of the individual components and demonstrate
that a reliable identification of the rare positron component has been
achieved up to 50 GeV.
Title: Application of UV-laser-diagnostics to combustion research
under zero-gravity
Authors: König, J.; Dinkelacker, F.; Eigenbrod, Ch.; Rath, H. J.;
Schröder, Th.; Albrecht, H.; Müller, D.; Triebel, W.
Bibcode: 1995AdSpR..16g.145K
Altcode: 1995AdSpR..16..145K
The application of modern laser diagnostical measurement techniques
for combustion research in earth-based laboratories has brought
essential experimental progress. In this paper the development of an
UV-laser system is described, which for the first time will allow
the application of two dimensional laser spectroscopic measurement
techniques for experiments at the drop tower ``Bremen''. The laser
system will be integrated at the top of the tower; the laser beam
follows the falling drop capsule and enters it from above. The drift
between capsule and laser beam has to be compensated with an accuracy
in the sub-mm range. Described are the laser-, control-, detection- and
data acquisition systems, first results of the experimental properties
and planned applications for experiments at the drop tower ``Bremen''.
Title: Cosmic Ray Positrons at High Energies: A New Measurement
Authors: Barwick, S. W.; Beatty, J. J.; Bower, C. R.; Chaput, C.;
Coutu, S.; de Nolfo, G.; Ficenec, D.; Knapp, J.; Lowder, D. M.; McKee,
S.; Müller, D.; Musser, J. A.; Nutter, S. L.; Schneider, E.; Swordy,
S. P.; Tang, K. K.; Tarlé, G.; Tomasch, A. D.; Torbet, E.
Bibcode: 1995PhRvL..75..390B
Altcode:
We present a new measurement of the cosmic-ray positron fraction
e+/\(e++e-\) obtained from the first
balloon flight of the High Energy Antimatter Telescope (HEAT). Using
a magnet spectrometer combined with a transition radiation detector,
an electromagnetic calorimeter, and time-of-flight counters we have
achieved a high degree of background rejection. Our results do not
indicate a major contribution to the positron flux from primary
sources. In particular, we see no evidence for the significant rise
in the positron fraction at energies above ~10 GeV previously reported.
Title: The Chemical Composition of Cosmic Rays in the Region of the
"Knee"
Authors: Gaisser, T. K.; Green, K. D.; Knapp, J.; Magnussen, N.;
Müller, D.; Nitz, D.; Plaga, R.; Stanev, T.; Swordy, S.; Yodh, G. B.
Bibcode: 1995pnac.conf..273G
Altcode:
No abstract at ADS
Title: The Relative Fluxes of Protons and Helium Nuclei up to
100 GeV/n
Authors: Swordy, S. P.; Barwick, S. W.; Beatty, J. J.; Bower, C. R.;
Chaput, C.; Coutu, S.; de Nolfo, G.; Ficenec, D.; Knapp, J.; Lowder,
D. M.; McKee, S.; Müller, D.; Musser, J. A.; Nutter, S. L.; Schneider,
E.; Tang, K. K.; Tarlé, Tomasch, A. D.; Torbet, E.
Bibcode: 1995ICRC....2..652S
Altcode: 1995ICRC...24b.652S
No abstract at ADS
Title: A New Measurement of the Positron Fraction at High Energies
Authors: Tarlé, G.; Barwick, S. W.; Beatty, J. J.; Bower, C. R.;
Chaput, C.; Coutu, S.; de Nolfo, G.; Ficenec, D.; Knapp, J.; Lowder,
D. M.; McKee, S.; Müller, D.; Musser, J. A.; Nutter, S. L.; Schneider,
E.; Swordy, S. P.; Tang, K. K.; Tomasch, A. D.; Torbet, E.
Bibcode: 1995ICRC....3...17T
Altcode: 1995ICRC...24c..17T
No abstract at ADS
Title: Flight Performance and Electron-Hadron Separation of the HEAT
- e±Experiment
Authors: Torbet, E.; Barwick, S. W.; Beatty, J. J.; Bower, C. R.;
Chaput, C.; Coutu, S.; de Nolfo, G.; Ficenec, D.; Knapp, J.; Lowder,
D. M.; McKee, S.; Müller, D.; Musser, J. A.; Nutter, S. L.; Schneider,
E.; Swordy, S. P.; Tang, K. K.; Tarlé, G.; Tomasch, A. D.
Bibcode: 1995ICRC....3..603T
Altcode: 1995ICRC...24c.603T
No abstract at ADS
Title: A new Ring Imaging Cherenkov Telescope for Measurements of
Light Cosmic Ray Nuclei
Authors: Ellithorpe, D.; Diehl, E.; Müller, D.; Swordy, S.
Bibcode: 1995ICRC....3..440E
Altcode: 1995ICRC...24c.440E
No abstract at ADS
Title: Measurement of the μ+/μ- Ratio as a
Function of Depth in the Atmosphere
Authors: Schneider, E.; Barwick, S. W.; Beatty, J. J.; Bower, C. R.;
Chaput, C.; Coutu, S.; deNolfo, G.; Ficenec, D.; Knapp, J.; Lowder,
D. M.; McKee, S.; Müller, D.; Musser, J. A.; Nutter S. L.; Swordy,
S. P.; Tang, K. K.; Tarlé, G.; Tomasch, A. D.; Torbet, E.
Bibcode: 1995ICRC....1..690S
Altcode: 1995ICRC...24a.690S
No abstract at ADS
Title: The Energy Spectrum of Cosmic Rays with the CASA-MIA Air
Shower Array
Authors: Borione, A.; Catanese, M.; Covault, C. E.; Cronin, J. W.;
Fick, B. E.; Forston, L. F.; Gibbs, K. G.; Glasmacher, M. A. K.; Green,
K. D.; Kieda, D. B.; Knapp, J.; Matthews, J.; Müller, D.; Newport,
B. J.; Nitz, D.; Ong, R. A.; Sinclair, D.; van der Velde, J. C.
Bibcode: 1995ICRC....2..744B
Altcode: 1995ICRC...24b.744B
No abstract at ADS
Title: Monte Carlo Calculations of Atmospheric Electrons Compared
with Data from HEAT
Authors: de Nolfo, G.; Barwick, S. W.; Beatty, J. J.; Bower, C. R;
Chaput, C.; Coutu, S.; Ficenec, D.; Knapp, J.; Lowder, D. M.; McKee,
S.; Müller, D.; Nutter, S. L.; Schneider, E.; Swordy, S. P.; Tang,
K. K.; Tarlé, G.; Tomasch, A. D.; Torbet, E.
Bibcode: 1995ICRC....1..589D
Altcode: 1995ICRC...24a.589D
No abstract at ADS
Title: The Cosmic Positron Fraction: Implications of a New Measurement
Authors: Müller, D.; Barwick, S. W.; Beatty, J. J.; Bower, C. R.;
Chaput, C.; Coutu, S.; de Nolfo, G.; Ficenec, D.; Knapp, J.; Lowder,
D. M.; McKee, S.; Musser, J. A.; Nutter, S. L.; Schneider, E.; Swordy,
S. P.; Tang, K. K.; Tarlé, G.; Tomasch, A. D.; Torbet, E.
Bibcode: 1995ICRC....3...13M
Altcode: 1995ICRC...24c..13M
No abstract at ADS
Title: Galactic Cosmic Rays Up to 10 TeV
Authors: Ormes, J. F.; Beatty, J.; Binns, W. R.; Wiedenbeck, M.;
Stephens, A.; Müller, D.; Barbier, L.; Stephens, A.; Salamon, M.;
Jones, F. C.; Seo, E. -S.; Streitmatter, R.
Bibcode: 1995pnac.conf..312O
Altcode:
No abstract at ADS
Title: A New Measurement of the Flux of the Light Cosmic-Ray Nuclei
at High Energies
Authors: Buckley, J.; Dwyer, J.; Mueller, D.; Swordy, S.; Tang, K. K.
Bibcode: 1994ApJ...429..736B
Altcode:
A new cosmic-ray detector utilizing a ring-imaging Cerenkov counter
to determine the energy of light cosmic-ray nuclei was flown on
high-altitude balloon from Fort Sumner, NM, in 1991 September. We
describe the design and performance of this instrument and discuss the
data analysis procedures. The measurement provides a new determination
of the absolute flux and differential energy spectrum of the primary
cosmic-ray species helium between 40 and 320 GeV/nucleon. The experiment
also yields the spectra of carbon and oxygen and some information on
the intensities of the secondary nuclei Li, Be, and B. A comparison
between our results and previous measurements of heavier nuclei (Z
greater than or equal to 4) from HEAO 3 and Spacelab 2 indicates good
consistency between these measurements. The data set is compared with
the results of a leaky box propagation model. We find good agreement
with this model if the abundance of helium relative to oxygen at the
source is taken to be 25 +/- 6 and if the source spectrum is given by
a power law in energy proportional to E-2.15.
Title: A large air shower array to search for astrophysical sources
emitting γ-rays with energies >=1014 eV
Authors: Borione, A.; Covault, C. E.; Cronin, J. W.; Fick, B. E.;
Gibbs, K. G.; Krimm, H. A.; Mascarenhas, N. C.; McKay, T. A.; Müller,
D.; Newport, B. J.; Ong, R. A.; Rosenberg, L. J.; Sanders, H.;
Catanese, M.; Ciampa, D.; Green, K. D.; Kolodziejczak, J.; Matthews,
J.; Nitz, D.; Sinclair, D.; van der Velde, J. C.
Bibcode: 1994NIMPA.346..329B
Altcode:
We describe the technical details and the performance of a large array
which detects both the electron and muon components in extensive air
showers with energies >= 1014 eV. The array was designed
to search for γ-rays from astrophysical sources. The background of
cosmic rays is reduced by the selection of muon poor events. The array
consists of 1089 scintillation detectors on the surface covering
an area of 0.23 km2 and 1024 scintillation counters
of 2.5 m2 each, buried 3 m below the surface for muon
detection. Each of the surface detectors has its own local electronics
and local data storage controlled by a microprocessor. The array is
located at Dugway, Utah USA (40.2°N, 112.8°W) where the average
atmospheric depth is 870 g/cm2.
Title: Observation of the shadows of the Moon and Sun using 100 TeV
cosmic rays
Authors: Borione, A.; Catanese, M.; Covault, C. E.; Cronin, J. W.;
Fick, B. E.; Gibbs, K. G.; Green, K. D.; Hauptfeld, S.; Kieda, D.;
Krimm, H. A.; Mascarenhas, N. C.; Matthews, J.; McKay, T. A.; Müller,
D.; Newport, B. J.; Nitz, D.; Ong, R. A.; Rosenberg, L. J.; Sinclair,
D.; van der Velde, J. C.
Bibcode: 1994PhRvD..49.1171B
Altcode:
The Chicago Air Shower Array has imaged the shadows of the Moon and Sun
and measured the angular diameter of the Moon with cosmic rays having
energies above about 100 TeV. The shadow of the Sun shows effects
attributed to the curvature of cosmic rays by the solar magnetic
field. This study verifies that our direction reconstruction has
no serious systematic errors, and provides a measure of the angular
resolution of the array.
Title: CASA-MIA: A ``precision'' EAS detector
Authors: Borione, A.; Cronin, J. W.; Covault, C. E.; Fick, B. E.;
Gibbs, K. G.; Krimm, H. A.; McKay, T. A.; Müller, D.; Newport, B. J.;
Ong, R. A.; Rosenberg, L. J.; Catanese, M.; Green, K. D.; Matthews,
J.; Nitz, D. F.; Sinclair, D.; van der Velde, J. C.; Kieda, D.
Bibcode: 1993AIPC..276..207B
Altcode:
The CASA-MIA detector was constructed to search for sources of UHE
neutral radiation. As such it has established limits well below those
of previously reported observations and of most contemporaneous
detectors. In addition to its primary mission, however, CASA-MIA
measures the lateral distribution of both electrons and muons in
EAS throughout a range of energies and with a degree of sampling not
previously available.
Title: Spatial Resolution Tests for the HEAT Cosmic-Ray Hodoscope
Authors: Tomasch, A.; Ficenec, D. J.; Barwick, S. W.; Beatty, J. J.;
Bower, C. R.; de Nolfo, G.; Ellithorpe, D.; Levin, D.; Lowder, D. M.;
Lynch, J.; McKee, S.; Miller, T.; Müller, D.; Musser, J. A.; Nutter,
S.; Price, P. B.; Richards, A.; Schneider, E.; Swordy, S.; Tang,
K. K.; Tarlé, G.; Torbet, E.
Bibcode: 1993ICRC....2..492T
Altcode: 1993ICRC...23b.492T
No abstract at ADS
Title: The Energy Spectrum and Flux of Cosmic Ray Helium at High
Energy
Authors: Dwyer, J.; Buckley, J.; Müller, D.; Swordy, S.; Tang, K. K.
Bibcode: 1993ICRC....1..587D
Altcode: 1993ICRC...23a.587D
No abstract at ADS
Title: A Search for Ultra-High Energy Gamma Ray Emission from Active
Galactic Nuclei with CASA-MIA
Authors: Borione, A.; Catanese, M.; Covault, C. E.; Cronin, J. W.;
Fick, B. E.; Gibbs, K. G.; Green, K. D.; Kieda, D.; McKay, T. A.;
Matthews, J.; Müller, D.; Newport, B. J.; Nitz, D.; Ong, R. A.;
Rosenberg, L. J.; Sinclair, D.; van der Velde, J. C.
Bibcode: 1993ICRC....1..424B
Altcode: 1993ICRC...23a.424B
No abstract at ADS
Title: Fluxes and Relative Abundances of Light Cosmic Ray Nuclei
above 40 GeV/amu
Authors: Buckley, J.; Dwyer, J.; Müller, D.; Swordy, S.; Tang, K. K.
Bibcode: 1993ICRC....1..599B
Altcode: 1993ICRC...23a.599B
No abstract at ADS
Title: HEAT-e±: Accelerator Calibration Results
Authors: Torbet, E.; Barwick, S. W.; Beatty, J.; Bower, C. R.; de
Nolfo, G.; Ellithorpe, D.; Ficenec, D.; Levin, D.; Lowder, D. M.;
Lynch, J.; McKee, S.; Miller, T.; Müller, D.; Musser, J. A.; Nutter,
S.; Price, P. B.; Richards, A.; Schneider, E.; Swordy, S.; Tang,
K. K.; Tarlé, G.; Tomasch, A. D.
Bibcode: 1993ICRC....2..496T
Altcode: 1993ICRC...23b.496T
No abstract at ADS
Title: Understanding the message of cosmic rays: direct measurements
of their composition at high energies
Authors: Müller, D.
Bibcode: 1993foap.conf..391M
Altcode:
No abstract at ADS
Title: A Procedure to Obtain the Cosmic Ray Energy Spectrum from
CASA-MIA Data
Authors: Borione, A.; Catanese, M.; Covault, C. E.; Cronin, J. W.;
Fick, B. E.; Gibbs, K. G.; Green, K. D.; Kieda, D.; McKay, T. A.;
Matthews, J.; Müller, D.; Newport, B. J.; Nitz, D.; Ong, R. A.;
Rosenberg, L. J.; Sinclair, D.; van der Velde, J. C.
Bibcode: 1993ICRC....2..112B
Altcode: 1993ICRC...23b.112B
No abstract at ADS
Title: Ring Imaging Cerenkov Counters: Flight Performance and Future
Applications
Authors: Swordy, S.; Buckley, J. H.; Dwyer J.; Müller, D.; Tang, K. K.
Bibcode: 1993ICRC....2..500S
Altcode: 1993ICRC...23b.500S
No abstract at ADS
Title: A ring imaging Cherenkov telescope for observations of high
energy cosmic rays
Authors: Buckley, J.; Dwyer, J.; Müller, D.; Swordy, S.; Tang, K. K.
Bibcode: 1992NIMPA.323..380B
Altcode:
We describe a ring imaging Cherenkov counter for high altitude
balloon flights designed to measure the energy spectra of cosmic
ray nuclei above 40 GeV/amu. The instrument has a 3 m long nitrogen
gas radiator at 1 atm, a spherical and planar mirror system, and ~
2.2 m2 of TMAE/ethane photon detecting drift chambers with
fused silica windows in the focal plane. The mirror system is designed
such that cosmic ray particles which trigger the instrument cannot
pass through the photon detectors. Cosmic ray trajectories through
the instrument are determined by eight low mass drift chambers, each
of 2.2 m2 area, which predict the ring image center to +/-
0.76 mm. Ground tests with cosmic ray muons prior to the flight show
that the detectors see about two photoelectrons from a high energy
singly charged particle. Special efforts were made to ensure stable
operation and constant temperatures and pressures under remote control
during the balloon flight. In September 1991, this instrument flew for
31 h at an altitude of ~ 37 km and collected cosmic ray events which
were transmitted to a ground station for recording. Now at the
University of Utah, Salt Lake City, UT 84112, USA.
Title: A Search for Ultra-High Energy Gamma Rays from EGRET Blazars
Authors: Covault, C. E.; Borione, A.; Cronin, J. W.; Fick, B. E.;
Gibbs, K. G.; Hauptfeld, S.; McKay, T. A.; Muller, D.; Newport, B. J.;
Ong, R. A.; Rosenberg, L. J.; Catanese, M.; Green, K. D.; Matthews,
J.; Nitz, D.; Sinclair, D.; van der Velde, J. C.; Kieda, D. B.
Bibcode: 1992AAS...181.2108C
Altcode: 1992BAAS...24.1156C
Recently, the EGRET experiment aboard the Compton Gamma Ray Observatory
has reported the detection of strong episodic emission from over
15 extra-galactic sources, typically radio-loud quasars and BL Lac
objects. These sources are generally classified as ``blazars'',
with significant gamma-ray energy which may be beamed towards
the observer. At least one of these objects, Mrk 421, has also been
detected at energies ~ 1 TeV by the Whipple observatory. Depending on
the details of intergalactic absorption, it may be possible to detect
such sources at energies above 50 TeV with large air shower arrays. We
present a progress report on a search for Ultra High Energy (UHE)
gamma rays from extra-galactic sources, such as the EGRET blazars,
using the UMC air shower facility at Dugway, Utah. The facility is
comprised of the large-area Chicago Air Shower Array (CASA) operating
in coincidence with the underground Michigan Muon array (MIA). We
describe our analysis approach for Mrk 421 and other AGN which are
under observation by CASA-MIA in the northern hemisphere. We anticipate
a sensitivity of ~ 3*E(-14) ph cm(-2) s(-1) above 80 TeV to flux from
Mrk 421 after one full year's observations.
Title: Search for discrete sources of 100 TeV gamma radiation
Authors: Cronin, J. W.; Fick, B. E.; Gibbs, K. G.; Krimm, H. A.;
Mascarenhas, N. C.; McKay, T. A.; Müller, D.; Newport, B. J.;
Ong, R. A.; Rosenberg, L. J.; Green, K. D.; Matthews, J.; Nitz, D.;
Sinclair, D.; van der Velde, J. C.
Bibcode: 1992PhRvD..45.4385C
Altcode:
The Chicago Air Shower Array is a large-area ground-based detector
designed to observe extensive air showers produced by primary
particles with energy >~100 TeV. It operates in coincidence with the
underground Michigan Muon Array. Data taken during 1989 are examined for
evidence of continuous and pulsed emission from localized regions of the
sky. The x-ray sources Cygnus X-3, Hercules X-1, and the Crab Nebula
and pulsar are examined for steady and periodic γ-ray emission. To
search for previously unknown compact sources, the background of cosmic
rays is estimated over the sky between declinations +5° and +90° and
enhancement is sought in small angular bins. There is no evidence for
a significant excess from any of these searches, and flux limits are
presented as a function of declination and muon content.
Title: A search for astrophysical point sources of 100 TeV gamma
rays by the UMC collaboration
Authors: McKay, T. A.; Borione, A.; Catanese, M.; Covault, C. E.;
Cronin, J. W.; Fick, B. E.; Gibbs, K. G.; Green, K. D.; Hauptfeld, S.;
Kieda, D.; Krimm, H. A.; Mascarenhas, N. M.; Matthews, J.; Müller,
D.; Newport, B. J.; Nitz, D.; Ong, R. A.; Rosenberg, L. J.; Sinclair,
D.; van der Velde, J. C.
Bibcode: 1992AIPC..272.1203M
Altcode:
The CASA-MIA experiment is a very large extensive air shower detector
with good angular resolution. This instrument has been used to search
the entire visible sky for astrophysical point sources of 100 TeV gamma
rays. Approximately 90% of the isotropic charged cosmic ray background
is rejected by measuring the muon content of the showers. Stringent
limits are placed on the possible flux of 100 TeV sources across a
large part of the Northern sky.
Title: A Search for Diffuse Cosmic Gamma-Rays 100 TeV from Giant
Molecular Cloud Regions and the Galactic Plane
Authors: Covault, C. E.; Aharonian, F. A.; Borione, A.; Cronin, J. W.;
Fick, B. E.; Gibbs, K. G.; Hauptfeld, S.; McKay, T. A.; Müller, D.;
Newport, B. J.; Ong, R. A.; Rosenberg, L. J.; Cantanese, M.; Green,
K. D.; Matthews, J.; Nitz, D.; Sinclair, D.; van der Velde, J. C.
Bibcode: 1991BAAS...23.1471C
Altcode:
No abstract at ADS
Title: A Search for the UHE Sources of Neutral Radiation
Authors: Nitz, D.; Catanese, M.; Green, K. D.; Matthews, J.; Sinclair,
D.; van der Velde, J. C.; Borione, A.; Covault, C. E.; Cronin, J. W.;
Fick, B. E.; Gibbs, K. G.; Krimm, H. A.; Mascarenhas, N. C.; McKay,
T. A.; Müller, D.; Newport, B. J.; Ong, R. A.; Rosenberg, L. J.
Bibcode: 1991ICRC....1..448N
Altcode: 1991ICRC...22a.448N
No abstract at ADS
Title: HEAT: A High Energy Antimatter Telescope
Authors: Müller, D.; Ahlen, S. P.; Barwick, S. W.; Beatty, J. J.;
Borione, A.; Ficenec, D.; Levin, D.; Lowder, D. M.; McKee, S.; Miller,
T.; Musser, J. A.; Price, P. B.; Swordy, S.; Tang, K. K.; Tarlé,
G.; Tomasch, A. D.; Torbet, E.
Bibcode: 1991ICRC....2..177M
Altcode: 1991ICRC...22b.177M
No abstract at ADS
Title: Galactic Propagation and Source Composition of High Energy
Cosmic Rays
Authors: Meyer, P.; Grunsfeld, J.; L'Heureux, J.; Müller, D.; Swordy,
S. P.
Bibcode: 1991ICRC....2...21M
Altcode: 1991ICRC...22b..21M
No abstract at ADS
Title: A Search for 100 TeV Gamma-Ray Emission from Cygnus X-3
Authors: Ong, R. A.; Borione, A.; Covault, C. E.; Cronin, J. W.; Fick,
B. E.; Gibbs, K. G.; Krimm, H. A.; Mascarenhas, N. C.; McKay, T. A.;
Müller, D.; Newport, B. J.; Rosenberg, L. J.; Catanese, M.; Green,
K. D.; Matthews, J.; Nitz, D.; Sinclair, D.; van der Velde, J. C.
Bibcode: 1991ICRC....1..273O
Altcode: 1991ICRC...22a.273O
No abstract at ADS
Title: A Search for 100 TeV Emission from the Crab Nebula and Pulsar
Using the UMC Detector
Authors: Gibbs, K. G.; Borione, A.; Covault, C. E.; Cronin, J. W.;
Fick, B. E.; Krimm, H. A.; Mascarenhas, N. C.; McKay, T. A.; Müller,
D.; Newport, B. J.; Ong, R. A.; Rosenberg, L. J.; Catanese, M.; Green,
K. D.; Matthews, J.; Nitz, D.; Sinclair, D.; van der Velde, J. C.
Bibcode: 1991ICRC....1..208G
Altcode: 1991ICRC...22a.208G
No abstract at ADS
Title: A Search for Discrete Sources of Neutral Radiation Above
1014 eV Using The 49 Element UMC Prototype
Authors: Krimm, H. A.; Cronin, J. W.; Fick, B. E.; Gibbs, K. G.;
Mascarenhas, N. C.; McKay, T. A.; Müller, D.; Newport, B. J.;
Ong, R. A.; Rosenberg, L. J.; Green, K. D.; Matthews, J.; Nitz, D.;
Sinclair, D.; van der Velde, J. C.
Bibcode: 1991ICRC....1..432K
Altcode: 1991ICRC...22a.432K
No abstract at ADS
Title: The Composition of the Arriving Cosmic Ray Flux at TeV Energies
and Beyond
Authors: Müller, D.; Grunsfeld, J.; L'Heureux, J.; Meyer, P.;
Swordy, S.
Bibcode: 1991ICRC....2...25M
Altcode: 1991ICRC...22b..25M
No abstract at ADS
Title: Study of Extensive Air Showers (EAS) Detected with the Fly's
Eye and the UMC Air Shower Array
Authors: Green, K. D.; Catanese, M.; Matthews, J.; Nitz, D.; Sinclair,
D.; van der Velde, J. C.; Borione, A.; Covault, C. E.; Cronin, J. W.;
Fick, B. E.; Gibbs, K. G.; Krimm, H. A.; Mascarenhas, N. C.; McKay,
T. A.; Müller, D.; Newport, B. J.; Ong, R. A.; Rosenberg, L. J.;
Cooper, R. G.; Corbató, S. C.; Dai, H. Y.; Dawson, B.; Emerson,
B. L.; Elbert, J. W.; Kieda, D.; Ko, S.; Loh, E. C.; Luo, M. Z.;
Salamon, M. H.; Sokolsky, P. V.; Sommers, P. D.; Smith, J. D.; Tang,
S. B.; Thomas, S. B.
Bibcode: 1991ICRC....4..347G
Altcode: 1991ICRC...22d.347G
No abstract at ADS
Title: The Performance of a New Cerenkov Telescope for Observations
of Light Cosmic Ray Nuclei at High Energies
Authors: Buckley, J.; Dwyer, J.; Müller, D.; Swordy, S. P.; Tan,
K. -K.
Bibcode: 1991ICRC....2..579B
Altcode: 1991ICRC...22b.579B
No abstract at ADS
Title: A Search For Continuous 100 TeV Gamma-Ray Emission from
Hercules X-1
Authors: McKay, T. A.; Borione, A.; Covault, C. E.; Cronin, J. W.;
Fick, B. E.; Gibbs, K. G.; Krimm, H. A.; Mascarenhas, N. C.; Müller,
D.; Newport, B. J.; Ong, R. A.; Rosenberg, L. J.; Catanese, M.; Green,
K. D.; Matthews, J.; Nitz, D.; Sinclair, D.; van der Velde, J. C.
Bibcode: 1991ICRC....1..230M
Altcode: 1991ICRC...22a.230M
No abstract at ADS
Title: The Construction of a Large Ring Imaging Cerenkov Counter
(RICH) for Balloon Borne Measurements
Authors: Dwyer, J.; Buckley, J.; Müller, D.; Swordy, S. P.; Tan,
K. -K.
Bibcode: 1991ICRC....2..575D
Altcode: 1991ICRC...22b.575D
No abstract at ADS
Title: A Search for 100 TeV Gamma-Ray Emission From Cygnus X-3 Using
the 49 Elements UMC Array
Authors: Krimm, H. A.; Cronin, J. W.; Fick, B. E.; Gibbs, K. G.;
Mascarenhas, N. C.; McKay, T. A.; Müller, D.; Newport, B. J.;
Ong, R. A.; Rosenberg, L. J.; Green, K. D.; Matthews, J.; Nitz, D.;
Sinclair, D.; van der Velde, J. C.
Bibcode: 1991ICRC....1..269K
Altcode: 1991ICRC...22a.269K
No abstract at ADS
Title: UMC: a sensitive new detector for UHE gamma-ray astronomy
Authors: Fick, B. E.; Borione, A.; Covault, C. E.; Cronin, J. W.;
Gibbs, K. G.; Krimm, H. A.; Mascarenhas, N. C.; McKay, T. A.; Muller,
D.; Newport, B. J.; Ong, R. A.; Rosenberg, L. J.; Catatnese, M.; Green,
K. D.; Matthews, J.; Nitz, D.; Sinclair, D.; Van der Velde, J. C.
Bibcode: 1991ICRC....2..728F
Altcode: 1991ICRC...22b.728F
No abstract at ADS
Title: Spectra and Composition Studies With The UMC Detector
Authors: Matthews, J.; Catanese, M.; Green, K. D.; Nitz, D.; Sinclair,
D.; van der Velde, J. C.; Borione, A.; Covault, C. E.; Cronin, J. W.;
Fick, B. E.; Gibbs, K. G.; Krimm, H. A.; Mascarenhas, N. C.; McKay,
T. A.; Müller, D.; Newport, B. J.; Ong, R. A.; Rosenberg, L. J.
Bibcode: 1991ICRC....2..105M
Altcode: 1991ICRC...22b.105M
No abstract at ADS
Title: A New Superconducting Magnet Based Rigidity Spectrometer for
the HEAT Balloon Instrument
Authors: Tomasch, A. D.; Ahlen, S. P.; Barwick, S. W.; Beatty, J. J.;
Borione, A.; Ficenec, D.; Levin, D.; Lowder, D. M.; Mckee, S.; Miller,
T.; Müller, D.; Musser, J. A.; Price, P. B.; Robbins, J. A.; Swordy,
S.; Tang, K. K.; Tarlé, G.; Torbet, E.
Bibcode: 1991ICRC....2..181T
Altcode: 1991ICRC...22b.181T
No abstract at ADS
Title: Muon and Electron Lateral Distributions in EAS from
1014 to 1016 eV as Observed by the UMC Detector
Authors: van der Velde, J. C.; Catanese, M.; Green, K. D.; Matthews,
J.; Nitz, D.; Sinclair, D.; Borione, A.; Covault, C. E.; Cronin,
J. W.; Fick, D. E.; Gibbs, K. G.; Krimm, H. A.; Mascarenhas, N. C.;
McKay, T. A.; Müller, D.; Newport, B. J.; Ong, R. A.; Rosenberg, L. J.
Bibcode: 1991ICRC....4..311V
Altcode: 1991ICRC...22d.311V
No abstract at ADS
Title: A Search for Diffuse Sources of 100 TeV Gamma-Ray Emission
Authors: Covault, C. E.; Borione, A.; Cronin, J. W.; Fick, B. E.;
Gibbs, K. G.; Krimm, H. A.; Mascarenhas, N. C.; McKay, T. A.; Müller,
D.; Newport, B. J.; Ong, R. A.; Rosenberg, L. J.; Catanese, M.; Green,
K. D.; Matthews, J.; Nitz, D.; Sinclair, D.; van der Velde, J. C.
Bibcode: 1991ICRC....1..420C
Altcode: 1991ICRC...22a.420C
No abstract at ADS
Title: New orbits for WDS 02231+7021, WDS 05373+6642, WDS 06425+6612
WDS 22356+5413.
Authors: Muller
Bibcode: 1991IAUDS.114....1M
Altcode:
No abstract at ADS
Title: Design and operation of the Chicago air shower array
Authors: Rosenberg, L. J.; Cronin, J. W.; Fick, B. E.; Gibbs, K. G.;
Krimm, H. A.; Mascarenhas, N. C.; McKay, T. A.; Müller, D.; Newport,
B. J.; Ong, R. A.; Wiedenbeck, M. E.; Green, K. D.; Matthews, J.;
Nitz, D.; Sinclair, D.; van der Velde, J. C.
Bibcode: 1991AIPC..220..111R
Altcode: 1991hegr.proc..111R
The Chicago Air Shower Array (CASA) is a large-area surface scintillator
array designed to study PeV sources of cosmic rays. The complete
detector will consist of 1089 detector stations, distributed on a
square 15 m grid. We have operated an array of 49 stations for much of
the 1989 calendar year, an array of 529 stations for much of 1990, and
the balance of the 1089 stations will be operating in early 1991. This
surface array, together with the University of Michigan underground
muon detectors (MIA), and the University of Utah atmospheric Čerenkov
telescopes and Fly's Eye air fluorescence detector, constitute a
uniquely powerful instrument, dubbed the Utah Michigan Chicago (UMC)
experiment, for the study of PeV sources. We report here the performance
and current status of these detectors.
Title: Preliminary results from the Chicago air shower array and
the Michigan muon array
Authors: Krimm, H. A.; Cronin, J. W.; Fick, B. E.; Gibbs, K. G.;
Mascarenhas, N. C.; McKay, T. A.; Müller, D.; Newport, B. J.; Ong,
R. A.; Rosenberg, L. J.; Wiedenbeck, M. E.; Green, K. D.; Matthews,
J.; Nitz, D.; Sinclair, D.; van der Velde, J. C.
Bibcode: 1991AIPC..220..122K
Altcode: 1991hegr.proc..122K
The Chicago Air Shower Array (CASA) is a large area surface array
designed to detect extensive air showers (EAS) produced by primaries
with energy ∼100 TeV. It operates in coincidence with the underground
Michigan Muon Array (MIA). Preliminary results are presented from a
search for steady emission and daily emission from three astrophysical
sources: Cygnus X-3, Hercules X-1, and the Crab nebula and pulsar. There
is no evidence for a significant signal from any of these sources in
the 1989 data.
Title: A detector for cosmic-ray nuclei at very high energies
Authors: L'Heureux, J.; Grunsfeld, J. M.; Meyer, P.; Müller, D.;
Swordy, S. P.
Bibcode: 1990NIMPA.295..246L
Altcode: 1990nimp..295..246L
We discuss the design and performance of a detector system that was
developed to measure the elemental abundance distribution of cosmic-ray
nuclei with energies up to several TeV/amu. The low flux of high-energy
cosmic rays requires an instrument with large geometric factor, but
of reasonably low weight to be carried on the Space Shuttle. To meet
these conditions we designed a counter telescope with gas Cherenkov
counters and transition radiation detectors for particle energy
measurements. Scintillation counters determine the particle's atomic
number. We describe design and performance of these individual detectors
and their interplay in the instrument. The instrument was flown for
eight days in the Spacelab-2 configuration on the Space Shuttle in
July/August 1985.
Title: The NASA cosmic ray program for the 1990's and beyond Interim
report of the NASA Cosmic Ray Program Working Group
Authors: Ahlen, S. P.; Binns, W. R.; Cherry, M. L.; Gaisser, T. K.;
Jones, W. V.; Ling, J. C.; Mewaldt, R. A.; Muller, D.; Ormes, J. O.;
Ramaty, R.; Stone, E. C.; Waddington, C. J.; Webber, W. R.; Miedenbeck,
M. E.
Bibcode: 1990AIPC..203....3A
Altcode: 1990pacr.rept....3A
The interim report of the 1989 NASA Cosmic Ray Program Working Group is
presented. The report summarizes the cosmic ray program for the 1990's,
including the recently approved ACE, Astromag, HNC, POEMS, and SAMPEX
missions, as well as other key elements of the program. New science
themes and candidate missions are identified for the first part of
the 21st Century, including objectives that might be addressed as
part of the Human Exploration Initiative. Among the suggested new
thrusts for the 21st century are: an Interstellar Probe into the
nearby interstellar medium; a Lunar-Based Calorimeter to measure
the cosmic ray composition near ~1016 eV; high precision element
and isotope spectroscopy of ultraheavy (Z>=30) elements; and new,
more sensitive, studies of impulsive solar flare events.
Title: Development of a Ring Imaging Cerenkov Counter For Cosmic
Ray Measurements
Authors: Buckley, J.; Dwyer, J.; Müller, D.; Swordy, P. S.; Tang,
K. -K.
Bibcode: 1990ICRC....4..406B
Altcode: 1989ICRC....4..406B; 1990ICRC...21d.406B
No abstract at ADS
Title: Operation and Performance of the Chicago Air Shower Array
Authors: Newport, J. B.; Ong, A. R.; Rosenberg, J. L.; Sanders,
H.; Wiedenbeck, E. M.; Cronin, W. J.; Gibbs, G. K.; Krimm, A. H.;
Mascarenhas, C. N.; McKay, A. T.; Müller, D.
Bibcode: 1990ICRC....4..310N
Altcode: 1990ICRC...21d.310N; 1989ICRC....4..310N
No abstract at ADS
Title: Design of the Chicago Air Shower Array
Authors: Gibbs, G. K.; Haar, P.; Krimm, A. H.; Mascarenhas, C. N.;
McKay, A. T.; Müller, D.; Newport, J. B.; Ong, A. R.; Rosenberg,
J. L.; Wiedenbeck, E. M.; Christensen, K.; Cronin, W. J.
Bibcode: 1990ICRC....4..306G
Altcode: 1989ICRC....4..306G; 1990ICRC...21d.306G
No abstract at ADS
Title: The Cosmic Ray Positron Enigma
Authors: Müller, D.; Tang, K. K.
Bibcode: 1990ICRC....3..249M
Altcode: 1990ICRC...21c.249M; 1989ICRC....3..249M
No abstract at ADS
Title: Source Spectra of Primary Cosmic Rays
Authors: Grunsfeld, J. M.; L'Heureux, J.; Meyer, P.; Müller, D.;
Swordy, P. S.
Bibcode: 1990ICRC....3...69G
Altcode: 1990ICRC...21c..69G; 1989ICRC....3...69G
No abstract at ADS
Title: Preliminary Results from the Chicago Air Shower Array
Authors: Ong, A. R.; Rosenberg, J. L.; Wiedenbeck, E. M.; Cronin,
W. J.; Gibbs, G. K.; Krimm, A. H.; Mascarenhas, C. N.; McKay, A. T.;
Muller, D.; Newport, J. B.
Bibcode: 1990ICRC....2..357O
Altcode: 1990ICRC...21b.357O; 1989ICRC....2..357O
No abstract at ADS
Title: The Response of Transition Radiation Detectors to Heavy Cosmic
Ray Nuclei at Very High Energies
Authors: Swordy, P. S.; Grunsfeld, J.; L'Heureux, J.; Meyer, P.;
Müller, D.; Tang, K. -K.
Bibcode: 1990ICRC....4..381S
Altcode: 1989ICRC....4..381S; 1990ICRC...21d.381S
No abstract at ADS
Title: Relative Abundances of Secondary and Primary Cosmic Rays at
High Energies
Authors: Swordy, P. S.; Müller, D.; Meyer, P.; L'Heureux, J.;
Grunsfeld, J. M.
Bibcode: 1990ICRC....3...93S
Altcode: 1990ICRC...21c..93S; 1989ICRC....3...93S
No abstract at ADS
Title: A detector for cosmic-ray nuclei at very high energies
Authors: L'Heureux, J.; Grunsfeld, J. M.; Meyer, P.; Mueller, D.;
Swordy, S. P.
Bibcode: 1990nimp..295..246L
Altcode:
The design and performance of a detector system that was developed to
measure the elemental abundance distribution of cosmic-ray nuclei with
energies up to several TeV/amu is discussed. The low flux of high-energy
cosmic rays requires an instrument with large geometric factor, but
of reasonably low weight to be carried on the Space Shuttle. To meet
these conditions, a counter telescope was designed with gas Cherenkov
counters and transition radiation detectors for particle energy
measurements. Scintillation counters determine the particle's atomic
number. The design and performance of these individual detectors and
their interplay in the instrument are described. The instrument was
flown for eight days in the Spacelab-2 configuration on the Space
Shuttle in July/August 1985.
Title: Propagation of cosmic ray nuclei above 50 GeV/amu
Authors: Meyer, P.; Grunsfeld, J.; L'Heureux, J.; Swordy, S.;
Muller, D.
Bibcode: 1989AdSpR...9l.143M
Altcode: 1989AdSpR...9..143M
It is now well-known that the relative abundance of secondary
cosmic ray nuclei which are produced by spallation in interstellar
space depends on energies. The mechanism responsible for this energy
dependence are not well understood because of the scarcity of data on
the cosmic ray composition at energy above 50 GeV/amu. The University
of Chicago experiment on the Spacelab-2 flown by the Space Shuttle in
1985 is aimed at the measurement of the elemental composition in this
unexplored energy regime. Our latest results on the energy dependence
of the secondary to primary abundance ratio using the pairs of elements
B,C and N,O, are discussed.
Title: The Abundance of Spallation Produced Nuclei at High Energies
Authors: Meyer, P.; Grunsfeld, J.; L'Heureux, J.; Swordy, S. P.;
Muller, D.
Bibcode: 1987ICRC....1..338M
Altcode: 1987ICRC...20a.338M; 1987ICRC....1..338G
No abstract at ADS
Title: The Energy Spectra of Primary Cosmic Ray Nuclei up to 1
Tev/nucleon
Authors: Muller, D.; Grunsfeld, J.; L'Heureux, J.; Meyer, P.; Swordy,
S. P.
Bibcode: 1987ICRC....1..334M
Altcode: 1987ICRC...20a.334M; 1987ICRC....1..334G
No abstract at ADS
Title: The Positron Fraction in the Cosmic Radiation: Interpretation
of a Recent Measurement
Authors: Tang, K. K.; Muller, D.
Bibcode: 1987ICRC....2...88T
Altcode: 1987ICRC...20b..88T; 1987ICRC....2...88M
No abstract at ADS
Title: High Energy Cosmic Rays: Interpretation of Recent Results
Authors: Swordy, S. P.; L'Heureux, J.; Meyer, P.; Muller, D.;
Grunsfeld, J.
Bibcode: 1987ICRC....1..337S
Altcode: 1987ICRC...20a.337S; 1987ICRC....1..337G
No abstract at ADS
Title: The High Energy Cosmic Ray Experiment on SPACELAB-2: Detector
Performance Calibrations and Data Reduction
Authors: L'Heureux, J.; Grunsfeld, J.; Meyer, P.; Muller, D.; Swordy,
S. P.
Bibcode: 1987ICRC....2..366L
Altcode: 1987ICRC...20b.366L; 1987ICRC....2..366G
No abstract at ADS
Title: The Detection of Cosmic Ray Nuclei at Very High Energies
Authors: Müller, D.
Bibcode: 1986BAAS...18..673M
Altcode:
No abstract at ADS
Title: A Observation of Cosmic Ray Positrons from 10-20 GEV
Authors: Mueller, D.; Tang, J.
Bibcode: 1985ICRC....2..378M
Altcode: 1985ICRC...19b.378M
A balloon flight of the University of Chicago electron telescope was
performed. Making use of the east-west asymmetry in the geomagnetic
cut off rigidity, the cosmic ray positrons and negatrons were
separated over the range 10 GeV to 20 GeV. The positron to electron
ratio, e+/(e++e-), was measured to be 17% + or - 5%, significantly
higher than the ratio measured in the 1 GeV to 10 GeV range by other
experiments. This increase appears to suggest that either a primary
component of positrons become significant above 10 GeV, or that the
spectrum of primary negatrons decreases above 10 GeV more sharply than
that of secondary positrons.
Title: Cerenkov counters for high energy nuclei: Some new developments
Authors: Swordy, S. P.; Muller, D.
Bibcode: 1985ICRC....3..266S
Altcode: 1985ICRC...19c.266S
A method to determine with gas Cerenkov counters the Lorentz factor,
gamma = E/mc, of cosmic ray nuclei with high accuracy over the
range gamma approx. 20 to 100 is discussed. The measurement of
the Cerenkov emission angle theta, by use of a suitable imaging
system is considered. Imaging counters, the ring imaging Cerenkov
counters (RICH), were developed for use on accelerators. The image
of off-axis particles to determine the amount of image distortion as
a function of the direction of the incoming nucleus is examined and
an acceptance solid angle, relative to the optical axis, within which
the nucleus produces an image with an acceptable level of distortion
is defined. The properties of the image, which becomes elliptical,
for off-axis particles are analyzed.
Title: The development of a high energy cosmic ray detector for
Spacelab-2.
Authors: Lheureux, J.; Meyer, P.; Mueller, D.; Swordy, S. P.
Bibcode: 1985ICRC....3..276L
Altcode: 1985ICRC...19c.276L
A large cosmic ray detector aimed at measurements of the energy spectra
and of the elemental abundances of cosmic ray nuclei at very high
energies, up to several TeV/nucleon was constructed. The instrument
is an electronic counter telescope with a geometric factor of 5 sq
ster. It accomplishes measurements of the particle energies through the
use of gas Cerenkov counters and of transition radiation detectors. The
solutions of a number of technological problems that are encountered
when developing such instrumentation for Shuttle missions are discussed.
Title: Detectors for High Energy Cosmic Rays on Spacelab
Authors: Lheureux, J.; Meyer, P.; Muller, D.; Swordy, S.
Bibcode: 1985crhe.work..310L
Altcode:
Two instruments designed to determine the spectra of the individual
cosmic-ray components at very high energies are described. One of these
(CRNE) uses a combination of gas Cerenkov counters and transition
radiation detectors for the cosmic-ray nuclei lithium to nickel;
the other (TRIC) is optimized for the light cosmic rays (electrons,
protons, helium) and uses a transition-radiation/ionization-calorimeter
combination. The CRNE instrument, constructed at the University of
Chicago, was delivered to NASA for a first Shuttle flight on Spacelab-2
in summer 1985. Some of the technical and programmatic requirements
encountered during the hardware construction and integration are
discussed, and the expected scientific return and the prospects of
using such instrumentation on the Space Station are considered.
Title: A Magnet Spectrometer Facility: Rationale and Science Themes
Authors: Muller, D.
Bibcode: 1985crhe.work..148M
Altcode:
The construction of a cosmic-ray facility is proposed. It consists of a
large superconducting magnet spectrometer combined with interchangeable
detector systems. This facility will address a number of significant
topics in cosmic-ray astrophysics, such as the search for antiprotons
and antimatter, measurements of electrons and positrons, precision
measurements of energy spectra of cosmic-ray nuclei, determination of
isotopic abundances at high energies, and observations of high-energy
nucleus-nucleus interactions. The magnet-spectrometer facility will
make use of the capabilities of the Space Station, such as assembly
and servicing in space, and thus planning and design efforts for the
facility should proceed simultaneously with the definition work for
the Space Station. The importance of an ongoing program of detector
development at the participating institutions is stressed.
Title: Coded Aperture Imaging of X-Ray and Gamma-Ray Sources
Authors: Kroeger, R.; Muller, D.
Bibcode: 1983ICRC....8....1K
Altcode: 1983ICRC...18h...1K
Coded aperture telescopes employing arrays of a small number of discrete
detector elements for hard X-rays or gamma-rays are discussed. Aperture
patterns are described that permit a unique reconstruction of the
image with high contrast, and that exhibit a specific rotational
antisymmetry to suppress systematic distortions. It is shown that
high flux sensitivity can be achieved in this fashion as well as good
angular resolution.
Title: The propagation of cosmic rays in the Galaxy: further evidence
for a "nested leaky box".
Authors: Tang, J.; Muller, D.
Bibcode: 1983ICRC....9..251T
Altcode: 1983ICRC...18i.251T
Recent data on the spectrum of cosmic ray electrons indicate that the
containment of electrons in the galaxy is independent of energy. On the
other hand, cosmic ray nuclei are known to propagate through an energy
dependent pathlength. Both results can be accounted for in a propagation
model in the form of a double leaky box similar to that suggested by
Cowsik and Wilson (1975). The model requires few adjustable parameters
but assumes that all primary cosmic ray species are accelerated in the
form of a common power law in momentum above 100 MeV/c. It is shown
that this model describes correctly the observed nuclear composition
and the energy spectra of electrons and nuclei.
Title: The Spectrum of High Energy Cosmic-Ray Electrons: Results
and Interpretation
Authors: Muller, D.; Tang, J.
Bibcode: 1983ICRC....2...60M
Altcode: 1983ICRC...18b..60M
Results of a measurement of high energy cosmic-ray electrons that was
performed with a balloon-borne transition radiation/shower detector
telescope are presented. The data cover the energy range from 5 to
300 GeV. The interstellar spectrum below 10 GeV, which is affected
by solar modulation, is derived through analysis of the nonthermal
galactic radio emission, and extended to lower energies (about 300
MeV). The interstellar differential spectrum is described by a power
law dependence on E with an index of -1.4 below 2 GeV, but attaining
a slope of -2.6 at 2-10 GeV, and steepening further to almost -3.6
at 30-300 GeV. The features of this spectrum are interpreted in the
context of galactic propagation models, assuming that the spectrum
at the acceleration site has the form of a single power law. It is
concluded that: (1) regions outside the galactic disk contribute to the
confinement volume of electrons, (2) the containment time of electrons
is of the order 10 to the 7th years and is independent of energy,
(3) the spectrum at the acceleration site has a power law exponent
equal to -2.65, and (4) a specific mechanism is responsible for the
apparent flattening of the electron spectrum below 2 GeV.
Title: The Propagation of Cosmic-Rays in the Galaxy: Further Evidence
for a "nested Leaky Box"
Authors: Tang, J.; Muller, D.
Bibcode: 1983ICRC....2..193T
Altcode: 1983ICRC...18b.193T
No abstract at ADS
Title: On the Generation of Delta-Rays in Detectors for High Energy
Cosmic-Ray Nuclei
Authors: Swordy, S. P.; Muller, D.; Have, A. T.
Bibcode: 1983ICRC....8...55S
Altcode: 1983ICRC...18h..55S
A common problem in detectors for cosmic-ray nuclei is the generation of
energetic knock-on electrons by an incident nucleus. These electrons
may produce additional signals which can obscure the true nature
of the signal from the nucleus itself. In this paper, Monte Carlo
simulations of these effects are discussed in the University of Chicago
CRNE instrument for Spacelab-2, and show that they do not impair the
performance of the transition radiation detector as designed. Some
qualitative properties of delta-ray effects are identified, which are
of use to other experimenters in this field.
Title: Solar Flare Neutron Fluxes Derived from Interplanetary Charged
Particle Measurements
Authors: Evenson, P.; Kroeger, R.; Meyer, P.; Muller, D.
Bibcode: 1983ICRC....4...97E
Altcode: 1983ICRC...18d..97E
The first observation of interplanetary protons produced by the decay
of solar neutrons made by Evenson et al. (1983) after a solar flare
which occurred on June 3, 1982, is expanded, extending the measurement
of the spectrum of the decay protons to higher energy. The spectrum
of the decay protons for the June 21, 1980, neutron event observed by
Chupp et al. (1982) is also determined. The measurements suggest that
neutron emission from solar flares is isotropic and that different
flares emit neutrons with similar spectra. The importance of such
measurements in the study of interplanetary propagation of charged
particles is discussed.
Title: a New Transition Radiation Detector for Cosmic-Ray Nuclei
Authors: L'Heureux, J.; Meyer, P.; Muller, D.; Swordy, S.
Bibcode: 1981ICRC....8...44L
Altcode: 1981ICRC...17h..44L; 1975ICRC....8...44L
No abstract at ADS
Title: Die Kosmische Strahlung im TeV-Bereich - ein unerforschtes
Gebiet.
Authors: Müller, D.
Bibcode: 1981PhyBl..37..267M
Altcode: 1981PhB....37..267M
No abstract at ADS
Title: Further measurements of high energy cosmic ray electrons
Authors: Mueller, D.; Tang, J.
Bibcode: 1981ICRC....9..142M
Altcode: 1982ICRC....9..142M; 1981ICRC...17i.142M
The University of Chicago balloon telescope for cosmic ray electrons
has been substantially modified and improved, and has been exposed in
another successful balloon flight in 1980. Preliminary results from
this flight, over the energy range 5 to 200 GeV, are presented. Data
indicate an electron flux of 0.27 plus or minus 0.04/(sq m sec sr GeV)
at 10 GeV, and a spectral shape consistent with a power law E to the
-3.0 power at low energies, but steepening further, probably due to
radiative energy losses, with increasing energy.
Title: PDX Divertor Operation
Authors: Owens, D. K.; Arunasalam, W.; Barnes, C.; Bell, M.; Bol, K.;
Cohen, S.; Cecchi, J.; Daughney, C.; Davis, S.; Dimock, D.; Dylla,
F.; Efthimion, P.; Fonck, R.; Grek, B.; Hawryluk, R.; Hinnov, E.;
Hsuan, H.; Irie, M.; Jacobsen, R.; Johnson, D.; Johnson, L.; Maeda,
H.; Mansfield, D.; Mazzucato, E.; McGuire, K.; Meade, D.; Mueller,
D.; Okabayashi, M.; Schmidt, G.; Schmidt, J.; Silver, E.; Sinnis,
J.; Staib, P.; Strachan, J.; Suckewer, S.; Tenney, F.; Ulrickson, M.
Bibcode: 1980JNuM...93...94O
Altcode:
No abstract at ADS
Title: The Flux of Cosmic Ray Electrons at 10 GEV
Authors: Muller, D.; Prince, T.; Tang, J.
Bibcode: 1979ICRC...12..102M
Altcode: 1980ICRC...12..102M; 1979ICRC...16l.102M
Recent experiments led to conflicting results with regard to the
absolute electron intensity around 10 GeV. The data in this energy
region are usually not limited by statistical accuracy, but systematic
uncertainties must be responsible for electron fluxes that vary by at
least a factor of two between individual observations. Because of the
significant implications of the electron flux for the interpretation of
other measurements (such as measurements of the galactic synchrotron
emission, or measurements of the electron-positron ratio), the
measurement of the electron spectrum was analyzed with emphasis on the
10 GeV region. It was found that the resulting electron flux remains
relatively high, at a level of about 0.3 electron/sq m sec ster GeV
at 10 GeV.
Title: The High Energy Cosmic Ray Detector for Spacelab II
Authors: Lamport, J. E.; Lheureux, J.; Meyer, P.; Muller, D.
Bibcode: 1979ICRC...11...62L
Altcode: 1980icrc...11...62L; 1979ICRC...16k..62L
A large cosmic ray detector to be flown on Spacelab II is presently
under construction at the University of Chicago. The instrument,
with a geometric factor of 5 sq m-ster, is designed to measure the
elemental composition and the energy spectra of individual cosmic ray
nuclei (Li to Fe) from 50 GeV/nucleon to several TeV/nucleon. Plastic
scintillators are used for charge determination, and gas Cerenkov and
transition radiation detectors for energy measurements. The instrument
and its functions are described, and several test results that are
important for an optimum design are discussed.
Title: The Flux of Cosmic Ray Electrons at 10 GEV
Authors: Müller, D.; Prince, T.
Bibcode: 1979ICRC....1..471M
Altcode: 1979ICRC...16a.471M
No abstract at ADS
Title: Energy spectrum, time structure, and arrival direction
of the 1976 August 16 cosmic gamma-ray burst: an observation at
balloon altitude.
Authors: Sommer, M.; Mueller, D.
Bibcode: 1978ApJ...222L..17S
Altcode:
No abstract at ADS
Title: High-Energy Cosmic-Ray Electrons: A New Measurement Using
Transition-Radiation Detectors
Authors: Hartmann, G.; Mueller, D.; Prince, T.
Bibcode: 1977PhRvL..38.1368H
Altcode:
A new detector for cosmic-ray electrons, consisting of a combination
of a transitionradiation detector and a shower detector, has been
constructed, calibrated at accelerator beams, and exposed in a balloon
flight under 5 g/cm2 of atmosphere. The design of this
instrument and the methods of data analysis are described. Preliminary
results in the energy range 9-300 GeV are presented. The energy spectrum
of electrons is found to be significantly steeper than that of protons,
consistent with a long escape lifetime of cosmic rays in the galaxy.
Title: A New Measurement of the Cosmic Ray Electron Spectrum from
10 GeV to 300 GeV
Authors: Hartmann, G.; Mueller, D.; Prince, T.
Bibcode: 1977ICRC....1..366H
Altcode: 1977ICRC...15a.366H; 1978ICRC....1..366H
The spectrum of cosmic-ray electrons has been measured with an
instrument that combines a transition-radiation detector with a
shower detector. The transition-radiation detector provides unique
identification of individual electrons and good discrimination
against protons. At the same time, it allows the construction of a
large-area instrument (0.48 sq m ster) and consequently makes possible
a measurement of improved statistical accuracy. The instrument has
been calibrated with electron beams of 5-300 GeV at Fermilab, thus
eliminating energy-dependent biases. A first balloon flight yielded 30
hours of data at an altitude of 5 g/sq cm. The design of the instrument
is described, along with the accelerator calibrations and the analysis
of the balloon flight data. The spectrum of electrons is found to be
significantly steeper than that of protons over the whole energy range.
Title: Recent Progress in the Development of Transition Radiation
Detectors
Authors: Cherry, M.; Hartmann, G.; Müller, D.; Prince, T.
Bibcode: 1977ICRC....9...46C
Altcode: 1977ICRC...15i..46C
No abstract at ADS
Title: Simulation of Shower Development for Various Models in an
Iron Ionization Spectrometer (Abstract)
Authors: Cherry, M. L.; Hartmann, G.; Prince, T.; Mueller, D.
Bibcode: 1977ICRC....9...47C
Altcode: 1978icrc....9...47C; 1977ICRC....9...52B; 1977ICRC...15i..52B
Transition-radiation detectors have been used in several recent
cosmic-ray experiments for particle identification at energies
E/mc-squared of at least about 1000. In order to optimize the design
of such detectors and to use them for energy measurements over
a broad energy range, it is necessary to study the details of the
transition-radiation process. Experimental results are presented which
test the theoretical predictions more precisely and at higher energies
than in previous experiments. The dependence of the interference pattern
in the frequency spectrum on the radiator dimensions is studied,
and the total transition-radiation yield generated by electrons in
various radiators is measured over a very wide energy range, from 5 to
300 GeV. The significance of the individual experimental parameters
in the design of transition radiation detectors is reviewed, and the
characteristics of transition-radiation detectors capable of measuring
particle energies over the range E/mc-squared from about 300 to 100,000
are discussed.
Title: Spectrum, Time Structure and Direction of Incidence of August
16 1976 Gamma Ray Burst
Authors: Sommer, M.; Müller, D.; Horstman, H.; Bassani, L.
Bibcode: 1977ICRC....1..173S
Altcode: 1977ICRC...15a.173S
No abstract at ADS
Title: Elemental Composition of Cosmic Rays and Cosmic Ray Electrons
Authors: Mueller, D.
Bibcode: 1977ICRC...10..474M
Altcode: 1977ICRC...15j.474M; 1978ICRC...10..474M
A summary of 40 papers on the elemental composition of cosmic rays and
cosmic ray electrons is presented. Attention is given to experimental
results concerning the 'anomalous component' of low energy cosmic
radiation, the composition of ultraheavy cosmic rays, the energy
dependence of cosmic ray composition at high energies (between 1 and
100 GeV/nucleon), and the energy spectrum of high-energy electrons.
Title: Cosmic Ray Electrons: A Discussion of Recent Observations
Authors: Mueller, D.; Prince, T.
Bibcode: 1977ICRC....1..360M
Altcode: 1978ICRC....1..360M; 1977ICRC...15a.360M
A recent measurement of the spectrum of cosmic-ray electrons has
provided statistically significant evidence for a spectral shape that
is much steeper than that of protons. The electron spectrum does
not fit well to a single power law, and the abundance of electrons
relative to that of protons decreases from approximately 1% at 10 GeV
to approximately 0.1% at 300 GeV. This result is consistent with a
galactic escape lifetime for electrons exceeding 10 million years. The
data are discussed in light of current models for the propagation of
cosmic rays in the Galaxy, and conclusions are drawn concerning the
consistency of various models with the observations.
Title: Electrons in the galactic cosmic radiation.
Authors: Mueller, D.
Bibcode: 1975rgcr.conf...13M
Altcode: 1975ESRO..109...13M; 1975rgcr.rept...13M
Measurements of the charge ratio of electrons indicate that most
electrons are generated in sources within the galaxy. Radiative energy
loss processes are expected to lead to a steepening of the energy
spectrum at high energies. A compilation of the existing measurements
of the flux and energy spectrum of electrons up to almost 1000 GeV is
shown. No unambiguous conclusion as to the existence of the spectral
steepening can be drawn on the basis of these data. The experimental
difficulties and prospects for future investigations are briefly
discussed.
Title: Transition-radiation detectors for cosmic-ray research
Authors: Mueller, D.
Bibcode: 1975rgcr.conf..133M
Altcode: 1975rgcr.rept..133M; 1975ESRO..109..133M
The transition-radiation detectors consist of plastic foam of multiple
plastic foil radiators, followed by proportional chambers. Properties
of such detectors are given, and the detection and discrimination
efficiencies for energetic particles are discussed. Several possible
applications of such devices for studies of cosmic ray particles in
the high energy region are suggested.
Title: Design of a Transition Radiation Detector for Cosmic Rays
Authors: Hartmann, G.; Mueller, D.; Prince, T.
Bibcode: 1975ICRC....9.3272H
Altcode: 1975ICRC...14.3272H; 1975icrc....9.3272H
Transition radiation detectors consisting of sandwiches of plastic
foam radiators and multiwire proportional chambers can be used to
identify cosmic ray particles with energies gamma E/mc-squared is
greater than 10 to the 3rd and to measure their energy in the region
gamma is roughly equal to 10 to the 3rd
Title: Transition radiation from relativistic electrons in periodic
radiators
Authors: Cherry, M. L.; Mueller, D.; Prince, T. A.; Hartmann, G.
Bibcode: 1974PhRvD..10.3594C
Altcode:
The generation and detection of transition radiation have been studied
in a series of experiments with electrons from 1 to 15 GeV at SLAC
and at the Cornell Synchrotron. Periodic radiators, consisting of
thin plastic foils stretched in air at constant spacings, were used,
and proportional chambers filled with krypton or xenon served as
detectors. A detailed discussion of the theoretical predictions
is given, and the measurements are systematically compared with
the predictions by varying the most critical parameters, such
as configuration of radiators and detectors, and energy of the
electrons. In general, good agreement between theory and experiment has
been found. On the basis of these results, the criteria are summarized
under which transition radiation can readily be observed.
Title: Measurements of the Spectrum of Galactic Electrons at Very
High Energies
Authors: Müller, D.
Bibcode: 1973ICRC....1..361M
Altcode: 1973ICRC...13..361M
No abstract at ADS
Title: Absolute and relative line intensity measurements when the
spectral lines are not optically thin.
Authors: Vujnovic, V.; Pichler, G.; Tonejc, A. M.; Acinger, K.;
Müller, D.
Bibcode: 1973JQSRT..13.1465V
Altcode:
No abstract at ADS
Title: Cosmic Rays at Very High Enregies: Discussion of Some New
Results
Authors: Juliusson, E.; Meyer, P.; Müller, D.
Bibcode: 1973ICRC....1..373J
Altcode: 1973ICRC...13..373J
No abstract at ADS
Title: Observation of Argon Lines at Normal Pressure in the Vacuum
Ultraviolet
Authors: Müller, D.; Vadla, Ć.; Vujnović, V.
Bibcode: 1972SSRv...13..563M
Altcode: 1972IAUCo..14..563M
No abstract at ADS
Title: Flux and Energy Spectrum of Cosmic Ray Electrons between 10
and 1000 GeV.
Authors: Meyer, P.; Muller, D.
Bibcode: 1971ICRC....1..117M
Altcode: 1971ICRC...12..117M
No abstract at ADS