Author name code: bocchialini ADS astronomy entries on 2022-09-14 author:"Bocchialini, Karine" ------------------------------------------------------------------------ Title: The role of asymmetries in coronal rain formation during thermal non-equilibrium cycles Authors: Pelouze, Gabriel; Auchère, Frédéric; Bocchialini, Karine; Froment, Clara; Mikić, Zoran; Soubrié, Elie; Voyeux, Alfred Bibcode: 2022A&A...658A..71P Altcode: 2021arXiv211009975P Context. Thermal non-equilibrium (TNE) produces several observables that can be used to constrain the spatial and temporal distribution of solar coronal heating. Its manifestations include prominence formation, coronal rain, and long-period intensity pulsations in coronal loops. The recent observation of abundant periodic coronal rain associated with intensity pulsations allowed for these two phenomena to be unified as the result of TNE condensation and evaporation cycles. On the other hand, many observed intensity pulsation events show little to no coronal rain formation.
Aims: Our goal is to understand why some TNE cycles produce such abundant coronal rain, while others produce little to no rain.
Methods: We reconstructed the geometry of the periodic coronal rain event, using images from the Extreme Ultraviolet Imager (EUVI) onboard the Solar Terrestrial Relations Observatory (STEREO), and magnetograms from the Helioseismic and Magnetic Imager (HMI). We then performed 1D hydrodynamic simulations of this event for different heating parameters and variations of the loop geometry (9000 simulations in total). We compared the resulting behaviour to simulations of TNE cycles that do not produce coronal rain.
Results: Our simulations show that both prominences and TNE cycles (with and without coronal rain) can form within the same magnetic structure. We show that the formation of coronal rain during TNE cycles depends on the asymmetry of the loop and of the heating. Asymmetric loops are overall less likely to produce coronal rain, regardless of the heating. In symmetric loops, coronal rain forms when the heating is also symmetric. In asymmetric loops, rain forms only when the heating compensates for the asymmetry.

Movie associated to Fig. 5 is available at https://www.aanda.org Title: Empirical relations between the intensities of Lyman lines of H and He+ Authors: Gordino, M.; Auchère, F.; Vial, J. -C.; Bocchialini, K.; Hassler, D. M.; Bando, T.; Ishikawa, R.; Kano, R.; Kobayashi, K.; Narukage, N.; Trujillo Bueno, J.; Winebarger, A. Bibcode: 2022A&A...657A..86G Altcode: 2022arXiv220101519G Context. Empirical relations between major UV and extreme UV spectral lines are one of the inputs for models of chromospheric and coronal spectral radiances and irradiances. They are also needed for the interpretation of some of the observations of the Solar Orbiter mission.
Aims: We aim to determine an empirical relation between the intensities of the H I 121.6 nm and He II 30.4 nm Ly-α lines.
Methods: Images at 121.6 nm from the Chromospheric Lyman-Alpha Spectro Polarimeter (CLASP) and Multiple XUV Imager (MXUVI) sounding rockets were co-registered with simultaneous images at 30.4 nm from the EIT and AIA orbital telescopes in order to derive a spatially resolved relationship between the intensities.
Results: We have obtained a relationship between the H I 121.6 nm and He II 30.4 nm intensities that is valid for a wide range of solar features, intensities, and activity levels. Additional SUMER data have allowed the derivation of another relation between the H I 102.5 nm (Ly-β) and He II 30.4 nm lines for quiet-Sun regions. We combined these two relationships to obtain a Ly-α/Ly-β intensity ratio that is comparable to the few previously published results.
Conclusions: The relationship between the H I 121.6 nm and He II 30.4 nm lines is consistent with the one previously obtained using irradiance data. We have also observed that this relation is stable in time but that its accuracy depends on the spatial resolution of the observations. The derived Ly-α/Ly-β intensity ratio is also compatible with previous results. 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 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: Role of the Coronal Environment in the Formation of Four Shocks Observed without Coronal Mass Ejections at Earth's Lagrangian Point L1 Authors: Pick, M.; Magdalenić, J.; Cornilleau-Wehrlin, N.; Grison, B.; Schmieder, B.; Bocchialini, K. Bibcode: 2020ApJ...895..144P Altcode: The main goal of this study is to determine the solar origin of four single shocks observed at the Lagrange point L1 and followed by storm sudden commencements (SSCs) during 2002. We look for associated coronal mass ejections (CMEs), starting from estimates of the transit time from Sun to Earth. For each CME, we investigate its association with a radio type II burst, an indicator of the presence of a shock wave. For three of the events, the type II burst is shown to propagate along the same, or a similar, direction as the fastest segment of the CME leading edge. We analyze for each event the role of the coronal environment in the CME development, the shock formation, and their propagation, to finally identify its complex evolution. The ballistic velocity of these shocks during their propagation from the corona to L1 is compared to the shock velocity at L1. Based on a detailed analysis of the shock propagation and possible interactions up to 30 solar radii, we find a coherent velocity evolution for each event, in particular for one event, the 2002 April 14 SSC, for which a previous study did not find a satisfactory CME source. For the other three events, we observe the formation of a white-light shock overlying the different sources associated with those events. The localization of the event sources over the poles, together with an origin of the shocks being due to encounters of CMEs, can explain why at L1 we observe only single shocks and not interplanetary CMEs. Title: Low Geo-Effectiveness of Fast Halo CMEs Related to the 12 X-Class Flares in 2002 Authors: Schmieder, B.; Kim, R. -S.; Grison, B.; Bocchialini, K.; Kwon, R. -Y.; Poedts, S.; Démoulin, P. Bibcode: 2020JGRA..12527529S Altcode: 2020arXiv200310777S It is generally accepted that extreme space weather events tend to be related to strong flares and fast halo coronal mass ejections (CMEs). In the present paper, we carefully identify the chain of events from the Sun to the Earth induced by all 12 X-class flares that occurred in 2002. In this small sample, we find an unusual high rate (58%) of solar sources with a longitude larger than 74°. Yet all 12 X-class flares are associated with at least one CME. The fast halo CMEs (50%) are related to interplanetary CMEs (ICMEs) at L1 and weak Dst minimum values (more than -51 nT), while five (41%) of the 12 X-class flares are related to solar proton events (SPEs). We conclude that (i) all 12 analyzed solar events, even those associated with fast halo CMEs originating from the central disk region, and those ICMEs and SPEs were not very geo-effective. This unexpected result demonstrates that the suggested events in the chain (fast halo CME, X-class flares, central disk region, ICME, and SPE) are not infallible proxies for geo-effectiveness. (ii) The low value of integrated and normalized southward component of the interplanetary magnetic field (Bz*) may explain the low geo-effectiveness for this small sample. In fact, Bz* is well correlated to the weak Dst and low auroral electrojet activity. Hence, the only space weather impact at Earth in 2002 we can explain is based on Bz* at L1. Title: Spectroscopic detection of coronal plasma flows in loops undergoing thermal non-equilibrium cycles Authors: Pelouze, Gabriel; Auchère, Frédéric; Bocchialini, Karine; Froment, Clara; Parenti, Susanna; Soubrié, Elie Bibcode: 2020A&A...634A..54P Altcode: 2019arXiv191202538P Context. Long-period intensity pulsations were recently detected in the EUV emission of coronal loops and attributed to cycles of plasma evaporation and condensation driven by thermal non-equilibrium (TNE). Numerical simulations that reproduce this phenomenon also predict the formation of periodic flows of plasma at coronal temperatures along some of the pulsating loops.
Aims: We aim to detect these predicted flows of coronal-temperature plasma in pulsating loops.
Methods: We used time series of spatially resolved spectra from the EUV imaging spectrometer (EIS) onboard Hinode and tracked the evolution of the Doppler velocity in loops in which intensity pulsations have previously been detected in images of SDO/AIA.
Results: We measured signatures of flows that are compatible with the simulations but only for a fraction of the observed events. We demonstrate that this low detection rate can be explained by line of sight ambiguities combined with instrumental limitations, such as low signal-to-noise ratio or insufficient cadence.

Movies associated to Figs. 1, 4, 7, 10 are available at https://www.aanda.org Title: Comprehensive Determination of the Hinode/EIS Roll Angle Authors: Pelouze, Gabriel; Auchère, Frédéric; Bocchialini, Karine; Harra, Louise; Baker, Deborah; Warren, Harry P.; Brooks, David H.; Mariska, John T. Bibcode: 2019SoPh..294...59P Altcode: 2019arXiv190311923P We present a new coalignment method for the EUV Imaging Spectrometer (EIS) on board the Hinode spacecraft. In addition to the pointing offset and spacecraft jitter, this method determines the roll angle of the instrument, which has never been systematically measured, and which is therefore usually not corrected. The optimal pointing for EIS is computed by maximizing the cross-correlations of the Fe XII 195.119 Å line with images from the 193 Å band of the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). By coaligning 3336 rasters with high signal-to-noise ratio, we estimate the rotation angle between EIS and AIA and explore the distribution of its values. We report an average value of (−0.387±0.007 ) ∘. We also provide a software implementation of this method that can be used to coalign any EIS raster. Title: Geoeffectiveness of the 12 X-class flares in 2002 Authors: Schmieder, Brigitte; Kim, Rocksoon; Grison, Benjamin; Bocchialini, Karine; Kwon, Young Bibcode: 2019EGUGA..21.1876S Altcode: We analyze systematically the chain of events related to the 12 X-ray flares of X class occurring in 2002: source region, CME, ICME, magnetic field at L1, geomagnetic indices, and SEP to determine if we could explain their weak geo-effectiveness by usual criteria. No intense geomagnetic storm is related to any of these flares. Only one of them is associated with a moderate storm. The three others are associated with a weak storm (-50 nT < min(Dst) < -30 nT). 75 % of the flares are associated with a halo CME with a good correlation rate for the speed/flux of the flare. The flare sources are mainly close to the limb (70%). We conclude that the association of big flares and strong geomagnetic disturbances may be valid only for extreme or intense geomagnetic storms. Otherwise the magnetic energy of active regions is released in an unexpected way into thermal energy and kinetic energy or in ejections of energetic particles. The most important parameter is the Bz value and its orientation. It seems that the CMEs launched with high speed (around 2000 km/s) avoid the Earth in our sample. The location of the solar source, the shape of the CME, and the shock front have a direct impact on the geo-effectiveness. Title: Solar data, dataproducts, and tools at MEDOC Authors: Buchlin, Eric; Caminade, Stéphane; Dufourg, Nicolas; Auchère, Frédéric; Baudin, Frédéric; Bocchialini, Karine; Boumier, Patrick; Janvier, Miho; Parenti, Susanna; Alingery, Pablo; Ballans, Hervé; Chane-Yook, Martine; Dexet, Marc; Mercier, Claude; Poulleau, Gilles Bibcode: 2019EGUGA..2117362B Altcode: MEDOC (Multi-Experiment Data and Operation Centre), initially created as a European data and operation centre for the SOHO mission, has grown with data from other solar physics space missions, from STEREO to SDO. Derived data products such as DEM maps from SDO/AIA, synoptic EUV intensity maps from SOHO/EIT, and catalogues of solar structures are also automatically produced and redistributed. Both the data and the derived data products are publicly available from web interfaces and from programmatic interfaces (with clients for IDL and Python), allowing classical data analysis as well as automatic queries, data download, and processing to be made on large datasets. Title: Erratum: Correction to: Statistical Analysis of Solar Events Associated with Storm Sudden Commencements over One Year of Solar Maximum During Cycle 23: Propagation from the Sun to the Earth and Effects Authors: Bocchialini, K.; Grison, B.; Menvielle, M.; Chambodut, A.; Cornilleau-Wehrlin, N.; Fontaine, D.; Marchaudon, A.; Pick, M.; Pitout, F.; Schmieder, B.; Régnier, S.; Zouganelis, I. Bibcode: 2019SoPh..294...38B Altcode: Correction to: Solar Phys (2018) 293:75https://doi.org/10.1007/s11207-018-1278-5

Please find in this correction document the correct versions of abstract, Sect. 3.1 and Figs. 3 and 12. Title: The SDO AIA and HMI archive at MEDOC Authors: Alingery, Pablo; Buchlin, Éric; Caminade, Stéphane; Ballans, Hervé; Baudin, Frédéric; Parenti, Susanna; Bocchialini, Karine Bibcode: 2018csc..confE.113A Altcode: MEDOC, created as the European data and operations center for SoHO, hosts also data from STEREO, SDO, and various other solar physics missions. The SDO archive at MEDOC represents more than 415TB of data, and covers the full length of the mission. It includes aia.lev1 data at a minimum cadence of 60s in the EUV channels (12s at specific periods of interest), and most of the 720s-cadence HMI series. It is complemented by a database of DEM maps derived from AIA. MEDOC provides a reliable, convenient, and fast (especially for European users) access to these SDO data, by a web interface and webservices. We also provide IDL and Python clients to these webservices, allowing complex queries and automated analyses on large datasets to be made. Title: Search for predicted periodic flows in loops undergoing thermal non-equilibrium Authors: Pelouze, Gabriel; Parenti, Susanna; Bocchialini, Karine; Soubrie, Elie; Auchere, Frederic; Froment, Clara Bibcode: 2018cosp...42E2623P Altcode: Long-period intensity pulsations have been recently detected in coronal loopswith EUV images of both SoHO/EIT (Auchère et al., 2014) and SDO/AIA (Froment etal., 2015). These pulsations have been interpreted as resulting from thermalnon-equilibrium (TNE), thus providing a signature of a highly-stratified andquasi-constant heating at the loops footpoints (Froment et al., 2017; Auchèreet al., 2016). Depending on the adequacy between the geometry of the loop andthe characteristics of the heating, this can result in either complete (atchromospheric temperatures) or incomplete (> 1 MK) condensation and evaporationcycles, that are responsible for the observed intensity pulsations. Using 1Dhydrodynamic simulations, Froment et al. (2017) were able to reproduce theobserved pulsations, with incomplete condensation for the active region studiedin their previous paper. The simulations also predict periodic plasma flowsalong the loops footpoints, with velocities up to 40 km/s. We try to detect these flows by using time series of spatially resolved spectrafrom the EUV spectrometer Hinode/EIS. We systematically search for EIS datasetsthat correspond to the observation of pulsation events among the 3000+ thatwere detected in AIA data, between 2010 and 2016. For the 9 datasets that arefound, we derive series of Doppler velocity maps, which allows us to track theevolution of the plasma velocity in the loop over several pulsation periods. Wethen compare these data to the results of previous simulations andobservations. However the expected pulsations in velocity cannot be identifiedin any of the datasets that we analysed. We demonstrate that line of sightambiguities, combined with low signal to noise ratio or lack of time cadence,can explain this non-detection. Title: Statistical Analysis of Solar Events Associated with Storm Sudden Commencements over One Year of Solar Maximum During Cycle 23: Propagation from the Sun to the Earth and Effects Authors: Bocchialini, K.; Grison, B.; Menvielle, M.; Chambodut, A.; Cornilleau-Wehrlin, N.; Fontaine, D.; Marchaudon, A.; Pick, M.; Pitout, F.; Schmieder, B.; Régnier, S.; Zouganelis, I. Bibcode: 2018SoPh..293...75B Altcode: 2018arXiv180307593B Taking the 32 storm sudden commencements (SSCs) listed by the International Service of Geomagnetic Indices (ISGI) of the Observatory de l'Ebre during 2002 (solar activity maximum in Cycle 23) as a starting point, we performed a multi-criterion analysis based on observations (propagation time, velocity comparisons, sense of the magnetic field rotation, radio waves) to associate them with solar sources, identified their effects in the interplanetary medium, and looked at the response of the terrestrial ionized and neutral environment. We find that 28 SSCs can be related to 44 coronal mass ejections (CMEs), 15 with a unique CME and 13 with a series of multiple CMEs, among which 19 (68%) involved halo CMEs. Twelve of the 19 fastest CMEs with speeds greater than 1000 km s−1 are halo CMEs. For the 44 CMEs, including 21 halo CMEs, the corresponding X-ray flare classes are: 3 X-class, 19 M-class, and 22 C-class flares. The probability for an SSC to occur is 75% if the CME is a halo CME. Among the 500, or even more, front-side, non-halo CMEs recorded in 2002, only 23 could be the source of an SSC, i.e. 5%. The complex interactions between two (or more) CMEs and the modification of their trajectories have been examined using joint white-light and multiple-wavelength radio observations. The detection of long-lasting type IV bursts observed at metric-hectometric wavelengths is a very useful criterion for the CME-SSC events association. The events associated with the most depressed Dst values are also associated with type IV radio bursts. The four SSCs associated with a single shock at L1 correspond to four radio events exhibiting characteristics different from type IV radio bursts. The solar-wind structures at L1 after the 32 SSCs are 12 magnetic clouds (MCs), 6 interplanetary coronal mass ejections (ICMEs) without an MC structure, 4 miscellaneous structures, which cannot unambiguously be classified as ICMEs, 5 corotating or stream interaction regions (CIRs/SIRs), one CIR caused two SSCs, and 4 shock events; note than one CIR caused two SSCs. The 11 MCs listed in 3 or more MC catalogs covering the year 2002 are associated with SSCs. For the three most intense geomagnetic storms (based on Dst minima) related to MCs, we note two sudden increases of the Dst, at the arrival of the sheath and the arrival of the MC itself. In terms of geoeffectiveness, the relation between the CME speed and the magnetic-storm intensity, as characterized using the Dst magnetic index, is very complex, but generally CMEs with velocities at the Sun larger than 1000 km s−1 have larger probabilities to trigger moderate or intense storms. The most geoeffective events are MCs, since 92% of them trigger moderate or intense storms, followed by ICMEs (33%). At best, CIRs/SIRs only cause weak storms. We show that these geoeffective events (ICMEs or MCs) trigger an increased and combined auroral kilometric radiation (AKR) and non-thermal continuum (NTC) wave activity in the magnetosphere, an enhanced convection in the ionosphere, and a stronger response in the thermosphere. However, this trend does not appear clearly in the coupling functions, which exhibit relatively weak correlations between the solar-wind energy input and the amplitude of various geomagnetic indices, whereas the role of the southward component of the solar-wind magnetic field is confirmed. Some saturation appears for Dst values <−100 nT on the integrated values of the polar and auroral indices. Title: On the Occurrence of Thermal Nonequilibrium in Coronal Loops Authors: Froment, C.; Auchère, F.; Mikić, Z.; Aulanier, G.; Bocchialini, K.; Buchlin, E.; Solomon, J.; Soubrié, E. Bibcode: 2018ApJ...855...52F Altcode: 2018arXiv180204010F Long-period EUV pulsations, recently discovered to be common in active regions, are understood to be the coronal manifestation of thermal nonequilibrium (TNE). The active regions previously studied with EIT/Solar and Heliospheric Observatory and AIA/SDO indicated that long-period intensity pulsations are localized in only one or two loop bundles. The basic idea of this study is to understand why. For this purpose, we tested the response of different loop systems, using different magnetic configurations, to different stratifications and strengths of the heating. We present an extensive parameter-space study using 1D hydrodynamic simulations (1020 in total) and conclude that the occurrence of TNE requires specific combinations of parameters. Our study shows that the TNE cycles are confined to specific ranges in parameter space. This naturally explains why only some loops undergo constant periodic pulsations over several days: since the loop geometry and the heating properties generally vary from one loop to another in an active region, only the ones in which these parameters are compatible exhibit TNE cycles. Furthermore, these parameters (heating and geometry) are likely to vary significantly over the duration of a cycle, which potentially limits the possibilities of periodic behavior. This study also confirms that long-period intensity pulsations and coronal rain are two aspects of the same phenomenon: both phenomena can occur for similar heating conditions and can appear simultaneously in the simulations. Title: Statistical analysis of solar events associated with SSC over year of solar maximum during cycle 23: 2. Characterisation on the Sun-Earth path - Geoeffectiveness Authors: Cornilleau-Wehrlin, N.; Bocchialini, K.; Menvielle, M.; Fontaine, D.; Grison, B.; Marchaudon, A.; Pick, M.; Pitout, F.; Schmieder, B.; Regnier, S.; Zouganelis, Y.; Chambodut, A. Bibcode: 2017AGUFMSH31A2712C Altcode: Taking the 32 sudden storm commencements (SSC) listed by the observatory de l'Ebre / ISGI over the year 2002 (maximal solar activity) as a starting point, we performed a statistical analysis of the related solar sources, solar wind signatures, and terrestrial responses. For each event, we characterized and identified, as far as possible, (i) the sources on the Sun (Coronal Mass Ejections -CME-), with the help of a series of criteria (velocities, drag coefficient, radio waves, magnetic field polarity), as well as (ii) the structure and properties in the interplanetary medium, at L1, of the event associated to the SSC: magnetic clouds -MC-, non-MC interplanetary coronal mass ejections -ICME-, co-rotating/stream interaction regions -SIR/CIR-, shocks only and unclear events that we call "miscellaneous" events. The geoeffectiveness of the events, classified by category at L1, is analysed by their signatures in the Earth ionized (magnetosphere and ionosphere) and neutral (thermosphere) environments, using a broad set of in situ, remote and ground based instrumentation. The role of the presence of a unique or of a multiple source at the Sun, of its nature, halo or non halo CME, is also discussed. The set of observations is statistically analyzed so as to evaluate and compare the geoeffectiveness of the events. The results obtained for this set of geomagnetic storms started by SSCs is compared to the overall statistics of year 2002, relying on already published catalogues of events, allowing assessing the relevance of our approach ; for instance all the 12 well identified Magnetic Clouds of 2002 give rise to SSCs. Title: Statistical Analysis of Solar Events Associated with Storm Sudden Commencements over One Year of Solar Maximum during Cycle 23: Propagation and Effects from the Sun to the Earth. Authors: Bocchialini, K.; Grison, B.; Menvielle, M.; Chambodut, A.; Cornilleau-Wehrlin, N.; Fontaine, D.; Marchaudon, A.; Pick, M.; Pitout, F.; Schmieder, B.; Régnier, S.; Zouganelis, I. Bibcode: 2017sf2a.conf..181B Altcode: From the list of 32 SSCs over the year 2002, we performed a multi-criteria analysis based on propagation time, velocity comparison, sense of the magnetic field rotation, radio waves to associate them with solar sources, identify their causes in the interplanetary medium and then look at the response of the terrestrial ionized and neutral environment to them. The complex interactions between two (or more) CMEs and the modification in their trajectory have been examined using joint white light and multiple-wavelength radio observations. The structures at L_1 after the 32 SSCs are regarded as Magnetic Clouds (MCs), ICMEs without a MC structure, Miscellaneous structures, CIRs/SIRs, and shock-only events. In terms of geoeffectivity, generally CMEs with velocities at the Sun larger than 1000 km.s-1 have larger probabilities to trigger moderate or intense storms. The most geoeffective events are MCs, since 92% of them trigger moderate or intense storms. The geoeffective events trigger an increased and combined AKR and NTC wave activity in the magnetosphere, an enhanced convection in the ionosphere and a stronger response in the thermosphere. Title: Statistical Analysis of Solar Events Associated with SSC over Year of Solar Maximum during Cycle 23: 1. Identification of Related Sun-Earth Events Authors: Grison, B.; Bocchialini, K.; Menvielle, M.; Chambodut, A.; Cornilleau-Wehrlin, N.; Fontaine, D.; Marchaudon, A.; Pick, M.; Pitout, F.; Schmieder, B.; Regnier, S.; Zouganelis, Y. Bibcode: 2017AGUFMSH31A2711G Altcode: Taking the 32 sudden storm commencements (SSC) listed by the observatory de l'Ebre / ISGI over the year 2002 (maximal solar activity) as a starting point, we performed a statistical analysis of the related solar sources, solar wind signatures, and terrestrial responses. For each event, we characterized and identified, as far as possible, (i) the sources on the Sun (Coronal Mass Ejections -CME-), with the help of a series of herafter detailed criteria (velocities, drag coefficient, radio waves, polarity), as well as (ii) the structure and properties in the interplanetary medium, at L1, of the event associated to the SSC: magnetic clouds -MC-, non-MC interplanetary coronal mass ejections -ICME-, co-rotating/stream interaction regions -SIR/CIR-, shocks only and unclear events that we call "miscellaneous" events. The categorization of the events at L1 is made on published catalogues. For each potential CME/L1 event association we compare the velocity observed at L1 with the one observed at the Sun and the estimated balistic velocity. Observations of radio emissions (Type II, Type IV detected from the ground and /or by WIND) associated to the CMEs make the solar source more probable. We also compare the polarity of the magnetic clouds with the hemisphere of the solar source. The drag coefficient (estimated with the drag-based model) is calculated for each potential association and it is compared to the expected range values. We identified a solar source for 26 SSC related events. 12 of these 26 associations match all criteria. We finally discuss the difficulty to perform such associations. Title: Erratum: “On the Fourier and Wavelet Analysis of Coronal Time Series” (2016, ApJ, 825, 110) Authors: Auchère, F.; Froment, C.; Bocchialini, K.; Buchlin, E.; Solomon, J. Bibcode: 2017ApJ...838..166A Altcode: No abstract at ADS Title: Statistical analysis of solar events associated with SSC over one year of solar maximum during cycle 23: propagation and effects from the Sun to the Earth Authors: Cornilleau-Wehrlin, Nicole; Bocchialini, Karine; Menvielle, Michel; Chambodut, Aude; Fontaine, Dominique; Grison, Benjamin; Marchaudon, Aurélie; Pick, Monique; Pitout, Frédéric; Schmieder, Brigitte; Régnier, Stéphane; Zouganelis, Yannis Bibcode: 2017EGUGA..19.3689C Altcode: Taking the 32 sudden storm commencements (SSC) listed by the observatory de l'Ebre / ISGI over the year 2002 (maximal solar activity) as a starting point, we performed a statistical analysis of the related solar sources, solar wind signatures, and terrestrial responses. For each event, we characterized and identified, as far as possible, (i) the sources on the Sun (Coronal Mass Ejections -CME-), with the help of a series of criteria (velocities, drag coefficient, radio waves, helicity), as well as (ii) the structure and properties in the interplanetary medium, at L1, of the event associated to the SSC: magnetic clouds -MC-, non-MC interplanetary coronal mass ejections -ICME-, co-rotating/stream interaction regions -SIR/CIR-, shocks only and unclear events that we call "miscellaneous" events. The observed Sun-to-Earth travel times are compared to those estimated using existing simple models of propagation in the interplanetary medium. This comparison is used to statistically assess performances of various models. The geoeffectiveness of the events, classified by category at L1, is analysed by their signatures in the Earth ionized (magnetosphere and ionosphere) and neutral (thermosphere) environments, using a broad set of in situ, remote and ground based instrumentation. The role of the presence of a unique or of a multiple source at the Sun, of its nature, halo or non halo CME, is also discussed. The set of observations is statistically analyzed so as to evaluate and compare the geoeffectiveness of the events. The results obtained for this set of geomagnetic storms started by SSCs is compared to the overall statistics of year 2002, relying on already published catalogues of events, allowing assessing the relevance of our approach (for instance the all 12 well identified Magnetic Clouds of 2002 give rise to SSCs). Title: Long-period Intensity Pulsations in Coronal Loops Explained by Thermal Non-equilibrium Cycles Authors: Froment, C.; Auchère, F.; Aulanier, G.; Mikić, Z.; Bocchialini, K.; Buchlin, E.; Solomon, J. Bibcode: 2017ApJ...835..272F Altcode: 2017arXiv170101309F In solar coronal loops, thermal non-equilibrium (TNE) is a phenomenon that can occur when the heating is both highly stratified and quasi-constant. Unambiguous observational identification of TNE would thus permit us to strongly constrain heating scenarios. While TNE is currently the standard interpretation of coronal rain, the long-term periodic evolution predicted by simulations has never been observed. However, the detection of long-period intensity pulsations (periods of several hours) has been recently reported with the Solar and Heliospheric Observatory/EIT, and this phenomenon appears to be very common in loops. Moreover, the three intensity-pulsation events that we recently studied with the Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA) show strong evidence for TNE in warm loops. In this paper, a realistic loop geometry from linear force-free field (LFFF) extrapolations is used as input to 1D hydrodynamic simulations. Our simulations show that, for the present loop geometry, the heating has to be asymmetrical to produce TNE. We analyze in detail one particular simulation that reproduces the average thermal behavior of one of the pulsating loop bundle observed with AIA. We compare the properties of this simulation with those deduced from the observations. The magnetic topology of the LFFF extrapolations points to the presence of sites of preferred reconnection at one footpoint, supporting the presence of asymmetric heating. In addition, we can reproduce the temporal large-scale intensity properties of the pulsating loops. This simulation further strengthens the interpretation of the observed pulsations as signatures of TNE. This consequently provides important information on the heating localization and timescale for these loops. Title: Thermal Non-Equilibrium Revealed by Periodic Pulses of Random Amplitudes in Solar Coronal Loops Authors: Auchère, F.; Froment, C.; Bocchialini, K.; Buchlin, E.; Solomon, J. Bibcode: 2016usc..confE.131A Altcode: We recently detected variations in extreme ultraviolet intensity in coronal loops repeating with periods of several hours. Models of loops including stratified and quasi-steady heating predict the development of a state of thermal non-equilibrium (TNE): cycles of evaporative upflows at the footpoints followed by falling condensations at the apex. Based on Fourier and wavelet analysis, we demonstrate that the observed periodic signals are indeed not signatures of vibrational modes. Instead, superimposed on the power law expected from the stochastic background emission, the power spectra of the time series exhibit the discrete harmonics and continua expected from periodic trains of pulses of random amplitudes. These characteristics reinforce our earlier interpretation of these pulsations as being aborted TNE cycles. Title: Fourier and Wavelet Analysis of Coronal Time Series Authors: Auchère, F.; Froment, C.; Bocchialini, K.; Buchlin, E.; Solomon, J. Bibcode: 2016usc..confE.130A Altcode: Using Fourier and wavelet analysis, we critically re-assess the significance of our detection of periodic pulsations in coronal loops. We show that the proper identification of the frequency dependence and statistical properties of the different components of the power spectra provies a strong argument against the common practice of data detrending, which tends to produce spurious detections around the cut-off frequency of the filter. In addition, the white and red noise models built into the widely used wavelet code of Torrence & Compo cannot, in most cases, adequately represent the power spectra of coronal time series, thus also possibly causing false positives. Both effects suggest that several reports of periodic phenomena should be re-examined. The Torrence & Compo code nonetheless effectively computes rigorous confidence levels if provided with pertinent models of mean power spectra, and we describe the appropriate manner in which to call its core routines. We recall the meaning of the default confidence levels output from the code, and we propose new Monte-Carlo-derived levels that take into account the total number of degrees of freedom in the wavelet spectra. These improvements allow us to confirm that the power peaks that we detected have a very low probability of being caused by noise. Title: Long-period Intensity Pulsations as the Manifestation of the Heating Stratification and Timescale in Coronal Loops Authors: Froment, Clara; Auchère, Frédéric; Aulanier, Guillaume; Mikić, Zoran; Bocchialini, Karine; Buchlin, Eric; Solomon, Jacques Bibcode: 2016usc..confE..47F Altcode: In solar coronal loops, thermal non-equilibrium (TNE) is a phenomenon that can occur when the heating is both highly-stratified and quasi-constant. Unambiguous observational identification of TNE would thus permit to strongly constrain heating scenarios. Up to now, while TNE is the standard interpretation of coronal rain, it was not believed to happen commonly in warm coronal loops. Recently, the detection of long-period intensity pulsations (periods of several hours) has been reported with SoHO/EIT. This phenomenon appears to be very common in loops (Auchère et al. 2014). In Froment et al. 2015, three intensity-pulsation events studied with SDO/AIA, show strong evidence for TNE in warm loops. We use realistic loop geometries from LFFF extrapolations for one of these events are used as input to a 1D hydrodynamic simulation of TNE. A highly-stratified heating function is chosen to reproduce the observed period of pulsation and temperature of the loops. With these conditions, the heating function has to be asymmetric. The magnetic topology of the LFFF extrapolations points to the presence of sites of preferred reconnection at one footpoint, supporting the presence of asymmetric heating. We compared the properties of the simulated loop with the properties deduced from observations. We found that the 1D hydrodynamic simulation can reproduce the large temporal scale intensity properties of the pulsating loops (Froment et al. 2016, submitted). This simulation further strengthen the interpretation of the observed pulsations as signatures of TNE. This implies that the heating for these loops is highly-stratified and that the frequency of the heating events must be high compared to the typical cooling time. Title: Thermal Non-equilibrium Revealed by Periodic Pulses of Random Amplitudes in Solar Coronal Loops Authors: Auchère, F.; Froment, C.; Bocchialini, K.; Buchlin, E.; Solomon, J. Bibcode: 2016ApJ...827..152A Altcode: 2016arXiv160803789A We recently detected variations in extreme ultraviolet intensity in coronal loops repeating with periods of several hours. Models of loops including stratified and quasi-steady heating predict the development of a state of thermal non-equilibrium (TNE): cycles of evaporative upflows at the footpoints followed by falling condensations at the apex. Based on Fourier and wavelet analysis, we demonstrate that the observed periodic signals are indeed not signatures of vibrational modes. Instead, superimposed on the power law expected from the stochastic background emission, the power spectra of the time series exhibit the discrete harmonics and continua expected from periodic trains of pulses of random amplitudes. These characteristics reinforce our earlier interpretation of these pulsations as being aborted TNE cycles. Title: Solar abundances with the SPICE spectral imager on Solar Orbiter Authors: Giunta, Alessandra; Haberreiter, Margit; Peter, Hardi; Vial, Jean-Claude; Harrison, Richard; Parenti, Susanna; Innes, Davina; Schmutz, Werner; Buchlin, Eric; Chamberlin, Phillip; Thompson, William; Bocchialini, Karine; Gabriel, Alan; Morris, Nigel; Caldwell, Martin; Auchere, Frederic; Curdt, Werner; Teriaca, Luca; Hassler, Donald M.; DeForest, Craig; Hansteen, Viggo; Carlsson, Mats; Philippon, Anne; Janvier, Miho; Wimmer-Schweingruber, Robert; Griffin, Douglas; Baudin, Frederic; Davila, Joseph; Fludra, Andrzej; Waltham, Nick; Eccleston, Paul; Gottwald, Alexander; Klein, Roman; Hanley, John; Walls, Buddy; Howe, Chris; Schuehle, Udo; Gyo, Manfred; Pfiffner, Dany Bibcode: 2016cosp...41E.681G Altcode: Elemental composition of the solar atmosphere and in particular abundance bias of low and high First Ionization Potential (FIP) elements are a key tracer of the source regions of the solar wind. These abundances and their spatio-temporal variations, as well as the other plasma parameters , will be derived by the SPICE (Spectral Imaging of the Coronal Environment) EUV spectral imager on the upcoming Solar Orbiter mission. SPICE is designed to provide spectroheliograms (spectral images) using a core set of emission lines arising from ions of both low-FIP and high-FIP elements. These lines are formed over a wide range of temperatures, enabling the analysis of the different layers of the solar atmosphere. SPICE will use these spectroheliograms to produce dynamic composition maps of the solar atmosphere to be compared to in-situ measurements of the solar wind composition of the same elements (i.e. O, Ne, Mg, Fe). This will provide a tool to study the connectivity between the spacecraft (the Heliosphere) and the Sun. We will discuss the SPICE capabilities for such composition measurements. Title: On the Fourier and Wavelet Analysis of Coronal Time Series Authors: Auchère, F.; Froment, C.; Bocchialini, K.; Buchlin, E.; Solomon, J. Bibcode: 2016ApJ...825..110A Altcode: 2016arXiv160605251A Using Fourier and wavelet analysis, we critically re-assess the significance of our detection of periodic pulsations in coronal loops. We show that the proper identification of the frequency dependence and statistical properties of the different components of the power spectra provides a strong argument against the common practice of data detrending, which tends to produce spurious detections around the cut-off frequency of the filter. In addition, the white and red noise models built into the widely used wavelet code of Torrence & Compo cannot, in most cases, adequately represent the power spectra of coronal time series, thus also possibly causing false positives. Both effects suggest that several reports of periodic phenomena should be re-examined. The Torrence & Compo code nonetheless effectively computes rigorous confidence levels if provided with pertinent models of mean power spectra, and we describe the appropriate manner in which to call its core routines. We recall the meaning of the default confidence levels output from the code, and we propose new Monte-Carlo-derived levels that take into account the total number of degrees of freedom in the wavelet spectra. These improvements allow us to confirm that the power peaks that we detected have a very low probability of being caused by noise. Title: Statistical analysis of CMEs' geoeffectiveness over one year of solar maximum during cycle 23 Authors: Schmieder, Brigitte; Bocchialini, Karine; Menvielle, Michel Bibcode: 2016cosp...41E1751S Altcode: Using different propagation models from the Sun to the Earth, we performed a statistical analysis over the year 2002 on CME's geoeffectiveness linked to sudden storm commencements (ssc). We also classified the perturbations of the interplanetary medium that trigger the sscs. For each CME, the sources on the Sun of the CME are identified as well as the properties of the parameters deduced from spacecraft measurements along the path of the CME related event, in the solar atmosphere, the interplanetary medium, and the Earth ionized (magnetosphere and ionosphere) and neutral (thermosphere) environments. The set of observations is statistically analysed so as to evaluate the geoeffectiveness of CMEs in terms of ionospheric and thermospheric signatures, with attention to possible differences related to different kinds of solar sources. The observed Sun-to-Earth travel times are compared to those estimated using the existing models of propagation in the interplanetary medium, and this comparison is used to statistically assess the performances of the various models. Title: Evidence for Evaporation-incomplete Condensation Cycles in Warm Solar Coronal Loops Authors: Froment, C.; Auchère, F.; Bocchialini, K.; Buchlin, E.; Guennou, C.; Solomon, J. Bibcode: 2015ApJ...807..158F Altcode: 2015arXiv150408129F Quasi-constant heating at the footpoints of loops leads to evaporation and condensation cycles of the plasma: thermal non-equilibrium (TNE). This phenomenon is believed to play a role in the formation of prominences and coronal rain. However, it is often discounted as being involved in the heating of warm loops because the models do not reproduce observations. Recent simulations have shown that these inconsistencies with observations may be due to oversimplifications of the geometries of the models. In addition, our recent observations reveal that long-period intensity pulsations (several hours) are common in solar coronal loops. These periods are consistent with those expected from TNE. The aim of this paper is to derive characteristic physical properties of the plasma for some of these events to test the potential role of TNE in loop heating. We analyzed three events in detail using the six EUV coronal channels of the Solar Dynamics Observatory/Atmospheric Imaging Assembly. We performed both a differential emission measure (DEM) and a time-lag analysis, including a new method to isolate the relevant signal from the foreground and background emission. For the three events, the DEM undergoes long-period pulsations, which is a signature of periodic heating even though the loops are captured in their cooling phase, as is the bulk of the active regions. We link long-period intensity pulsations to new signatures of loop heating with strong evidence for evaporation and condensation cycles. We thus simultaneously witness widespread cooling and TNE. Finally, we discuss the implications of our new observations for both static and impulsive heating models. Title: The SUMER Data in the SOHO Archive Authors: Curdt, W.; Germerott, D.; Wilhelm, K.; Schühle, U.; Teriaca, L.; Innes, D.; Bocchialini, K.; Lemaire, P. Bibcode: 2014SoPh..289.2345C Altcode: 2013arXiv1309.1314C We have released an archive of all observational data of the VUV spectrometer Solar Ultraviolet Measurements of Emitted Radiation (SUMER) on SOHO that have been acquired until now. The operational phase started with `first light' observations on 27 January 1996 and will end in 2014. Future data will be added to the archive when they become available. The archive consists of a set of raw data (Level 0) and a set of data that are processed and calibrated to the best knowledge we have today (Level 1). This communication describes step by step the data acquisition and processing that has been applied in an automated manner to build the archive. It summarizes the expertise and insights into the scientific use of SUMER spectra that has accumulated over the years. It also indicates possibilities for further enhancement of the data quality. With this article we intend to convey our own understanding of the instrument performance to the scientific community and to introduce the new, standard FITS-format database. Title: Long-period intensity pulsations in the solar corona during activity cycle 23 Authors: Auchère, F.; Bocchialini, K.; Solomon, J.; Tison, E. Bibcode: 2014A&A...563A...8A Altcode: 2013arXiv1312.3792A We report on the detection (10σ) of 917 events of long-period (3 to 16 h) intensity pulsations in the 19.5 nm passband of the SOHO Extreme ultraviolet Imaging Telescope. The data set spans from January 1997 to July 2010, i.e. the entire solar cycle 23 and the beginning of cycle 24. The events can last for up to six days and have relative amplitudes up to 100%. About half of the events (54%) are found to happen in active regions, and 50% of these have been visually associated with coronal loops. The remaining 46% are localized in the quiet Sun. We performed a comprehensive analysis of the possible instrumental artefacts and we conclude that the observed signal is of solar origin. We discuss several scenarios that could explain the main characteristics of the active region events. The long periods and the amplitudes observed rule out any explanation in terms of magnetohydrodynamic waves. Thermal non-equilibrium could produce the right periods, but it fails to explain all the observed properties of coronal loops and the spatial coherence of the events. We propose that moderate temporal variations of the heating term in the energy equation, so as to avoid a thermal non-equilibrium state, could be sufficient to explain those long-period intensity pulsations. The large number of detections suggests that these pulsations are common in active regions. This would imply that the measurement of their properties could provide new constraints on the heating mechanisms of coronal loops.

Movies are available in electronic form at http://www.aanda.org Title: Observations and possible interpretations of very long period intensity pulsations in solar coronal loops Authors: Froment, Clara; Solomon, Jacques; Buchlin, Eric; Bocchialini, Karine; Auchere, Frederic; Guennou, Chloe Bibcode: 2014cosp...40E.903F Altcode: We discovered that intensity pulsations with periods ranging from 3 to 16 hours are common in solar coronal loops. Initially developed for EIT/SOHO 195 nm images, the automatic detection algorithm is now running on AIA/SDO data and allows detection of pulsation events in six coronal bands simultaneously. From may 2010 to december 2013, we detected more than 2000 events in the 6 EUV bands. We focus our study on pulsations in active regions and in particular in solar coronal loops where most of events are detected. A multi-wavelength analysis of some characteristic events is presented to help understand their physical nature. We perform a Differential Emission Measure analysis on AIA time series in order to determine the temporal variations of the thermal structure of the pulsating loops. This analysis gives important clues to investigate possible physical interpretations in particular in term of small perturbations of loops in static equilibrium and to study how this can constraint coronal heating models. We will also compare our observations to the results of a MHD turbulence and heating model of coronal loops. Title: Can the Differential Emission Measure Constrain the Timescale of Energy Deposition in the Corona? Authors: Guennou, C.; Auchère, F.; Klimchuk, J. A.; Bocchialini, K.; Parenti, S. Bibcode: 2013ApJ...774...31G Altcode: 2013arXiv1306.3114G In this paper, the ability of the Hinode/EIS instrument to detect radiative signatures of coronal heating is investigated. Recent observational studies of active region cores suggest that both the low and high frequency heating mechanisms are consistent with observations. Distinguishing between these possibilities is important for identifying the physical mechanism(s) of the heating. The differential emission measure (DEM) tool is one diagnostic that allows us to make this distinction, through the amplitude of the DEM slope coolward of the coronal peak. It is therefore crucial to understand the uncertainties associated with these measurements. Using proper estimations of the uncertainties involved in the problem of DEM inversion, we derive confidence levels on the observed DEM slope. Results show that the uncertainty in the slope reconstruction strongly depends on the number of lines constraining the slope. Typical uncertainty is estimated to be about ±1.0 in the more favorable cases. Title: Tomographic reconstructions of large scale coronal structures Authors: Guennou, C.; Auchère, F.; Seaton, D.; Canou, A.; Barbey, N.; Bocchialini, K. Bibcode: 2013enss.confE..83G Altcode: Classical plasma diagnostic techniques suffer from the line of sight (LOS) integration problem, which can confuse structures to the point that measurements crucial to the understanding of coronal physics are difficult to interpret. Tomography provides one way of understanding the LOS content, giving important insights on the morphology and physical properties of the coronal structures. Large scale, long-lived, arch-like structures are observed in the field of view of EUV telescopes at mid-latitudes, most notably in the 174 nm passband. In the present work, we use tomographic inversions of the solar corona the 3D morphology of these structures. We focus on a 28 days period of data from July/August 2012 during which some of these features were observed up to 1.7 Rsol by the SWAP/PROBA2 telescope. Additional multi-wavelength observations in the 6 bands of AIA/SDO are used to derive the corresponding 3-D maps of electron density and temperature. The results are then compared with global magnetic field extrapolations. We conclude by proposing an interpretation of the morphology of these structures as seen in EUV images. Title: GAIA-DEM : The Gaussian AIA DEm Maps database Authors: Guennou, C.; Auchère, F.; Soubrié, E.; Bocchialini, K. Bibcode: 2013enss.confE...7G Altcode: Providing the amount of emitting material as a function of the temperature along the line-of-sight, the Differential Emisssion Measure (DEM) analysis is a widespread diagnostic tool, used for most types of coronal structures. With six available coronal bands, the AIA instrument on board the SDO satellite provides new possibilities to more reliably estimate the DEM than previous UV imagers, and over a large FOV. The purpose of this database is to provide synoptic Gaussian DEM inversions of the AIA data. Using our recent results (Guennou et al. 2012a and 2012b), these maps can be then interpreted, taking advantage of our new tools developed to facilitate the DEM interpretation. The GAIA database provides the best Gaussian DEM fit matching the observations. A Gaussian form is a good first order approximation to determine the main thermal characteristics of the coronal plasma. With generally four inversions per day, at a 6 hours cadence, this database enables the user to quickly examine the global evolution of the thermal structure of the solar corona. DEM maps are available at http://medoc-dem.ias.u-psud.fr/. Title: Can the Differential Emission Measure diagnostic be used to constrain the timescale of energy deposition in the corona? Authors: Guennou, C.; Auchère, F.; Klimchuk, J. A.; Bocchialini, K.; Parenti, S. Bibcode: 2013enss.confE..34G Altcode: Differential emission measure (DEM) analysis is a widespread tool used to diagnose the thermal properties of coronal plasmas. The slope of the DEM distribution coolward of the coronal peak (near 3-4MK in active regions) can be used to diagnose the timescale for the energy deposition repeating on a given magnetic strand. Recent AR studies suggest that some active region cores are consistent with low frequency heating mechanisms, where the plasma cools completely before being reheated, while other show consistency with high frequency energy deposition, where rapid reheating causes the temperature to fluctuate about a particular value. Distinguishing between these possibilities is important for identifying the physical mechanism of the heating. It is therefore crucial to understand the uncertainties in measurements of observed DEM slopes. In this work, based on a probabilistic approach and Monte Carlo simulations, we carefully assess the errors in the slopes determined from EIS data. We consider both the random errors due to photon counting statistics, and the systematic errors associated with uncertainties in atomic physics and instrument calibration. The technique developed provides all the solutions consistent with the data and their associated probabilities. We demonstrate how the quality and the accuracy of the inversion are affected by the presence of noises and systematic errors, and we characterise the quality of the DEM inversion and its statistical properties. From these results, estimation of the uncertainties in the reconstructed slopes can be derived, thereby allowing a proper interpretation of the degree of agreement between observations and heating model predictions. Title: MEDIA : MEDoc Interface for AIA Authors: Alingery, P.; Soubrié, E.; Auchère, F.; Bocchialini, K.; Boignard, J. P.; Buchlin, E.; Malappert, J. C.; Parenti, S. Bibcode: 2013enss.confE..88A Altcode: MEDOC, the space solar data center at Orsay (http://www.ias.u-psud.fr/medoc) is now providing a new web access to the AIA/SDO level 1 images. This interface has the advantage of being simple, intuitive, very stable and fast. The full resolution 4k x 4k AIA level 1 images archived at MEDOC are downloaded from upstream DRMS nodes with a 1 minute cadence at all wavelengths. The dataset will be kept online on a redundant archive for the whole SDO mission duration. The FITS files are accessible via an user friendly web interface (http://medoc-sdo.ias.u-psud.fr) that allows users to request data by selecting a date range, the desired wavelengths and a sampling rate (choosing a cadence from 1 minute to 1 day). For each file, users can preview the image (using the Helioviewer tool) or display the header information before downloading the FITS files (with or without Rice-compression). This web interface was built using Sitools2, a tool developed by CNES, the French space agency, and supports most browsers. For more advanced users, a Search/Get Python module is also available at http://sdo.ias.u-psud.fr/python. The users can use it to build more complex yet more powerful queries. We encourage everyone in Europe and beyond to use these new services! Title: On the Accuracy of the Differential Emission Measure Diagnostics of Solar Plasmas. Application to SDO/AIA. II. Multithermal Plasmas Authors: Guennou, C.; Auchère, F.; Soubrié, E.; Bocchialini, K.; Parenti, S.; Barbey, N. Bibcode: 2012ApJS..203...26G Altcode: 2012arXiv1210.2302G Differential emission measure (DEM) analysis is one of the most used diagnostic tools for solar and stellar coronae. Being an inverse problem, it has limitations due to the presence of random and systematic errors. We present in this series of papers an analysis of the robustness of the inversion in the case of SDO/AIA observations. We completely characterize the DEM inversion and its statistical properties, providing all the solutions consistent with the data along with their associated probabilities, and a test of the suitability of the assumed DEM model. While Paper I focused on isothermal conditions, we now consider multithermal plasmas and investigate both isothermal and multithermal solutions. We demonstrate how the ambiguity between noises and multithermality fundamentally limits the temperature resolution of the inversion. We show that if the observed plasma is multithermal, isothermal solutions tend to cluster on a constant temperature whatever the number of passbands or spectral lines. The multithermal solutions are also found to be biased toward near-isothermal solutions around 1 MK. This is true even if the residuals support the chosen DEM model, possibly leading to erroneous conclusions on the observed plasma. We propose tools for identifying and quantifying the possible degeneracy of solutions, thus helping the interpretation of DEM inversion. Title: On the Accuracy of the Differential Emission Measure Diagnostics of Solar Plasmas. Application to SDO/AIA. I. Isothermal Plasmas Authors: Guennou, C.; Auchère, F.; Soubrié, E.; Bocchialini, K.; Parenti, S.; Barbey, N. Bibcode: 2012ApJS..203...25G Altcode: 2012arXiv1210.2304G Differential emission measure (DEM) analysis is a major diagnostic tool for stellar atmospheres. However, both its derivation and its interpretation are notably difficult because of random and systematic errors, and the inverse nature of the problem. We use simulations with simple thermal distributions to investigate the inversion properties of SDO/AIA observations of the solar corona. This allows a systematic exploration of the parameter space, and using a statistical approach the respective probabilities of all the DEMs compatible with the uncertainties can be computed. Following this methodology, several important properties of the DEM inversion, including new limitations, can be derived and presented in a very synthetic fashion. In this first paper, we describe the formalism and we focus on isothermal plasmas as building blocks to understand the more complex DEMs studied in the second paper. The behavior of the inversion of AIA data being thus quantified, and we provide new tools to properly interpret the DEM. We quantify the improvement of the isothermal inversion with six AIA bands compared to previous EUV imagers. The maximum temperature resolution of AIA is found to be 0.03 log Te , and we derive a rigorous test to quantify the compatibility of observations with the isothermal hypothesis. However, we demonstrate limitations in the ability of AIA alone to distinguish different physical conditions. Title: Studying Sun-Planet Connections Using the Heliophysics Integrated Observatory (HELIO) Authors: Pérez-Suárez, D.; Maloney, S. A.; Higgins, P. A.; Bloomfield, D. S.; Gallagher, P. T.; Pierantoni, G.; Bonnin, X.; Cecconi, B.; Alberti, V.; Bocchialini, K.; Dierckxsens, M.; Opitz, A.; Le Blanc, A.; Aboudarham, J.; Bentley, R. B.; Brooke, J.; Coghlan, B.; Csillaghy, A.; Jacquey, C.; Lavraud, B.; Messerotti, M. Bibcode: 2012SoPh..280..603P Altcode: 2012SoPh..tmp..215P The Heliophysics Integrated Observatory (HELIO) is a software infrastructure involving a collection of web services, heliospheric data sources (e.g., solar, planetary, etc.), and event catalogues - all of which are accessible through a unified front end. In this paper we use the HELIO infrastructure to perform three case studies based on solar events that propagate through the heliosphere. These include a coronal mass ejection that intersects both Earth and Mars, a solar energetic particle event that crosses the orbit of Earth, and a high-speed solar wind stream, produced by a coronal hole, that is observed in situ at Earth (L1). A ballistic propagation model is run as one of the HELIO services and used to model these events, predicting if they will interact with a spacecraft or planet and determining the associated time of arrival. The HELIO infrastructure streamlines the method used to perform these kinds of case study by centralising the process of searching for and visualising data, indicating interesting features on the solar disk, and finally connecting remotely observed solar features with those detected by in situ solar wind and energetic particle instruments. HELIO represents an important leap forward in European heliophysics infrastructure by bridging the boundaries of traditional scientific domains. Title: On the Thermal diagnostics of Coronal Loops with SDO/AIA Authors: Guennou, Chloe; Parenti, Susanna; Bocchialini, Karine; Soubrie, Elie; Auchere, Frederic; Barbey, Nicolas Bibcode: 2012cosp...39..675G Altcode: 2012cosp.meet..675G With simultaneous observations in 6 coronal bands, AIA has the capability to provide spectral diagnostics over an extended field of view at high resolution and high cadence. Therefore, DEM diagnostics of coronal loops can in principle be performed routinely for statistical studies. We investigate here the pertinence of the DEM analysis with AIA. The inevitable presence of noises and uncertainties, incompleteness of the atomic physics databases lead to notable difficulties in the inversion process. The complications involved in the derivation of the DEM are one of the reasons of the controversial results regarding the thermal structure and thus the heating scenario of the coronal loops. The purpose of this work, based on a probabilistic approach, is precisely to investigate the properties of the solutions, providing a quantification of the DEM inversion problem robustness. The technique relies on Monte Carlo simulations of observed intensities in the six AIA coronal bands. The comparison between the known inputs and the inversion results allows us to determine the degree of robustness. This approach provides all the solutions consistent with the data along with their associated probabilities, as well as a test of the validity of the assumptions made on the DEM shape. Applications to SDO/AIA coronal loops data are presented. Title: Homologous flares inducing EUV filament oscillations with subsequent eruption Authors: Bocchialini, K.; Koutchmy, S.; Solomon, J.; Tavabi, E. Bibcode: 2012EAS....55..335B Altcode: We focus our analysis on an event which occurred at the W-limb on May 30, 2003. The dynamical behavior of the filament, including damped oscillations, was investigated with the CDS and EIT (SoHO) experiments, as well as with Hα filtergrams (movies). The eruptive phase is analyzed taking into account the approximate phasing with other eruptive phenomena occurring at the same time or before, called homologous flares and eruptions. Title: HELIO - A Research Environment for Heliophysics Authors: Bentley, R. D.; Abourdarham, J.; Csillaghy, A.; Messerotti, M.; Gallagher, P.; Bocchialini, K.; Jacquey, C.; Hapgood, M. Bibcode: 2012EGUGA..1411634B Altcode: HELIO, the Heliophysics Integrated Observatory, is a research infrastructure funded under Capacities programme of the EC's 7th Framework Programme (FP7). It provides a collaborative environment where scientists can discover, understand and model the connection between solar phenomena, interplanetary disturbances and their effects on the planets. The project is designed around a service-oriented architecture with needed capabilities that support metadata curation and search, data location and retrieval, and data processing and storage being established as independent services. HELIO provides integrated access to the data and metadata from the domains that constitute heliophysics - solar, heliospheric, geophysics and planetary. More than 50 event catalogues can be used in the search, together with just under 10 feature catalogues; data from more than 150 instruments from nearly 50 observatories can be accessed. A comprehensive user interface is available and the serves can also be accessed through IDL; a workflow tool provides the ability to combine services together and it is possible to execute programmes on demand including propagation models. We will report on the status of HELIO and the services that are available and demonstrate how these resources can be used to address use cases involving multiple spacecraft and modelling. We will also describe how we hope to combine the tools developed by HELIO into a Collaborative Research Environment for Heliophysics. We have been holding a series of Coordinated Data Analysis Workshops (CDAW) in which we demonstrate the capabilities of the project and participants are able to use them to address science use cases. Two CDAWs have been held so far, in Dublin and Trieste; a third will be held in February 2012 in Orsay, and a fourth is planned in May/June 2012. Typical use cases relate to phenomena propagating from the Sun and being observed by at least two observatories in different parts of the inner Solar System. The HELIO Consortium includes thirteen groups from the UK, France, Ireland, Italy, Switzerland, Spain and the US; the project started in June 2009 and has a duration of 36 months Title: SOHO observations of oscillatory motions in an eruptive filament: Intensity and velocity variations Authors: Bocchialini, K.; Koutchmy, S.; Solomon, J. Bibcode: 2011sf2a.conf..369B Altcode: The variations in intensity and velocity inside an eruptive filament, observed on May 30, 2003 with CDS and EIT on-board SOHO, are analysed in the transition region He I line and the coronal Mg X line. Vertical oscillating motions of the filament with damped velocity oscillations before its disappearance are revealed. The link between theses oscillations, the flaring regions nearby and the filament eruption is investigated. Title: Oscillatory motions observed in eruptive filaments Authors: Bocchialini, K.; Baudin, F.; Koutchmy, S.; Pouget, G.; Solomon, J. Bibcode: 2011A&A...533A..96B Altcode: 2011arXiv1107.0596B Context. The origin of the variable component of the solar wind is of great intrinsic interest for heliophysics and spaceweather, e.g. the initiation of coronal mass ejections and the problem of mass loss of all stars. It is also related to the physics of coronal neutral sheets and streamers, which occur above lines of magnetic polarity reversal. Filaments and prominences correspond to the cool coronal component of these regions.
Aims: We examine the dynamical behaviour of these structures where reconnection and dissipation of magnetic energy in the turbulent plasma are occurring. The link between the observed oscillatory motions and the eruption occurrence is investigated in detail for two different events.
Methods: Two filaments were analysed using two different datasets: time series of spectra using a transition region line (He I at 584.33 Å) and a coronal line (Mg X at 609.79 Å) measured with CDS on-board SOHO, observed on May 30, 2003, and time series of intensity and velocity images from the NSO/Dunn Solar Telescope in the Hα line on September 18, 1994 for the other. The oscillatory content was investigated using Fourier transform and wavelet analysis and compared to different models.
Results: In both filaments, oscillations are clearly observed, in intensity and velocity in the He I and Mg X lines, in velocity in Hα, with similar periods from a few minutes up to 80 min, with a main range from 20 to 30 min, simultaneously with eruptions. Both filaments exhibit vertical oscillating motions. For the filament observed in the UV (He I and Mg X lines), we provide evidence of damped velocity oscillations, and for the filament observed in the visible (Hα line), we provide evidence that parts of the filament are oscillating, while the filament is moving over the solar surface, before its disappearance. Title: HELIO: The Heliophysics Integrated Observatory Authors: Bentley, R. D.; Csillaghy, A.; Aboudarham, J.; Jacquey, C.; Hapgood, M. A.; Bocchialini, K.; Messerotti, M.; Brooke, J.; Gallagher, P.; Fox, P.; Hurlburt, N.; Roberts, D. A.; Duarte, L. Sanchez Bibcode: 2011AdSpR..47.2235B Altcode: Heliophysics is a new research field that explores the Sun-Solar System Connection; it requires the joint exploitation of solar, heliospheric, magnetospheric and ionospheric observations.HELIO, the Heliophysics Integrated Observatory, will facilitate this study by creating an integrated e-Infrastructure that has no equivalent anywhere else. It will be a key component of a worldwide effort to integrate heliophysics data and will coordinate closely with international organizations to exploit synergies with complementary domains.HELIO was proposed under a Research Infrastructure call in the Capacities Programme of the European Commission’s 7th Framework Programme (FP7). The project was selected for negotiation in January 2009; following a successful conclusion to these, the project started on 1 June 2009 and will last for 36 months. Title: The SDO data centre at IDOC/MEDOC in France Authors: Parenti, Susanna; Bocchialini, Karine; Soubrie, Elie; Auchere, Frederic; Ballans, Herv; Buchlin, Eric; Gabriel, Alan; Mercier, Claude; Poulleau, Gilles; Vial, Jean-Claude Bibcode: 2010cosp...38.2888P Altcode: 2010cosp.meet.2888P The IDOC/MEDOC centre at the Institut d'Astrophysique Spatiale (IAS, Université Paris 11/CNRS) has a long experience in solar data archiving and distribution, including almost 15 years of data from SOHO, STEREO and TRACE. The center is now expanding its activity and becoming a Pˆle Thématique Solaire of the CNES and INSU/CNRS. Part of the new activities of the centre will be linked to the arrival of the enormous volume of the new SDO data. The center will be one of the three European centers to receive and redistribute the data to the community. It will also be the only European site to permanently store about 10% of the data (mainly from AIA). In continuity with its previous activities, SDO data will be included in the data visualization tool FESTIVAL and it will provide new services, like tools for the solar feature identification (filaments, EUV intensity fluctuations). We will present an overview of the facilities and activities of the centre in relation to the SDO data. Title: On the observations and possible interpretations of very long period intensity oscillations of solar coronal loops Authors: Solomon, Jacques; Auchere, Frederic; Bocchialini, Karine; Gabriel, Alan; Tison, Emmanuelle Bibcode: 2010cosp...38.2853S Altcode: 2010cosp.meet.2853S A comprehensive analysis of intensity oscillations in the Fe XII line (19.5 nm) observed with EIT/SoHO in solar coronal loops during solar cycle 23 (january 1997-september 2008) was performed. About 450 occurences of oscillations were obtained with periods ranging between 3.4 and 13.6 hours and with durations up to about a hundred hours. Interpratations in term of slow waves or of thermal nonequilibrium were examined. However numerous inconsistencies arise between current theories (in fact mostly expressed in terms of various numerical simulations) and observations. Presently the lack of a direct link between those very long oscillation periods and the characteristic physical parameters of the loops (density, temperature, loop geometry) hampers making progress in this major issue. This situation requires an effort in a specific time analysis of the classical system of equations of the problem: the question is examined from different angles in relation to the data. Title: Distributing and mining SDO data in Europe Authors: Parenti, Susanna; Delouille, Véronique; Dalla, Silvia; Bocchialini, Karine; Ballans, Herv; Boyes, David; Chapman, Steve; Hochedez, Jean-François; Mampaey, Benjamin; March, Mike S.; Soubrie, Elie; Walsh, Robert Bibcode: 2010cosp...38.2883P Altcode: 2010cosp.meet.2883P The properties of the highly dynamic Sun will soon be revealed by the newly launched SDO, with data provided by its three instruments: AIA, HMI and EVE. This suite will produce, for the first time in solar physics, a large volume of data, equivalent to about 1.5 Tb/day, by observing the full disk Sun continuously at high cadence. A backbone network of data centres has been established to handle these data and redistribute them to Europe. The Royal Observatory of Belgium (Belgium) will receive the entire flow directly from the Harvard-Smithsonian Center for Astrophysics. This will next be further redistributed to University of Central Lancashire (United Kingdom), and to Institut d'Astrophysique Spatiale (France). These institutes will also permanently store part of the data. With such huge data rate, it is necessary to develop automated algorithms that scan the data and extract information related to important events or features. The European partners have gathered within an ISSI team on 'Mining and exploiting the NASA Solar Dynamics Observatory data in Europe', a.k.a the Soldyneuro project. One of the outputs from the ISSI team will be to use the feature recognition algorithms to populate the Heliophysics Events Knowledgebase (HEK) hosted by LMSAL, and provide a service as added value to the local database centers. Title: Using HELIO to study cross-disiplinary science problems using data from multiple spacecraft Authors: Bentley, Robert; Aboudarham, Jean; Messerotti, Mauro; Jacquey, Christian; Gallagher, Peter T.; Hapgood, Mike; Bocchialini, Karine Bibcode: 2010cosp...38.1917B Altcode: 2010cosp.meet.1917B The Heliophysics Integrated Observatory, HELIO, is creating a collaborative environment where scientists can discover, understand and model the connection between solar phenomena, inter-planetary disturbances and their effects on the planets. HELIO will provide integrated access to data from the solar, heliospheric, geophysics and plan-etary domains and allow the user to undertake a search for interesting events and phenomena based solely on metadata and data products. The HELIO infrastructure will provide services to support the search that can either be used independently or as part of a work flow. The services include event and feature catalogues derived from data from all the domains and a processing capability that will use models to relate observations made in different part of the solar system. We will describe how HELIO can be used to address science problems that span the domains by allowing the user to track phenomena as they propagate through the solar system and report on progress to date. HELIO is a research infrastructure funded under Capacities programme of the EC's 7th Frame-work Programme (FP7); the project started in June 2009 and has a duration of 36 months. The HELIO Consortium includes thirteen groups from the UK, France, Ireland, Italy, Switzerland, Spain and the US. Title: Automatic detection and statistical analysis of intensity oscillations in the solar corona with SDO Authors: Auchere, Frederic; Bocchialini, Karine; Solomon, Jacques; Gabriel, Alan; Tison, Emmanuelle Bibcode: 2010cosp...38.2863A Altcode: 2010cosp.meet.2863A We present the generalization to SDO data of our automatic oscillation detection algorithm. This technique was successfully tested using EIT data on board SOHO at 19.5 nm from January 1997 to September 2008, i.e almost the entire solar cycle 23. In the EIT data set we detected 400 oscillations whose periods range between 3.4 and 13.6 h with a maximum around 6-7 hours. Most of the oscillations are localized in coronal structures associated with active regions and last several tens of hours. The AIA data will allow the detection of similar events in several coronal temperature bands simultaneously, which will help understand their physical nature. Title: Addressing Science Use Cases with HELIO Authors: Bentley, R. D.; Aboudarham, J.; Csillaghy, A.; Jacquey, C.; Hapgood, M. A.; Messerotti, M.; Gallagher, P.; Bocchialini, K.; Hurlburt, N. E.; Roberts, D.; Sanchez Duarte, L. Bibcode: 2009AGUFMSH54A..06B Altcode: The Heliophysics Integrated Observatory (HELIO) is a new VO project funded under the EC's Seventh Framework Programme (FP7). It includes thirteen partners scattered over six countries and is led by University College London. HELIO is designed to support the heliophysics community and is based on a Service Oriented Architecture. The services developed by and integrated into HELIO can be used to address a wide range of science problems; they can be used individually or as part of a work-flow driven search engine that can use a propagation (or other) model to help locate obervations that describe interesting phenomena. We will describe and discuss how the components of HELIO could be used to address science use cases, particularly how a user can adapt the work flow to their own science interests. Networking is one of the three Activities of the HELIO Integrated Infrastructure Initiatives (I3) project. Within this activity we plan to involve the community in all aspects of the design and testing of the HELIO system, including determining which data and metadata should be included, how the quality and content of metadata can be included, etc. We are investigating ways of making HELIO "domain-aware" so that researchers who are specialists in one of the communities that constitute heliophysics can easily identify, access and use data they need from the other communities. We will discuss how the community can help us develop this capability. Title: FESTIVAL: A Multiscale Visualization Tool for Solar Imaging Data Authors: Auchère, F.; Soubrié, E.; Bocchialini, K.; LeGall, F. Bibcode: 2008SoPh..248..213A Altcode: 2008SoPh..tmp...59A Since 4 December 2006, the SECCHI instrument suites onboard the two STEREO A and B probes have been imaging the solar corona and the heliosphere on a wide range of angular scales. The EUVI telescopes have a plate scale of 1.7 arcseconds pixel−1, while that of the HI2 wide-angle cameras is 2.15 arcminutes pixel−1, i.e. 75 times larger, with the COR1 and COR2 coronagraphs having intermediate plate scales. These very different instruments, aimed at studying Coronal Mass Ejections and their propagation in the heliosphere, create a data visualization challenge. This paper presents FESTIVAL, a SolarSoftware package originally developed to be able to map the SECCHI data into dynamic composite images of the sky as seen by the STEREO and SOHO probes. Data from other imaging instruments can also be displayed. Using the mouse, the user can quickly and easily zoom in and out and pan through these composite images to explore all spatial scales from EUVI to HI2 while keeping the native resolution of the original data. A large variety of numerical filters can be applied, and additional data (i.e. coordinate grids, stars catalogs, etc.) can be overlaid on the images. The architecture of FESTIVAL is such that it is easy to add support for other instruments and these new data immediately benefit from the already existing capabilities. Also, because its mapping engine is fully 3D, FESTIVAL provides a convenient environment to display images from future out-of-the-Ecliptic solar missions, such as Solar Orbiter or Solar Probe. Title: A Contribution to the Understanding of Chromospheric Oscillations Authors: Baudin, F.; Ibarra, E.; Avrett, E. H.; Vial, J. -C.; Bocchialini, K.; Costa, A.; Lemaire, P.; Rovira, M. Bibcode: 2007SoPh..241...39B Altcode: We present SUMER/SOHO UV measurements of chromospheric oscillations of intensity, velocity, and linewidth observed in C I, S I, O I, and C II lines, which are formed in the altitude range from 1000 km to 2000 km above τ500=1. Oscillations in lines originating at similar altitudes exhibit different behaviors which we discuss in terms of the formation of the lines. Title: Rotational Tomography of the Solar Corona-Calculation of the Electron Density and Temperature Authors: Barbey, Nicolas; Auchère, Frédéric; Rodet, Thomas; Bocchialini, Karine; Vial, Jean-Claude Bibcode: 2006ESASP.617E..82B Altcode: 2006soho...17E..82B No abstract at ADS Title: Two Observations of Damped Oscillations During Filament Eruptions: A Signature of the Eruptions? Authors: Pouget, G.; Bocchialini, K.; Solomon, J. Bibcode: 2006ESASP.617E.141P Altcode: 2006soho...17E.141P No abstract at ADS Title: Oscillations in a solar filament: first observation of long periods in the HeI 584.33 Å line, modelling and diagnostic Authors: Pouget, G.; Bocchialini, K.; Solomon, J. Bibcode: 2006A&A...450.1189P Altcode: Three long observations of filaments were carried out in the 584.33 HeI line during MEDOC campaigns in November 2003 and November 2004, by the Coronal Diagnostic Spectrometer onboard SOHO. Their duration was 15-16 h and the temporal resolution was 20 s, allowing measurements of the entire range of periodicities theoretically expected in a filament (particularly both the short periods, less than 10 min, and the long ones, more than 40 min). Fourier analysis of the Doppler velocities in the filament allows us to detect oscillations over a wide range, and particularly very slow velocity oscillations (5-6 h) that were not detected previously. We test an earlier interpretation of these velocity oscillations in the prominence model of Joarder & Roberts (1993, A&A, 277, 225), who treat the prominence as a slab. We used a systematic method to identify the six fundamental modes predicted by the model among the numerous frequencies detected. Identification of these modes - and especially the slowest one, the slow kink mode - provides a complete diagnostic of the filament in terms of the Alfvén speed, temperature, and angle between the magnetic field and the main axis of the filament. Title: From the Sun to the Earth: impact of the 27-28 May 2003 solar events on the magnetosphere, ionosphere and thermosphere Authors: Hanuise, C.; Cerisier, J. C.; Auchère, F.; Bocchialini, K.; Bruinsma, S.; Cornilleau-Wehrlin, N.; Jakowski, N.; Lathuillère, C.; Menvielle, M.; Valette, J. -J.; Vilmer, N.; Watermann, J.; Yaya, P. Bibcode: 2006AnGeo..24..129H Altcode: During the last week of May 2003, the solar active region AR 10365 produced a large number of flares, several of which were accompanied by Coronal Mass Ejections (CME). Specifically on 27 and 28 May three halo CMEs were observed which had a significant impact on geospace. On 29 May, upon their arrival at the L1 point, in front of the Earth's magnetosphere, two interplanetary shocks and two additional solar wind pressure pulses were recorded by the ACE spacecraft. The interplanetary magnetic field data showed the clear signature of a magnetic cloud passing ACE. In the wake of the successive increases in solar wind pressure, the magnetosphere became strongly compressed and the sub-solar magnetopause moved inside five Earth radii. At low altitudes the increased energy input to the magnetosphere was responsible for a substantial enhancement of Region-1 field-aligned currents. The ionospheric Hall currents also intensified and the entire high-latitude current system moved equatorward by about 10°. Several substorms occurred during this period, some of them - but not all - apparently triggered by the solar wind pressure pulses. The storm's most notable consequences on geospace, including space weather effects, were (1) the expansion of the auroral oval, and aurorae seen at mid latitudes, (2) the significant modification of the total electron content in the sunlight high-latitude ionosphere, (3) the perturbation of radio-wave propagation manifested by HF blackouts and increased GPS signal scintillation, and (4) the heating of the thermosphere, causing increased satellite drag. We discuss the reasons why the May 2003 storm is less intense than the October-November 2003 storms, although several indicators reach similar intensities. Title: Toward a Virtual Observatory for Solar System Plasmas: an exceptional scientific opportunity Authors: Jacquey, C.; Bocchialini, K.; Aboudarham, J.; Meunier, N.; Andre, N.; Genot, V.; Harvey, C.; Budnik, E.; Hitier, R.; Gangloff, M.; Bouchemit, M. Bibcode: 2006epsc.conf..714J Altcode: During the coming years, the "Solar System Plasma" environment will be explored by an exceptional set of observatories : RHESSI, SOHO, STEREO, SOLAR-B and ground based observatories will all provide continuous observations of the Sun and its corona. In situ plasma and field measurements will be obtained at and near Mercury (MESSENGER), Venus (VEX), Earth (ACE, WIND, GEOTAIL, CLUSTER, THEMIS), Mars (MEX, MGS) and Saturn (CASSINI), and inside the heliosphere (STEREO, ULYSSES, VOYAGER). These data will be complemented by UV and radio astronomical observations of Jovian, Saturnian and terrestrial auroral activity. This wealth of data will offer previously unequalled opportunities to study (i) global and multi-scale phenomena of the inner heliosphere (ii) the propagation of the solar perturbations and space meteorology, (iii) local interplanetary conditions around planets and (iv) the comparison of the ionised environments of various planets. However, the exploitation of all these data is a major technical challenge, as it requires accessing heterogeneous data from diverse origins to perform an integrated study using software tools appropriate for analysis of the phenomena observed. Moreover, the huge amount of data to manage coming from future space and ground based instruments requires extraction that could no more be done by hand, but automatically. This challenge is unlikely to be met by instrument teams or laboratories working individually ; it requires collaboration of the whole international community through a Virtual Observatory. The Europlanet/IDIS prototype will give a foretaste of what will be achievable by a Virtual Observatory for planetology. The overlap in functionality between a "Planetary VO" and a "Solar System Plasma VO" remains to be defined, but both are undoubtedly essential and complimentary components of any Solar System VO. In this paper, we present potential science cases in Space Plasma, which we then use to identify requirements for the access and analysis tools needed to exploit the promised exceptional harvest of solar and in situ plasma data. Title: The Beleinos cornerstone: the Sun, the star close to Earth Authors: Appourchaux, T.; Auchère, F.; Bocchialini, K.; Bonnet, R. M.; Gabriel, A.; Vial, J. -C. Bibcode: 2005ESASP.588..389A Altcode: 2005tssc.conf..389A No abstract at ADS Title: About the fe XIV 530.3 NM Line Emissions of the Middle Corona Authors: Koutchmy, S.; Contesse, L.; Viladrich, Ch.; Vilinga, J.; Bocchialini, K. Bibcode: 2005ESASP.600E..26K Altcode: 2005ESPM...11...26K; 2005dysu.confE..26K No abstract at ADS Title: The August 11th, 1999 CME Authors: Koutchmy, S.; Baudin, F.; Bocchialini, K.; Daniel, J. -Y.; Delaboudinière, J. -P.; Golub, L.; Lamy, P.; Adjabshirizadeh, A. Bibcode: 2004A&A...420..709K Altcode: We present here a set of observations, space borne and ground based, at different wavelengths, of the solar corona at and after the time of the total solar eclipse of August 11{th}. It is used to consider some unusual features of the coronal dynamics related to a limb Coronal Mass Ejection (CME) observed after the total eclipse. The complementary aspect of simultaneous ground-based and space-borne observations of the corona is used to produce an accurate composite image of the White Light (W-L) corona before the CME. A high arch system (possibly a dome-like structure, with large cavities inside but without a cusp further out) which appeared on the eclipse W-L images, is suggested to be a large-scale precursor of the CME, well preceding the eruption of the top part of the brightest prominence recorded in W-L. This bright prominence is shown as a filament in absorption using the Transition Region And Corona Explorer (TRACE) images taken in different coronal lines. The analysis of the images of the Large Angle and Spectrometric Coronograph (LASCO) on board the Solar and Heliospheric Observatory (SoHO), showing the progression of the CME, is discussed in an attempt to make a connection with the surface event. A SoHO-EIT (Extreme UV Imager Telescope) image sequence details the prominence eruption and shows the sudden heating processes of the ejected parts. We found that there is no reason to assume that the huge cavity is significantly destabilised well before the eruption of the upper part of the low-lying bright twisted filament which coincides with the position of one of the legs of the high arch. Observations are still compatible with the assumption of both the break-out model and of the flux rope erupting model as a result of a shear or of an increasing poloıdal magnetic flux from below. We stress the possible role of buoyancy of the giant cavity as a destabilizing factor leading to the CME, noticing that some motion of coronal material back toward the surface can be seen during at least the first phase of the CME, from both EIT and LASCO observations. Title: Analysis of the oscillations in the solar prominences with Soho (CD-SUMER) Authors: Pouget, G.; Bocchialini, K.; Solomon, J. Bibcode: 2004cosp...35.4231P Altcode: 2004cosp.meet.4231P Solar prominences (also called filaments when they are seen on the disk) often exhibit oscillatory movements. These oscillations may result in instability, thus causing the ejection of some of the prominence's mass, which contributes to the solar wind. By studying the different oscillation modes that occur inside prominences, we would intend to infer characteristic predicting signatures of CMEs. Series of observations were carried out in 2003 by the SUMER and CDS UV spectrometers on SoHO, simultaneously in several spectral lines, and with long duration for some events (>16 hours). The Fourier analysis of the Doppler velocities in the filament allows us to detect oscillations (after having set a detection threshold). A comparison is done between the observed frequencies and the frequencies calculated considering the prominence model of Joarder & Roberts (1993). By identifying observed and calculated frequencies, we were able in general to find four of the six oscillation modes of the model. This identification provides a diagnostic of the filament, in terms of magnetic field, temperature, density, and angle between the magnetic field and the main axis of the filament. More specifically, in the case of the longer sequences, we are presently interested in identifying the lower frequency modes of oscillations in order to put more constraints on the prominence physical parameters. Title: The solar high-resolution imager - coronagraph LYOT mission Authors: Vial, Jean-Claude; Song, Xueyan; Lemaire, Philippe; Gabriel, Alan H.; Delaboudiniere, Jean-Pierre; Bocchialini, Karine; Koutchmy, Serge L.; Lamy, Philippe L.; Mercier, Raymond; Ravet, Marie Francoise; Auchere, Frederic Bibcode: 2003SPIE.4853..479V Altcode: The LYOT (LYman Orbiting Telescope) solar mission is proposed to be implemented on a micro-satellite of CNES (France) under phase A study. It includes two main instruments, which image the solar disk and the low corona up to 2.5 Ro in the H I Lyman-α line at 121.6 nm. The spatial resolution is about 1” for the disk and 2.5” for corona. It also carries an EIT-type telescope in the He II (30.4 nm) line. The coronagraph needs a super polished mirror at the entrance pupil to minimize the light scattering. Gratings and optical filters are used to select the Lyman-α wavelength. VUV cameras with 2048×2048 pixels record solar images up to every 10 seconds. The satellite operates at a high telemetry rate (more then 100 kb/s, after onboard data compression). The envisaged orbits are either geostationary or heliosynchronous. Possible launch dates could be end of 2006 - beginning of 2007. Title: The August 11th, 1999 total eclipse CME Authors: Koutchmy, S.; Baudin, F.; Bocchialini, K.; Delaboudinière, J. -P.; Adjabshirizadeh, A. Bibcode: 2002ESASP.477...55K Altcode: 2002scsw.conf...55K We use spaceborne observations and ground-based eclipse observations to analyse the spectacular W-limb CME which occurred several hours after the totality in Iran. The underlying high arch system (possibly a dome-like structure with cavities inside) which appeared on the eclipse White-Light (W-L) images, is suggested to be a large scale precursor of the CME, taking into account the related coronal cavities (as measured from the broadening of the green Fe XIV line) and the properties of the inserted prominence which erupted during the CME. Title: On a mechanism of intensification of field-aligned currents at the solar chromosphere-quiescent prominence boundaries Authors: Nenovski, P.; Dermendjiev, V. N.; Detchev, M.; Vial, J. -C.; Bocchialini, K. Bibcode: 2001A&A...375.1065N Altcode: Field-aligned electric currents (FAC) are assumed to support various prominence configurations and it is usually supposed that the quiescent prominence (QP) destabilisation can be initiated by some plasma instability. In this work we study another possibility of QP destabilisation connected with FAC changes. Such a destabilisation may occur when FAC flowing along a loop-shaped QP structure are intensified by bouncing surface MHD modes, presumably generated by motions in the photosphere under, or adjacent to, the QP. The MHD disturbances at the prominence ``feet'' propagate upwards as Alfven waves and surface modes. We study the possibility that the generated MHD modes, which carry FAC, bounce in the loop-shaped QP structure, provided that they undergo multiple reflection at the prominence feet. This is an interesting physical situation leading to intensification of FAC and promising to be another source of QP destabilisation. Title: Joint EUV/Radio Observations of a Solar Filament Authors: Chiuderi Drago, F.; Alissandrakis, C. E.; Bastian, T.; Bocchialini, K.; Harrison, R. A. Bibcode: 2001SoPh..199..115C Altcode: In this paper we compare simultaneous extreme ultraviolet (EUV) line intensity and microwave observations of a filament on the disk. The EUV line intensities were observed by the CDS and SUMER instruments on board SOHO and the radio data by the Very Large Array and the Nobeyama radioheliograph. The main results of this study are the following: (1) The Lyman continuum absorption is responsible for the lower intensity observed above the filament in the EUV lines formed in the transition region (TR) at short wavelengths. In the TR lines at long wavelengths the filament is not visible. This indicates that the proper emission of the TR at the filament top is negligible. (2) The lower intensity of coronal lines and at radio wave lengths is due to the lack of coronal emission: the radio data supply the height of the prominence, while EUV coronal lines supply the missing hot matter emission measure (EM). (3) Our observations support a prominence model of cool threads embedded in the hot coronal plasma, with a sheath-like TR around them. From the missing EM we deduce the TR thickness and from the neutral hydrogen column density, derived from the Lyman continuum and He i absorption, we estimate the hydrogen density in the cool threads. Title: Dynamics of a Quiescent Solar Prominence Observed with the SUMER/SOHO Instrument Authors: Bocchialini, K.; Costa, A.; Domenech, G.; Rovira, M.; Vial, J. C.; Wingfield, K. Bibcode: 2001SoPh..199..133B Altcode: We present the results obtained from analyzing SUMER/SOHO observational data of a quiescent solar prominence. The studied prominence is made of complex structures. From the 1-hr data set, we derive characteristic frequencies in terms of intensity and velocity oscillations, as measured in 4 transition-region lines. The presence of different types of frequencies is detected: chromospheric oscillations and intermediate periods (6 min to 12 min). This result suggests that these oscillations are transmitted by the magnetic fields from the chromosphere to the transition region. Title: An Observational Test for Solar Atmospheric Heating Authors: van Driel-Gesztelyi, L.; Démoulin, P.; Ireland, J.; Thompson, B.; Fludra, A.; Oláh, K.; Kövári, Zs.; Harra, L. K.; Mandrini, C. H.; Bocchialini, K.; Orlando, S. Bibcode: 2001IAUS..203..514V Altcode: We study the evolution of the emissivity and heating correlated with magnetic observables of an active region from its birth throughout its decay during seven solar rotations (July-Dec. 1996). Taking one "snapshot" per g:wq: Command not found. time of flares, we analyse multi-wavelength and multi-instrument data obtained from SOHO (MDI, EIT, CDS and SUMER), Yohkoh (SXT), GOES, SOLSTICE and 10.7 cm radio data from DRAO, Canada. We utilise our results to test the validity of coronal heating models. We find that models which are based on the dissipation of stressed, current-carrying magnetic fields are in better agreement with the observations than the models which attribute coronal heating to the dissipation of MHD waves. Title: Oscillations Observed in Intensity and Velocity for a Quienscent Prominence Authors: Bocchialini, K.; Costa, A.; Domenech, G.; Rovira, M.; Vial, J. -C. Bibcode: 2001IAUS..203..419B Altcode: We present the results obtained from analyzing SUMER/SOHO observation data of a solar prominence. The studied prominence can be characterized as having a complex structure. From the 1 hour data set, we derived characteristic frequencies in terms of intensity and velocity oscillations, for 4 transition region lines. The homogenity in the characteristic frequencies suggests the engagemente of coronal oscillations with the chromospheric structure. The presence of different types of frequencies is detected: chromospheric oscillations, intermediate periods (6min to 12min) and also long periods (25min to 51min). This result suggests that these oscillations are transmitted by the magnetic fields. Title: Microscale Structures on the Quiet Sun and Coronal Heating Authors: Aletti, V.; Velli, M.; Bocchialini, K.; Einaudi, G.; Georgoulis, M.; Vial, J. -C. Bibcode: 2000ApJ...544..550A Altcode: We present some results concerning transient brightenings on the quiet Sun, based on data from the Extreme-Ultraviolet Imaging Telescope on board the Solar and Heliospheric Observatory. Histograms of intensity are found to be well fitted by χ2 distributions for small values of the intensity, while at high intensities power-law distributions are always observed. Also, the emission presents the same statistical properties when the resolution is downgraded by local averaging; i.e., it appears to be self-similar down to the resolution scale of the instruments. These properties are characteristic of the emission from a forced turbulent system whose dissipation scale is much smaller than the pixel dimension. On the basis of the data presented as well as other published results and our present theoretical understanding of MHD turbulence, we discuss the realism of the nanoflare scenario of coronal heating. Title: Observational Signatures of Microscale Heating Authors: Bocchialini, K.; Aletti, V.; Vial, J. -C.; Lemaire, P. Bibcode: 1999ESASP.448..539B Altcode: 1999ESPM....9..539B; 1999mfsp.conf..539B No abstract at ADS Title: Eclipse of August 11, 1999: White-light Images and Simultaneous EIT/SOHO Observations Authors: Adjabshirizadeh, A.; Baudin, F.; Bocchialini, K.; Delaboudinière, J. -P.; Grorod, P. -A.; Koutchmy, S.; Laal Aaly, M.; Lamy, P.; Lochard, J.; Mouette, J. Bibcode: 1999ESASP.448.1283A Altcode: 1999ESPM....9.1283A; 1999mfsp.conf.1283A No abstract at ADS Title: Research Of Micro-Scale Coronal Heating Signatures Authors: Aletti, V.; Bocchialini, K. Bibcode: 1999ESASP.446..113A Altcode: 1999soho....8..113A Bright points, small and short lifetime structures, appear permanentely in the solar atmopsphere and could be consideres as intermittent energetic burst. They could be the result of the superpositioon of non-observable small scales events, characterized by an intensity distribution that follows a powerlaw, as obtained in SOC and MHD models. Several brights points are indentifiable in the quiet Sun observed by EIT/SoHO. We have performed a statistical analysis in those brights points in order to determine the index of the power law and to compare this index with the models's one. Title: Long-Term Evolution Of Emissivity And Heating In A Solar Active Region Authors: van Driel-Gesztelyi, L.; Thompson, B.; Démoulin, P.; Orlando, S.; Bocchialini, K.; Oláh, K.; Kövári, Z.; Deforest, C.; Khan, J.; Fludra, A.; Mandrini, C. Bibcode: 1999ESASP.446..663V Altcode: 1999soho....8..663V We study the evolution of the heating and emissivity of an active region from its birth throughout its decay during six solar rotations (July-Nov. 1996). We analyse multi-wavelength and multi-instrument data obtained from SOHO (EIT, SUMER, CDS, MDI), Yohkoh (SXT), GOES and 10.7cm radio data from DRAO, Canada. We take one "snapshot" per rotation at the time of the central meridian passage (CMP) of the AR, outside of time of flares, which appears to be representative enough to allow us to make some general conclusions about the long-term evolution. Deriving physical parameters like intensity (flux), temperature and emission measure of the entire AR vs. time, we formulate mathematically the change in radiation emitted by the decaying AR at several wavelengths. Combining the emissivity data with the evolution of magnetic flux density as the flux is being dispersed by small- and larger-scale convective motions, we make an attempt to understand the physics behind the emission and heating. We also analyse the effects of flaring on the heating of the AR, and study whether and how the flare properties evolve during the life of the active region. Title: Plasma Diagnostics Of A Solar Prominence Observed On 12 June 1997 by EIT, Sumer And CDS Authors: Madjarska, M. S.; Vial, J. -C.; Bocchialini, K.; Dermendjiev, V. N. Bibcode: 1999ESASP.446..467M Altcode: 1999soho....8..467M The plasma diagnostics of a quiescent prominence observed on June 12, 1997 with SUMER, CDS and EIT instruments aboard SOHO in the frame of Joint Observing Programme 9 has been made. Two sets of SUMER observations were taken in the four spectral lines Si IV 1393.755, 1402.770 (6-8 104 K) and O IV 1401.156, 1404.812 (1.7-2.0 105 K) at two different slit positions on the prominence body. The relative line-of-sight velocities using both Si IV 1393.755 and 1402.770 lines are derived. The electron density (derived from the intensity ratio of O IV 1401.156 to 1404.812 lines) in the prominence-corona interface is determined for both slit positions. CDS obtained 10 rasters in Si X 347.40, He I 584.33, Si X 356.04, Fe XVI 360.76, Mg IX 368.06, O V 629.73 lines covering a temperature range from 104 to 106 K. By analysing the CDS spectra in He I and O V ions the relative line-of-sight velocity maps with regards to the quiet sun are derived. Title: Simultaneous LASCO/1998-Eclipse Observations Of A Large-Scale Polar Event Authors: Zhukov, A.; Koutchmy, S.; Lamy, Ph.; Delaboudinière, J. -P.; Delannée, C.; Bocchialini, K.; Guisard, S.; Filippov, B.; Veselovsky, I. Bibcode: 1999ESASP.446..731Z Altcode: 1999soho....8..731Z A relatively faint but large scale polar region event was observed in Aug. 1996 by Boulade et al. 1998 (SoHO SP 404, 217); we first reconsider this event which has been related to a high latitude filament disappearance. We continue the study of this class of events by analyzing the large scale restructuring which occurred above the N-Pole region at the time of the last Feb. 26, 1998 total solar eclipse. Well calibrated WL-eclipse images are used to provide the absolute values of electron densities of the quasi-radial structure appearing at the feet of the event. This structure can also be considered as a type of abnormally broad and curved polar plume, a type of activity already reported in the literature. Unfortunately, the examination of sequences of EIT images taken at that time seems to indicate that the roots of the structure are on the back side of the Sun. However the most impressive effects are seen in the high polar region, at several radii, based on the analysis of processed Lasco-C2 difference images. Large proper motions are deduced over density structures. Both these events confirm that polar regions are indeed showing a new class of CME activity (possibly related to the Hewish's CMEs), which is seen inside coronal holes. A whole set of interesting questions is then appearing to understand the occurrence of a polar CME propagating in the heart of a large unipolar magnetic region of the corona. Title: Propagating Magneto-Acoustic Waves in the Network Authors: Baudin, F.; Bocchialini, K.; Koutchmy, S. Bibcode: 1999ASPC..184..232B Altcode: The analysis of spectroscopic data taken in the chromospheric network is interpreted as evidence for propagating waves. These waves are seen from the photospheric level propagating upward to the highest levels of the chromosphere at velocities around 40 km/s, suggesting a magneto-acoustic nature. We note the lack of an adequate one-dimensional model of the solar chromosphere to interpret these data. Title: Multiresolution wavelet analysis of SUMER/SOHO observations in a solar prominence Authors: Blanco, S.; Bocchialini, K.; Costa, A.; Domenech, G.; Rovira, M.; Vial, J. -C. Bibcode: 1999SoPh..186..281B Altcode: We have studied through a multiresolution wavelet analysis the oscillations in a limb prominence. Intensity fluctuations in time and height corresponding to different lines of Si iv and O iv observed with SUMER on board SOHO have been analyzed in the wavelet bands of J3= 1 min 36 s to 3 min 12 s and J4=3 min 12 s to 6 min 24 s. For all species, oscillations in the J4 band were dominant. We found relevant differences between the behavior of line D1 (1393.76 Å) corresponding to Si iv and the set D2 (1401.16 Å), D3 (1404.81 Å), D4 (1402.77 Å) corresponding to O iv, O iv and Si iv respectively. We also report the identification of a pulse in the intensity of the line D1 that appears in the range of 15-20 min. This disturbance seems to travel with a speed of about 170 km s−1. Title: Oscillations of the upper chromosphere Authors: Gouttebroze, P.; Vial, J. -C.; Bocchialini, K.; Lemaire, P.; Leibacher, J. W. Bibcode: 1999SoPh..184..253G Altcode: Variations of intensity and wavelength in several UV lines have been observed with the SUMER spectroheliometer onboard SOHO, and they have been analysed to obtain oscillation spectra and phase differences between lines of different ions. Lines intensities of neutral or singly ionized atoms (with temperature of formation ≤ 30 000 K) exhibit an increase of oscillatory power between 2.5 and 7 mHz, which may be considered as the signature of p modes. Lines of highly ionized elements (with a temperature of formation ≥ 50 000 K) yield power spectra which are continuously decreasing with frequency. Brightness variations of the continuum at different wavelengths between 1000 and 1400 Å present oscillations in the same frequency range. Thus, p modes seem to be efficiently stopped by the transition region. No clear evidence is found for the existence of a chromospheric oscillation mode. Phase comparisons between lines formed at different altitudes (in particular Si i and Si ii) indicate that these lines oscillate in phase, within the precision of the measurements. Title: Dinámica y frecuencias características de una protuberancia solar observada con los instrumentos SUMER y CDS/SOHO Authors: Rovira, M.; Costa, A.; Bocchialini, K. Bibcode: 1999BAAA...43...22R Altcode: La estructura de la protuberancia estudiada puede dividirse en cuatro regiones. A partir del análisis de las imágenes del CDS y los espectros del SUMER utilizando técnicas de multiresolución con Wavelets se obtuvieron las frecuencias y velocidades relativas de cada una de las regiones. Se observan frecuencias características del orden de los 5 min y otras de largo período. Se obtuvo una fuerte anticorrelación entre las intensidades y las velocidades Doppler. La presencia de las oscilaciones de 5 min en todas las regiones sugieren el acoplamiento entre la estructura cromosférica y la protuberancia. Title: Solar chromospheric structures observed in UV ressonance lines : a multivariate analysis approach Authors: Patsourakos, S.; Bocchialini, K.; Vial, J. -C. Bibcode: 1999CR2...322..337P Altcode: We present the results of a statistical analysis carried out from a data base of 6 solar chromospheric emission lines recorded simultaneously and with high spectral resolution. An empirical and a clustering method for separating the different solar structures contributions have been used and been found in a good agreement. Mean profiles corresponding to the different populations have been built. Correlations of different parameters for each profile allowed us to deduce different properties of the solar chromosphere, such as the existence of magnetic canopies and downflows in active regions. Title: Search for Signatures of a Coronal Hole in Transition Region Lines Near Disk Center Authors: Lemaire, P.; Bocchialini, K.; Aletti, V.; Hassler, D.; Wilhelm, K. Bibcode: 1999SSRv...87..249L Altcode: The analysis of data taken by SUMER near disk center, where a small coronal hole is observed in EIT images, is performed. From the measurements of Doppler non-thermal velocities and intensities, we search for the diagnostics and the signature of small scale structures in the coronal hole using transition region lines. Transition region lines in the range of 7 × 104 K to 2.5 × 105 K have a non-thermal velocity excess of 4.0 to 5.5 km s-1 relative to the contiguous quiet Sun. While the average intensity is lower in the coronal hole than in the quiet area, this result shows an increase of turbulence at the base of the high speed solar wind. Title: Solar chromospheric structures observed in UV resonance lines: a multivariate analysis approach. Authors: Patsourakos, S.; Bocchialini, K.; Vial, J. -C. Bibcode: 1998CRASB.326..337P Altcode: The authors present the results of a statistical analysis carried out from a data base of six solar chromospheric emission lines recorded simultaneously and with high spectral resolution. An empirical and a clustering method for separating the different solar structure contributions have been used and found to be in good agreement. Mean profiles corresponding to the different populations have been built. Correlations of different parameters for each profile allowed one to deduce different properties of the solar chromosphere, such as the existence of magnetic canopies and downflows in active regions. Title: Statistical analysis of solar bright points observed with the SOHO spacecraft. Authors: Régnier, S.; Bocchialini, K.; Vial, J. -C.; Delaboudinière, J. -P.; Thompson, W. Bibcode: 1998CRASB.326..211R Altcode: 1998CR2...326..211R Bright points, small and short lifetime structures, appear permanently in the atmosphere and could be associated with magnetic reconnections, potential sources of coronal heating. Such structures have been observed with the coronal instruments on-board SOHO and a statistical analysis was carried out in order to find the signature of very small scale structures. Title: About polar ejection events and surges Authors: Loucif, M. L.; Koutchmy, S.; Stellmacher, G.; Georgakilas, A.; Bocchialini, K.; Delaboudinière, J. -P. Bibcode: 1998ESASP.421..299L Altcode: 1998sjcp.conf..299L No abstract at ADS Title: Wave Activity and Prominence Eruption Authors: Baudin, F.; Bocchialini, K.; Delannee, C.; Koutchmy, S.; Stellmacher, G.; Shibata, K.; Veselovsky, I. S.; Panasenko, O. A.; Zhukov, A. N. Bibcode: 1998ASPC..150..314B Altcode: 1998IAUCo.167..314B; 1998npsp.conf..314B No abstract at ADS Title: EUV and Microwave Observations of a Filament Authors: Chiuderi-Drago, F.; Bocchialini, K.; Lamartinie, S.; Vial, J. -C.; Bastian, T.; Alissandrakis, C. E.; Harrison, R.; Delaboudiniere, J. -P.; Lemaire, P. Bibcode: 1998ASPC..150...55C Altcode: 1998IAUCo.167...55C; 1998npsp.conf...55C No abstract at ADS Title: Quiescent filament diagnostic. Authors: Lamartinie, S.; Bocchialini, K.; Vial, J. -C.; Chiuderi-Drago, F.; Harrison, R.; Alissandrakis, C. E. Bibcode: 1998joso.proc..139L Altcode: UV observations of a quiescent filament were performed on July 28, 1996 by SUMER and CDS, two spectrometers onboard SOHO. Title: White-light polar plumes from solar eclipses Authors: Koutchmy, S.; Bocchialini, K. Bibcode: 1998ESASP.421...51K Altcode: 1998sjcp.conf...51K No abstract at ADS Title: Space solar physics : theoretical and observational issues in the context of the SOHO mission Authors: Vial, Jean Claude; Bocchialini, Karine; Boumier, Patrick Bibcode: 1998LNP...507.....V Altcode: 1998sspt.conf.....V No abstract at ADS Title: Eclipse WL polar plumes: what is the connection with the disk activity? Authors: Koutchmy, Serge; Bocchialini, Karine Bibcode: 1997AIPC..385..137K Altcode: 1997recs.conf..137K We discuss both the origin and the role that eclipse WL-polar plumes could have in the context of the coronal hole physics: densities, temperatures and flows. Some new results coming from the campaigns of the 1994 and 95 eclipses are reported and YOHKOH data are also taken into account. Title: Statistical Analysis of a Bright Point Observed Simultaneously in Two Chromospheric and Transition Region Lines by SUMER Authors: Bocchialini, K.; Vial, J. -C.; Einaudi, G. Bibcode: 1997ESASP.404..211B Altcode: 1997cswn.conf..211B No abstract at ADS Title: Low Transition-Region Characteristics of Equatorial Coronal Holes Authors: Patsourakos, S.; Bocchialini, K.; Vial, J. -C. Bibcode: 1997ESASP.404..577P Altcode: 1997cswn.conf..577P No abstract at ADS Title: Diagnostic and observations of quiescent and Authors: Vial, J. -C.; Gontikakis, C.; Bocchialini, K.; Gouttebroze, P. Bibcode: 1997IAUJD..19E..55V Altcode: We present a new diagnostic tool for investigating the plasma conditions in a moving structure in the solar corona, such as an eruptive filament or prominence. It relies on NLTE radiative transfer calculations and the signatures of outward directed velocities on Lyman and Balmer lines profiles. Preliminary observations with SUMER on SOHO are discussed. Title: Microwave and UV observations of filaments with SOHO and the VLA Authors: Alissandrakis, C. E.; Drago, F.; Bastian, T.; Bocchialini, K.; Delaboudiniere, J. -P.; Lemaire, P.; Vial, J. -C.; Harrison, R. A.; Thompson, B. Bibcode: 1997ASPC..118..289A Altcode: 1997fasp.conf..289A Observations performed in coordination between SOHO instruments and ground-based observatories offer the unique possibility to derive information simultaneously in several wavelengths formed at different altitudes and/or temperatures in the solar atmosphere. The SUMER and CDS spectrometers, the imaging telescope EIT aboard SOHO, and the VLA provide complementary information in the UV and the radio ranges. We illustrate such a coordination with observations of filaments in the transition region, performed in July 1996. The observations in the UV between 10(4) and 10(6) K provide the differential emission measure as a function of temperature; this can be used to compute the expected brightness temperature in the microwave range and check models of the filament-corona transition region. Title: First Results of SOHO's Joint Observing Programme 40 Authors: Patsourakos, S.; Bocchialini, K.; Vial, J. -C. Bibcode: 1997IAUJD..19E..38P Altcode: The first results of SOHO's JOP 40 are presented. This program proposes to study the chromospheric to transition region of equatorial coronal holes in order to derive parameters such as the temperature, the density, using different lines formed at different altitudes, in different places: the boundary of a coronal hole or the central region, on the disk. The two components of the chromospheric quiet Sun, network and internetwork, should be observed, in and out of an equatorial coronal hole. Title: High frequency magneto-acoustic waves in the chromosphere Authors: Bocchialini, Karine; Koutchmy, Serge Bibcode: 1997AIPC..385..153B Altcode: 1997recs.conf..153B From a time series taken over the disk center network and cell elements in different chromospheric and photospheric lines, we discuss the possible detection of wave-trains corresponding to frequencies higher than the 7 mHz frequency of the familiar chromospheric 3 mn oscillations. Their analysis would greatly benefit from observations taken with an improved spatial resolution, free of seeing effects which limit the precision in ground-based measurements. Title: Propagating magneto-acoustic waves in the solar chromosphere. Authors: Baudin, F.; Bocchialini, K.; Koutchmy, S. Bibcode: 1996A&A...314L...9B Altcode: We report on spectroscopic one dimensional observations showing for the first time upward propagating 5mn period waves, which emerge from the deep chromospheric network. Wavetrains are well measured at the height where the He I line (at A=1083nm) is formed by the coronal back radiation. We also present results from a time series of narrow filtergrams of a quiet region at the disk center. The two dimensional mapping of the power of waves observed in the chrormosphere shows the familiar cell-like distribution corresponding to the network magnetic field pattern. In addition, Fourier components with significantly longer periods than 5mn were detected in the chromospheric network. We suggest that the waves propagating in the open corona are reminescent of photospheric oscillations transmitted by the magnetic field of the chromospheric network. Title: High-Chromosphere and Low-Transition-Region Network: a Different Organization in an Equatorial Coronal Hole? Authors: Bocchialini, K.; Vial, J. -C. Bibcode: 1996SoPh..168...37B Altcode: In order to investigate the high chromosphere and the low transition region in a coronal hole, we have analysed Ca II, Mg II and hydrogen resonance lines, recorded by the OSO-8 spectrometer in 1975. We present the comparison between average profiles observed in and out of the equatorial coronal hole which was at the center of the solar disk between 27 and 29 November, 1975. We separate internetwork and quiet-Sun (network+internetwork) profiles: for the internetwork, we observe that the hydrogen and Mg II profiles recorded in the hole are stronger than the profiles recorded out of the hole; a similar result, but with a much lower contrast, is found for the quiet Sun. We discuss this surprising result. Title: Solar chromospheric structures as observed simultaneously in strong UV lines. II. Network and cell modelling. Authors: Bocchialini, K.; Gouttebroze, P. Bibcode: 1996A&A...313..949B Altcode: Mean line profiles of the quiet Sun spectrum, recorded simultaneously in Lα, Lβ, Ca II H and K, and Mg II h and k lines with the OSO-8/LPSP spectrometer were derived for structures such as supergranulation cell and network. We compare these observed profiles with theoretical ones computed by Vernazza et al. (1981, VAL81) and by Fontenla et al. (1993, FAL93). We also present our own theoretical profiles : with our non-LTE radiative transfer codes, we compute the line profiles corresponding to different atmospheric models, derived from the reference VAL and FAL models. Finally, we propose two new semi-empirical models, NET and CEL, which are in better agreement with the network and cell line profiles observed by OSO-8. Title: VizieR Online Data Catalog: Solar chromospheric structures. II. (Bocchialini+, 1996) Authors: Bocchialini, K.; Gouttebroze, P. Bibcode: 1996yCat..33130949B Altcode: Mean line profiles of the quiet Sun spectrum, recorded simultaneously in Lα, Lβ, Ca II H and K, and Mg II h and k lines with the OSO-8/LPSP spectrometer were derived for structures such as supergranulation cell and network. We compare these observed profiles with theoretical ones computed by Vernazza et al. (1981, VAL81) and by Fontenla et al. (1993, FAL93). We also present our own theoretical profiles : with our non-LTE radiative transfer codes, we compute the line profiles corresponding to different atmospheric models, derived from the reference VAL and FAL models. Finally, we propose two new semi-empirical models, NET and CEL, which are in better agreement with the network and cell line profiles observed by OSO-8. (2 data files). Title: Analyse de raies de la chromosphère solaire: diagnostic et dynamique. Authors: Bocchialini, K. Bibcode: 1995JAF....49Q..52B Altcode: No abstract at ADS Title: Wavelet analysis of chromospheric solar oscillations. Authors: Bocchialini, K.; Baudin, F. Bibcode: 1995A&A...299..893B Altcode: We obtain new information on chromospheric oscillations from the application of wavelet analysis to observations of the quiet Sun in He I and Ca II lines. Using this analysing technique the temporal behaviour of oscillations at different frequencies is illustrated in two regions: a magnetic element network and a non magnetic intra-network cell. The results presented below show the duration of the chromospheric wavetrains and the correlation between the two lines, and also include a study of the lags between the signals. Title: Chromospheric Oscillations from Simultaneous Sequences of HEL 1083 and Call K 393.4 Spectroscopic Measurements Authors: Bocchialini, K.; Koutchmy, S. Bibcode: 1995ESASP.376b.499B Altcode: 1995help.confP.499B; 1995soho....2..499B No abstract at ADS Title: Wave Properties of the Chromosphere in He I 1083 nm and CA II K Authors: Bocchialini, K.; Baudin, F.; Koutchmy, S. Bibcode: 1995itsa.conf..423B Altcode: No abstract at ADS Title: Solar chromospheric structures as observed simultaneously in strong UV lines I. Observations, statistical analysis and characteristic line profiles. Authors: Bocchialini, K.; Vial, J. -C. Bibcode: 1994A&A...287..233B Altcode: We present a set of high resolution profiles of H Lyman α and β, Mg II h and k, Ca II H and K lines measured near the center of the solar disk and simultaneously above different solar chromospheric structures. The large data base provides a way of correlating different parameters in the different lines: correlations such as Lα reversal vs intensity, Lα vs Ca K are discussed. We notice that Mg II and Ca II have a similar behaviour, different from Lα and β. We also discuss a classification derived from the distribution of integrated intensities in Ca II K, from which average profiles (for cell, network, plage) are computed for the six lines and are compared with theoretical ones derived from several models. Title: Dynamical Properties of the Chromosphere In and Out of the Solar Magnetic Network Authors: Bocchialini, Karine; Vial, Jean-Claude; Koutchmy, Serge Bibcode: 1994ApJ...423L..67B Altcode: We present the results of a comparative analysis of an 83 minute time sequence of spectra taken around the Ca II and He I 1083 lines, near the center of the solar disk and away from active regions. We discuss the behavior of the Fourier spectra at low frequency: 3 minute oscillations are well observed out of the network, and 5 minute oscillation waves are prominent in the network. The 5 s sampling time also permits the observation of the high-frequency part of the Fourier spectra of intensity and velocity fluctuations at different heights. At high frequencies, K2V-K2R and 1083 (velocity) results differ when magnetic and non-magnetic regions are compared. Title: Wave Properties in the Upper Chromosphere and at the Base of the Corona Authors: Bocchialini, K.; Vial, J. -C.; Koutchmy, S. Bibcode: 1994scs..conf..123B Altcode: 1994IAUCo.144..123B From a 83 min long sequence of observations of Ca II K and He I (1083 nm) line profiles, some dynamical properties of the main components of the quiet upper chromosphere are derived: for both the magnetic network and the internetwork, amplitude and phase spectra of the Doppler velocities are presented. Title: Analysis of Chromospheric Proxies of Coronal Bright Points Authors: Bocchialini, K.; Vial, J. -C.; Koutchmy, S.; Zirker, J. B. Bibcode: 1994ASPC...68..389B Altcode: 1994sare.conf..389B No abstract at ADS Title: Observed Chromospheric Profiles Compared with Theoretical Ones Authors: Bocchialini, K.; Gouttebroze, P.; Vial, J. -C. Bibcode: 1994emsp.conf...49B Altcode: No abstract at ADS Title: Analysis of the Chromospheric Proxies of Coronal Bright Points - Preliminary Results Authors: Bocchialini, K.; Koutchmy, S.; Vial, J. -C.; Zirker, J. B. Bibcode: 1994emsp.conf..173B Altcode: No abstract at ADS Title: Quiet and active solar structures as observed at the bottom of the transition region. Authors: Bocchialini, K.; Vial, Jean-Claude Bibcode: 1992ESASP.348..197B Altcode: 1992cscl.work..197B The authors present a set of high resolution profiles of H Lyman α and β, Mg II h and k, Ca II H and K lines measured simultaneously above different solar structures. The large data base provides a way of correlating different parameters in the different lines: Lα reversal vs intensity, Lα vs Ca K, etc... The authors notice that Mg II and Ca II have a similar behaviour, different from Lα and β ones. They also discuss two classifications derived from the distribution of intensities, from which average (cell, network, plage, sunspot) profiles are computed for the 6 lines. They compare the Ca K results with the two-dimensional models of Solanki et al. (1991).