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1. Crossbar Arrays based on 'Wall' Phase-Change Memory (PCM) and Ovonic- Threshold Switching (OTS) Selector: a Device Integration Challenge Towards New Computing Paradigms in Embedded Applications

Author: Bourgeois, G., Meli, V., Antonelli, R., Socquet-Clerc, C., Magis, T., Laulagnet, F., Hemard, B., Bernard, M., Fellouh, L., Dezest, P., Krawczyk, J., Dominguez, S., Baudin, F., Garrione, J., Pellissier, C., Dallery, J.-A., Castellani, N., Cyrille, M.-C., Charpin, C., Andrieu, F., Navarro, G., Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), IEEE, and European Project: 101007321,StorAlge
Subjects: "Wall" PCM, Crossbar, OTS selector), [SPI.MAT]Engineering Sciences [physics]/Materials
Abstract: International audience; In this work, we demonstrate the integration feasibility of Crossbar arrays based on Ovonic-Threshold Switching (OTS) selector and "Wall"-based Phase-Change Memory, realized with a "Double-Patterned Self-Aligned" (DPSA) structure in the Back-End-of-Line (BEOL) of the CMOS fabrication. We fabricated devices with critical dimensions down to 60 nm×80 nm, integrating materials providing improved thermal stability (against BEOL thermal budget). Preliminary statistical electrical tests performed in 1 kb 1T1S1R arrays confirm the devices correct programming and cycling operations. These results pave the way to the integration of Crossbar arrays in embedded applications.
Published: 2023

2. Planned Peri-Extubation Fasting in Critically Ill Children: An International Survey of Practice

Author: Nabialek, T, Tume, LN, Cercueil, E, Morice, C, Bouvet, L, Baudin, F, and Valla, FV
Subjects: Pediatrics, Perinatology and Child Health
Abstract: IntroductionCumulative energy/protein deficit is associated with impaired outcomes in pediatric intensive care Units (PICU). Enteral nutrition is the preferred mode, but its delivery may be compromised by periods of feeding interruptions around procedures, with peri-extubation fasting the most common procedure. Currently, there is no evidence to guide the duration of the peri-extubation fasting in PICU. Therefore, we aimed to explore current PICU fasting practices around the time of extubation and the rationales supporting them.Materials and MethodsA cross sectional electronic survey was disseminated via the European Pediatric Intensive Care Society (ESPNIC) membership. Experienced senior nurses, dieticians or doctors were invited to complete the survey on behalf of their unit, and to describe their practice on PICU fasting prior to and after extubation.ResultsWe received responses from 122 PICUs internationally, mostly from Europe. The survey confirmed that fasting practices are often extrapolated from guidelines for fasting prior to elective anesthesia. However, there were striking differences in the duration of fasting times, with some units not fasting at all (in patients considered to be low risk), while others withheld feeding for all patients. Fasting following extubation also showed large variations in practice: 46 (38%) and 26 (21%) of PICUs withheld oral and gastric/jejunal nutrition more than 5 h, respectively, and 45 (37%) started oral feeding based on child demand. The risk of vomiting/aspiration and reducing nutritional deficit were the main reasons for fasting children [78 (64%)] or reducing fasting times [57 (47%)] respectively.DiscussionThis variability in practices suggests that shorter fasting times might be safe. Shortening the duration of unnecessary fasting, as well as accelerating the extubation process could potentially be achieved by using other methods of assessing gastric emptiness, such as gastric point of care ultrasonography (POCUS). Yet only half of the units were aware of this technique, and very few used it.
Published: 2022

3. Mechanism of riboregulation of p62 protein oligomerisation by vault RNA1-1 in selective autophagy

Author: Janosch Hennig, Buescher M, Rastislav Horos, Dobrev N, Matthias W. Hentze, Kevin Haubrich, and Baudin F
Subjects: Chemistry, Vesicle, Organelle, Autophagy, RNA, Linker, Function (biology), Vault (organelle), Intracellular, Cell biology
Abstract: Macroautophagy ensures the clearance of intracellular substrates ranging from single ubiquitinated proteins to large proteotoxic aggregates and defective organelles. The selective autophagy receptor p62 binds these targets and recruits them to double-membrane vesicles, which fuse with lysosomes to degrade their content. We recently uncovered that p62 function is riboregulated by the small non-coding vault RNA1-1. Here, we present detailed insight into the underlying mechanism. We show that the PB1 domain and adjacent linker region of p62 (aa 1-122) are necessary and sufficient for specific vault RNA1-1 binding, and identify lysine 7 and arginine 21 as key hinges for p62 riboregulation. Chemical structure probing of vault RNA1-1 further reveals a central flexible loop within the RNA that mediates the specific p62 interaction. Our data define molecular determinants that govern mammalian autophagy via the p62-vault RNA1-1 riboregulatory pair.
Published: 2021

4. The Flare Likelihood and Region Eruption Forecasting (FLARECAST) Project: Flare forecasting in the big data & machine learning era

Author: Georgoulis, M. K., Bloomfield, D. S., Piana, M., Massone, A. M., Soldati, M., Gallagher, P. T., Pariat, E., Vilmer, N., Buchlin, E., Baudin, F., Csillaghy, A., Sathiapal, H., Jackson, D. R., Alingery, P., Benvenuto, F., Campi, C., Florios, K., Gontikakis, C., Guennou, C., Guerra, J. A., Kontogiannis, I., Latorre, V., Murray, S. A., Park, S. -H., von Stachelski, S., Torbica, A., Vischi, D., and Worsfold, M.
Subjects: FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: The EU funded the FLARECAST project, that ran from Jan 2015 until Feb 2018. FLARECAST had a R2O focus, and introduced several innovations into the discipline of solar flare forecasting. FLARECAST innovations were: first, the treatment of hundreds of physical properties viewed as promising flare predictors on equal footing, extending multiple previous works; second, the use of fourteen (14) different ML techniques, also on equal footing, to optimize the immense Big Data parameter space created by these many predictors; third, the establishment of a robust, three-pronged communication effort oriented toward policy makers, space-weather stakeholders and the wider public. FLARECAST pledged to make all its data, codes and infrastructure openly available worldwide. The combined use of 170+ properties (a total of 209 predictors are now available) in multiple ML algorithms, some of which were designed exclusively for the project, gave rise to changing sets of best-performing predictors for the forecasting of different flaring levels. At the same time, FLARECAST reaffirmed the importance of rigorous training and testing practices to avoid overly optimistic pre-operational prediction performance. In addition, the project has (a) tested new and revisited physically intuitive flare predictors and (b) provided meaningful clues toward the transition from flares to eruptive flares, namely, events associated with coronal mass ejections (CMEs). These leads, along with the FLARECAST data, algorithms and infrastructure, could help facilitate integrated space-weather forecasting efforts that take steps to avoid effort duplication. In spite of being one of the most intensive and systematic flare forecasting efforts to-date, FLARECAST has not managed to convincingly lift the barrier of stochasticity in solar flare occurrence and forecasting: solar flare prediction thus remains inherently probabilistic., 67 pages, 14 figures; submitted
Published: 2021
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5. Locally variable responses to a global carbon-cycle disturbance: environmental perturbations during the Frasnian–Famennian mass extinction

Author: Percival, Lawrence, Marynowski, Leszek, Baudin, F., Goderis, Steven, De Vleeschouwer, David, Rakociński, Michal, Narkiewicz, Kataryna, Da Silva, Anne-Christine, Claeys, Philippe, Analytical, Environmental & Geo-Chemistry, and Chemistry
Published: 2021

6. The Solar Orbiter SPICE instrument

Author: Anderson, M., Appourchaux, T., Auchère, F., Aznar Cuadrado, R., Barbay, J., Baudin, F., Beardsley, S., Bocchialini, K., Borgo, B., Bruzzi, D., Buchlin, Eric, Burton, G., Büchel, V., Caldwell, M., Caminade, S., Carlsson, M., Curdt, W., Davenne, J., Davila, J., DeForest, C., 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., Haugan, S., Howe, C., Janvier, M., Klein, R., Koller, S., Kucera, T., Kouliche, D., Marsch, E., Marshall, A., Marshall, G., Matthews, S., 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., 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., Institut d'astrophysique spatiale (IAS), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; Aims. The Spectral Imaging of the Coronal Environment (SPICE) instrument is a high-resolution imaging spectrometer operating at extreme ultraviolet (EUV) 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.
Published: 2020

7. Groupe de Travail Soleil Heliosphere-Magnetospheres (SHM)

Author: Auchère, F., Astafyeva, E., Baudin, F., Briand, C., Brun, S., Célestin, Sebastien, Génot, V., Kretzschmar, Matthieu, Leblanc, François, Rouillard, A., Sahraoui, F., Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and CNES - Centre national d'études spatiales
Subjects: [SDU]Sciences of the Universe [physics]
Abstract: Les grandes questions scientifiques abordées dans le cadre de la thématique Soleil Héliosphère et Magnétosphères (SHM) couvrent l'ensemble des problématiques liées aux relations entre notre étoile et le système solaire. Cela commence par l'étude de la structure interne du Soleil à travers l'observation multi-spectrales, l'hélio-sismologie et la modélisation ; par l'étude de l'origine de la couronne solaire, son chauffage et l'accélération du vent solaire et des particules énergétiques solaires lors d'événements énergétiques solaires ; et enfin par l'étude de la propagation du vent solaire et des mécanismes de chauffage de celui-ci par dissipation turbulente.
Published: 2019

8. Monsoon control on channel avulsions in the Late Quaternary Congo Fan

Author: Picot, M., Marsset, T., Droz, L., Dennielou, B., Baudin, F., Hermoso, M., de Rafélis, M., Sionneau, T., Cremer, M., Laurent, D., Bez, M., Laboratoire Géosciences Océan (LGO), Institut Français de Recherche pour l'Exploitation de la Mer - Brest (IFREMER Centre de Bretagne), Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Bretagne Sud (UBS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Earth Sciences [Oxford], University of Oxford [Oxford], Géosciences Environnement Toulouse (GET), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Max-Planck-Institut für Extraterrestrische Physik (MPE), TOTAL-Scientific and Technical Center Jean Féger (CSTJF), TOTAL FINA ELF, ISBlue - Interdisciplinary Graduate School for the Blue planet (2017), ANR-17-EURE-0015,ISBlue,Interdisciplinary Graduate School for the Blue planet(2017), Université de Bretagne Sud (UBS)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), University of Oxford, Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Centre scientifique et Technique Jean Feger (CSTJF)
Subjects: [SDU.STU.TE]Sciences of the Universe [physics]/Earth Sciences/Tectonics, [SDU.STU.VO]Sciences of the Universe [physics]/Earth Sciences/Volcanology, [SDU.STU.PG]Sciences of the Universe [physics]/Earth Sciences/Paleontology, ComputingMilieux_MISCELLANEOUS, [SDU.STU.OC]Sciences of the Universe [physics]/Earth Sciences/Oceanography
Abstract: International audience
Published: 2019

9. Acute endophthalmitis after intravitreal injections of corticosteroids or anti-vascular growth factor agents. A nationwide study in France from 2012 to 2015

Author: BAUDIN, F., BENZENINE, E., MARIET, A. S., BRON, A., DAIEN, V., KOROBELNIK, Jean-Francois, QUANTIN, C., and CREUZOT-GARCHER, C.
Published: 2018

10. PLATO as it is: A legacy mission for Galactic archaeology

Author: Miglio, A, Chiappini, C, Mosser, B, Davies, GR, Freeman, K, Girardi, L, Jofré, P, Kawata, D, Rendle, BM, Valentini, M, Casagrande, L, Chaplin, WJ, Gilmore, G, Hawkins, K, Holl, B, Appourchaux, T, Belkacem, K, Bossini, D, Brogaard, K, Goupil, MJ, Montalbán, J, Noels, A, Anders, F, Rodrigues, T, Piotto, G, Pollacco, D, Rauer, H, Prieto, CA, Avelino, PP, Babusiaux, C, Barban, C, Barbuy, B, Basu, S, Baudin, F, Benomar, O, Bienaymé, O, Binney, J, Bland-Hawthorn, J, Bressan, A, Cacciari, C, Campante, TL, Cassisi, S, Christensen-Dalsgaard, J, Combes, F, Creevey, O, Cunha, MS, Jong, RS, Laverny, P, Degl'Innocenti, S, Deheuvels, S, Depagne, Ridder, J, Matteo, PD, Mauro, MPD, Dupret, MA, Eggenberger, P, Elsworth, Y, Famaey, B, Feltzing, S, García, RA, Gerhard, O, Gibson, BK, Gizon, L, Haywood, M, Handberg, R, Heiter, U, Hekker, S, Huber, D, Ibata, R, Katz, D, Kawaler, SD, Kjeldsen, H, Kurtz, DW, Lagarde, N, Lebreton, Y, Lund, MN, Majewski, Marigo, P, Gilmore, Gerard [0000-0003-4632-0213], and Apollo - University of Cambridge Repository
Subjects: galaxy: structure, stars: oscillations – surveys, stars: abundances, stars: fundamental parameters
Abstract: Deciphering the assembly history of the Milky Way is a formidable task, which becomes possible only if one can produce high-resolution chrono-chemo-kinematical maps of the Galaxy. Data from large-scale astrometric and spectroscopic surveys will soon provide us with a well-defined view of the current chemo-kinematical structure of the Milky Way, but it will only enable a blurred view on the temporal sequence that led to the present-day Galaxy. As demonstrated by the (ongoing) exploitation of data from the pioneering photometric missions CoRoT, Kepler, and K2, asteroseismology provides the way forward: solar-like oscillating giants are excellent evolutionary clocks thanks to the availability of seismic constraints on their mass and to the tight age–initial mass relation they adhere to. In this paper we identify five key outstanding questions relating to the formation and evolution of the Milky Way that will need precise and accurate ages for large samples of stars to be addressed, and we identify the requirements in terms of number of targets and the precision on the stellar properties that are needed to tackle such questions. By quantifying the asteroseismic yields expected from PLATO for red giant stars, we demonstrate that these requirements are within the capabilities of the current instrument design, provided that observations are sufficiently long to identify the evolutionary state and allow robust and precise determination of acoustic-mode frequencies. This will allow us to harvest data of sufficient quality to reach a 10% precision in age. This is a fundamental prerequisite to then reach the more ambitious goal of a similar level of accuracy, which will be possible only if we have at hand a careful appraisal of systematic uncertainties on age deriving from our limited understanding of stellar physics, a goal that conveniently falls within the main aims of PLATO's core science. We therefore strongly endorse PLATO's current design and proposed observational strategy, and conclude that PLATO, as it is, will be a legacy mission for Galactic archaeology., International Space Science Institute (ISSI), European Commission's Seventh Framework Programme, DFG, CH1188/2-1. COST (European Cooperation in Science and Technology), ChETEC COST Action, CA16117. The Danish National Research Foundation, DNRF106. UK Science and Technology Facilities Council (STFC), PRIN INAF 2014 – CRA 1.05.01.94.05, European Union FP7 program, ERC, 320360. Australian Research Council, DP150100250; FT160100402. NASA, NNX16AI09G. FCT; UID/FIS/04434/2013; FEDER (COMPETE); IF/00894/2012/; POPH/FSE (EC), CNES, DLR; NYUAD Institute, G1502. “Programme National de Physique Stellaire” (PNPS), “Programme National Cosmologie et Galaxies” (CNRS/INSU, France), CNES Fellowship, Swedish National Space Board (SNSB/Rymdstyrelsen), NASA, NNX16AJ17G. ERC Consolidator (STARKEY), 615604). Belspo (PRODEX PLATO), Australian Research Council Future Fellowship, FT1400147. ESP2015-66134-R (MINECO), VILLUM FONDEN, 10118.
Published: 2017

11. The life of stars and their planets

Author: Catala, C, Aerts, C, Aigrain, S, Antonello, E, Appourchaux, T, Auvergne, M, Baglin, A, Barge, P, Barstow, M, Baudin, F, Boumier, P, Cameron, A, Christensen-Dalsgaard, J, Cutispoto, G, Deeg, H, Deleuil, M, Desidera, S, Donati, J, Favata, F, Foing, B, Gameiro, J, García, R, Garrido, R, Horne, K, and Lanza, A
Abstract: We lack a reliable scenario for the formation and evolution of stars and their planetary systems, involving key factors such as magnetic fields and turbulence. We present the case for a mission concept that will clarify these problems and give us a global view of the evolution of combined star and planetary systems. This will be achieved by simultaneously addressing the search for planetary transits in front of a large number of stars, including many nearby stars, the study of their internal structure and evolution via asteroseismology, and that of their magnetic activity, via UV monitoring.
Published: 2016

12. NORTHWESTERN PACIFIC ATOLLS AND GUYOTS - ODP LEG 143 PRELIMINARY-RESULTS

Author: Baudin, F, Arnaud, H, Sager, W, Winterer, E, Firth, J, Baker, P, Bralower, T, Castillo, P, Cooper, P, Flood, P, Golovchenko, X, Iryu, Y, Ivanov, M, Jenkyns, H, Kenter, J, Murdmaa, I, Mutterlose, J, Nogi, Y, Paull, C, Polgreen, E, Rohl, U, Sliter, W, Strasser, A, Swinburne, N, and Tarduno, J
Published: 2016

13. A calcareous nannofossil and organic geochemical study of marine palaeoenvironmental changes across the Sinemurian/Pliensbachian (early Jurassic, ~191Ma) in Portugal

Author: Plancq, J., Mattioli, E., Pittet, B., Baudin, F., Duarte, L.V., Boussaha, M., and Grossi, V.
Abstract: The Sinemurian/Pliensbachian boundary (~ 191 Ma) is acknowledged as one of the most important steps in the radiation of planktonic organisms, especially primary producers such as dinoflagellates and coccolithophores. To date, there is no detailed study documenting changes in planktonic assemblages related to palaeoceanographic changes across this boundary. The aim of this study is to characterize the palaeoenvironmental changes occurring across the Sinemurian/Pliensbachian boundary at the São Pedro de Moel section (Lusitanian Basin, Portugal) using micropalaeontology and organic geochemistry approaches. Combined calcareous nannofossil assemblage and lipid biomarker data document for a decrease in primary productivity in relation to a major sea-level rise occurring above the boundary. The Lusitanian Basin was particularly restricted during the late Sinemurian with a relatively low sea level, a configuration that led to the recurrent development of black shales. After a sharp sea-level fall, the basin became progressively deeper and more open during the earliest Pliensbachian, subsequently to a major transgression. This sea-level increase seems to have been a global feature and could have been related to the opening of the Hispanic Corridor that connected the Tethys and palaeo-Pacific oceans. The palaeoceanographic and palaeoclimatic changes induced by this opening may have played a role in the diversification of coccolithophores with the first occurrence or colonization of Tethyan waters by placolith-type coccoliths.
Published: 2016

14. Caractérisation sédimentaire de la formation roche mère carbonatée du jurassique supérieur du Quercy

Author: Bastianini, L., Caline, B., Hoareau, Guilhem, Bonnel, Cédric, Lezin, C., Baudin, F., Brasier, A., Guy, L., Centre scientifique et Technique Jean Feger (CSTJF), TOTAL FINA ELF, Laboratoire des Fluides Complexes et leurs Réservoirs (LFCR), TOTAL FINA ELF-Université de Pau et des Pays de l'Adour (UPPA)-Centre National de la Recherche Scientifique (CNRS), Géosciences Environnement Toulouse (GET), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Solvay Silica, and Solvay (France)
Subjects: [PHYS]Physics [physics], [PHYS.MECA.MEMA]Physics [physics]/Mechanics [physics]/Mechanics of materials [physics.class-ph], [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], [SPI.MECA.MEMA]Engineering Sciences [physics]/Mechanics [physics.med-ph]/Mechanics of materials [physics.class-ph], [PHYS.MECA.GEME]Physics [physics]/Mechanics [physics]/Mechanical engineering [physics.class-ph], [SPI.MECA.MEFL]Engineering Sciences [physics]/Mechanics [physics.med-ph]/Fluids mechanics [physics.class-ph]
Abstract: ACT; International audience
Published: 2016

15. CA176 - Intérêt de l’ustékinumab pour le traitement des uvéites antérieures chez une patiente avec un rhumatisme psoriasique

Author: Bielefeld, Philip, Picque, J. B., Devilliers, Hervé, Maupin, E., Baudin, F., Turcu, A., Muller, Géraldine, Bron, Alain, Creuzot Garcher, Catherine, Besancenot, Jean-François, Centre Hospitalier Universitaire de Dijon - Hôpital François Mitterrand (CHU Dijon), Centre des Sciences du Goût et de l'Alimentation (CSGA), and Institut National de la Recherche Agronomique (INRA)-Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDV.MHEP.OS]Life Sciences [q-bio]/Human health and pathology/Sensory Organs, [SDV.MHEP]Life Sciences [q-bio]/Human health and pathology
Abstract: National audience; Introduction Une patiente de 36ans présente un rhumatisme psoriasique depuis 15 ans, assez calme puisque sensible aux anti-inflammatoires non stéroïdiens, avec peu de manifestations cutanées. Observation Les uvéites antérieures récidivantes posent problème chez cette patiente avec au moins 3 épisodes par an, avec extension au pôle postérieur et nécessité d’une corticothérapie orale à chaque poussée. Un traitement de fond par méthotrexate ne prévient pas les récidives. Un traitement par anti-TNF est tenté, tout d’abord des perfusions d’infliximab, qui se soldent dès la troisième par des éruptions cutanées prurigineuses. Un remplacement par adalimumab provoque le même effet secondaire allergique. Il est décidé de changer de classe de biothérapie, par crainte de la récidive de cet effet secondaire avec un autre anti-TNF. L’ustékinumab est introduit à la dose de 45mg selon le schéma classique, avec une excellente tolérance. Aucune récidive d’uvéite n’est survenue au bout d’un an de traitement. Discussion L’ustékinumab est un inhibiteur des interleukines IL-12 et IL-23 agissant contre la sous-unité P40 commune à l’IL-12/23. Si la place de l’ustékinumab dans le traitement du rhumatisme psoriasique demande à être précisée, on sait que l’interleukine-23 intervient dans la pathogénie des uvéites inflammatoires [1]. Conclusion Il n’existe pour le moment pas de protocole d’essai de ce médicament pour les uvéites résistantes aux anti-TNF, ou les patients avec inflammation oculaire sévère intolérants aux anti-TNF. Une évaluation à plus grande échelle serait nécessaire.
Published: 2015

16. Young [$��$/Fe]-enhanced stars discovered by CoRoT and APOGEE: What is their origin?

Author: Chiappini, C., Anders, F., Rodrigues, T. S., Miglio, A., Montalban, J., Mosser, B., Girardi, L., Valentini, M., Noels, A., Morel, T., Minchev, I., Steinmetz, M., Santiago, B. X., Schultheis, M., Martig, M., da Costa, L. N., Maia, M. A. G., Prieto, C. Allende, Peralta, R. de Assis, Hekker, S., Theme��l, N., Kallinger, T., Garcia, R. A., Mathur, S., Baudin, F., Beers, T. C., Cunha, K., Harding, P., Holtzman, J., Majewski, S., Meszaros, Sz., Nidever, D., Pan, K., Schiavon, R. P., Shetrone, M. D., Schneider, D. P., and Stassun, K.
Subjects: Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We report the discovery of a group of apparently young CoRoT red-giant stars exhibiting enhanced [alpha/Fe] abundance ratios (as determined from APOGEE spectra) with respect to Solar values. Their existence is not explained by standard chemical evolution models of the Milky Way, and shows that the chemical-enrichment history of the Galactic disc is more complex. We find similar stars in previously published samples for which isochrone-ages could be robustly obtained, although in smaller relative numbers, which could explain why these stars have not received prior attention. The young [alpha/Fe]-rich stars are much more numerous in the CoRoT-APOGEE (CoRoGEE) inner-field sample than in any other high-resolution sample available at present, as only CoRoGEE can explore the inner-disc regions and provide ages for its field stars. The kinematic properties of the young [$��$/Fe]-rich stars are not clearly thick-disc like, despite their rather large distances from the Galactic mid-plane. Our tentative interpretation of these and previous intriguing observations in the Milky Way is that these stars were formed close to the end of the Galactic bar, near corotation -- a region where gas can be kept inert for longer times, compared to other regions shocked more frequently by the passage of spiral arms. Moreover, that is where the mass return from older inner-disc stellar generations should be maximal (according to an inside-out disc-formation scenario), further diluting the in-situ gas. Other possibilities to explain these observations (e.g., a recent gas-accretion event) are also discussed., Letter in press in Astronomy and Astrophysics (5 pages, 4 figures + 2 pages Appendix)
Published: 2015
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17. Paléoenvironnements et caractérisation des roches mères carbonatées du bassin aquitain

Author: Bastianini, L., Hoareau, Guilhem, Caline, B., Martinez, C., Baudin, F., Guy, L., Bonnel, Cédric, Laboratoire des Fluides Complexes et leurs Réservoirs (LFCR), Centre National de la Recherche Scientifique (CNRS)-Université de Pau et des Pays de l'Adour (UPPA)-TOTAL FINA ELF, Centre scientifique et Technique Jean Feger (CSTJF), TOTAL FINA ELF, Institut d'astrophysique spatiale (IAS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Solvay Silica, and Solvay (France)
Subjects: [PHYS]Physics [physics], [PHYS.MECA.MEMA]Physics [physics]/Mechanics [physics]/Mechanics of materials [physics.class-ph], [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], [SPI.MECA.MEMA]Engineering Sciences [physics]/Mechanics [physics.med-ph]/Mechanics of materials [physics.class-ph], [PHYS.MECA.GEME]Physics [physics]/Mechanics [physics]/Mechanical engineering [physics.class-ph], [SPI.MECA.MEFL]Engineering Sciences [physics]/Mechanics [physics.med-ph]/Fluids mechanics [physics.class-ph]
Abstract: ACT; International audience
Published: 2015

18. The PLATO 2.0 mission

Author: Rauer, H., Catala, C., Aerts, C., Appourchaux, T., Benz, W., Brandeker, A., Christensen-Dalsgaard, J., Deleuil, M., Gizon, L., Goupil, M. -J., G��del, M., Janot-Pacheco, E., Mas-Hesse, M., Pagano, I., Piotto, G., Pollacco, D., Santos, N. C., Smith, A., C., J., Su��rez, Szab��, R., Udry, S., Adibekyan, V., Alibert, Y., Almenara, J. -M., Amaro-Seoane, P., Eiff, M. Ammler-von, Asplund, M., Antonello, E., Ball, W., Barnes, S., Baudin, F., Belkacem, K., Bergemann, M., Bihain, G., Birch, A. C., Bonfils, X., Boisse, I., Bonomo, A. S., Borsa, F., Brand��o, I. M., Brocato, E., Brun, S., Burleigh, M., Burston, R., Cabrera, J., Cassisi, S., Chaplin, W., Charpinet, S., Chiappini, C., Church, R. P., Csizmadia, Sz., Cunha, M., Damasso, M., Davies, M. B., Deeg, H. J., D��az, R. F., Dreizler, S., Dreyer, C., Eggenberger, P., Ehrenreich, D., Eigm��ller, P., Erikson, A., Farmer, R., Feltzing, S., Fialho, F. de Oliveira, Figueira, P., Forveille, T., Fridlund, M., Garc��a, R. A., Giommi, P., Giuffrida, G., Godolt, M., da Silva, J. Gomes, Granzer, T., Grenfell, J. L., Grotsch-Noels, A., G��nther, E., Haswell, C. A., Hatzes, A. P., H��brard, G., Hekker, S., Helled, R., Heng, K., Jenkins, J. M., Johansen, A., Khodachenko, M. L., Kislyakova, K. G., Kley, W., Kolb, U., Krivova, N., Kupka, F., Lammer, H., Lanza, A. F., Lebreton, Y., Magrin, D., Marcos-Arenal, P., Marrese, P. M., Marques, J. P., Martins, J., Mathis, S., Mathur, S., Messina, S., Miglio, A., Montalban, J., Montalto, M., Monteiro, M. J. P. F. G., Moradi, H., Moravveji, E., Mordasini, C., Morel, T., Mortier, A., Nascimbeni, V., Nelson, R. P., Nielsen, M. B., Noack, L., Norton, A. J., Ofir, A., Oshagh, M., Ouazzani, R. -M., P��pics, P., Parro, V. C., Petit, P., Plez, B., Poretti, E., Quirrenbach, A., Ragazzoni, R., Raimondo, G., Rainer, M., Reese, D. R., Redmer, R., Reffert, S., Rojas-Ayala, B., Roxburgh, I. W., Salmon, S., Santerne, A., Schneider, J., Schou, J., Schuh, S., Schunker, H., Silva-Valio, A., Silvotti, R., Skillen, I., Snellen, I., Sohl, F., Sousa, S. G., Sozzetti, A., Stello, D., Strassmeier, K. G., ��vanda, M., Szab��, Gy. M., Tkachenko, A., Valencia, D., van Grootel, V., Vauclair, S. D., Ventura, P., Wagner, F. W., Walton, N. A., Weingrill, J., Werner, S. C., Wheatley, P. J., Zwintz, K., DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Stockholm University, Stellar Astrophysics Centre [Aarhus] (SAC), Aarhus University [Aarhus], Department of Palaeontology, National Institutes of Health [Bethesda] (NIH)-The Natural History Museum (NHM), Laboratoire d'Informatique Avancée de Saint-Denis (LIASD), Université Paris 8 Vincennes-Saint-Denis (UP8), High Speed Networks Laboratory, Dept. of Telecommunications and Media Informatics, Budapest University of Technology and Economics [Budapest] (BME), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes - UFR Pharmacie (UGA UFRP), Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Department of Physics and Astronomy [Leicester], University of Leicester, Institute for Digital Communication Joint Research Institute for Signal & Image Processing School of Engineering and Electronics - University of Edinburgh, University of Edinburgh, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), DLR Institute of Planetary Research, German Aerospace Center (DLR), UCLA Economics, University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Nottingham Transportation Engineering Centre, University of Nottingham, UK (UON), Thüringer Landessternwarte Tautenburg (TLS), Tel Aviv University (TAU), Center for Space and Habitability (CSH), University of Bern, Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Département Langues et Culture Internationale (LCI), Université européenne de Bretagne - European University of Brittany (UEB)-Télécom Bretagne-Institut Mines-Télécom [Paris] (IMT), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, CTS/UNINOVA, Faculty of Sciences and Technology, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, School of Physics and Astronomy, University of Birmingham [Birmingham], Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), LAboratoire PLasma et Conversion d'Energie (LAPLACE), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT), Institut für Physik, Universität Rostock, Landessternwarte Königstuhl [ZAH] (LSW), Universität Heidelberg [Heidelberg] = Heidelberg University, Mécanismes adaptatifs : des organismes aux communautés (MAOAC), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Historisches Institut, Universität Paderborn (UPB), Hansen Experimental Physics Lab [Stanford] (HEPL), Stanford University, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), Department of Experimental Physics, University of Szeged [Szeged], ELTE Gothard Astrophysical Observatory, Eötvös Loránd University (ELTE), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Juelich Centre for Neutron Science, IFF, Forschungszentrum Juelich, Institut fuer Festkoerperforschung Juelich, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universität Bern [Bern], Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Genève (UNIGE), Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Grenoble Alpes (UGA), University of California-University of California, Universidade do Porto [Porto], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Space Agency (ESA)-European Space Agency (ESA), Tel Aviv University [Tel Aviv], Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), The Open University [Milton Keynes] (OU), Max-Planck-Institut für Sonnensystemforschung (MPS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Osaka City University Advanced Mathematical Institute (OCAMI), Osaka Media Center, Technical University of Denmark [Lyngby] (DTU), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées, Universität Heidelberg [Heidelberg], Muséum national d'Histoire naturelle (MNHN)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), Hansen Experimental Physics Laboratory (HEPL), Stanford University [Stanford], ELTE Gao-Lendulet Research Group, Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Low Energy Astrophysics (API, FNWI), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universidade do Porto, Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Osaka City university Advanced Mathematical Institute [Osaka] (OCAMI), Osaka City University (OCU), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), and Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: photometry, Gas giant, 530 Physics, FOS: Physical sciences, asteroseismology, Astrophysics::Cosmology and Extragalactic Astrophysics, transit surey, Asteroseismology, INSTRUMENTAÇÃO (ASTRONOMIA), Planet, Astrophysics::Solar and Stellar Astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Seismaology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Exoplanetary science, Planetary habitability, Exoplanets, 520 Astronomy, Stellar science, Astronomy, Astronomy and Astrophysics, Planetary system, 620 Engineering, Exoplanet, Stars, exoplanets, 13. Climate action, Space and Planetary Science, Transit survey, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Circumstellar habitable zone, Astrophysics - Earth and Planetary Astrophysics
Abstract: PLATO 2.0 has recently been selected for ESA's M3 launch opportunity (2022/24). Providing accurate key planet parameters (radius, mass, density and age) in statistical numbers, it addresses fundamental questions such as: How do planetary systems form and evolve? Are there other systems with planets like ours, including potentially habitable planets? The PLATO 2.0 instrument consists of 34 small aperture telescopes (32 with 25 sec readout cadence and 2 with 2.5 sec candence) providing a wide field-of-view (2232 deg2) and a large photometric magnitude range (4-16 mag). It focusses on bright (4-11 mag) stars in wide fields to detect and characterize planets down to Earth-size by photometric transits, whose masses can then be determined by ground-based radial-velocity follow-up measurements. Asteroseismology will be performed for these bright stars to obtain highly accurate stellar parameters, including masses and ages. The combination of bright targets and asteroseismology results in high accuracy for the bulk planet parameters: 2%, 4-10% and 10% for planet radii, masses and ages, respectively. The planned baseline observing strategy includes two long pointings (2-3 years) to detect and bulk characterize planets reaching into the habitable zone (HZ) of solar-like stars and an additional step-and-stare phase to cover in total about 50% of the sky. PLATO 2.0 will observe up to 1,000,000 stars and detect and characterize hundreds of small planets, and thousands of planets in the Neptune to gas giant regime out to the HZ. It will therefore provide the first large-scale catalogue of bulk characterized planets with accurate radii, masses, mean densities and ages. This catalogue will include terrestrial planets at intermediate orbital distances, where surface temperatures are moderate. Coverage of this parameter range with statistical numbers of bulk characterized planets is unique to PLATO 2.0., Comment: 63 pages, 17 figures, submitted to Experimental Astronomy (ExA)
Published: 2014

19. Caractérisation sédimentaire d’une roche mère carbonatée du Bassin aquitain : exemple de la formation Parnac du Quercy

Author: Bastianini, L., Hoareau, Guilhem, Caline, B., Guy, L., Martinez, M., Baudin, F., Bonnel, Cédric, Laboratoire des Fluides Complexes et leurs Réservoirs (LFCR), TOTAL FINA ELF-Université de Pau et des Pays de l'Adour (UPPA)-Centre National de la Recherche Scientifique (CNRS), Centre scientifique et Technique Jean Feger (CSTJF), TOTAL FINA ELF, Solvay Silica, Solvay (France), DAM Île-de-France (DAM/DIF), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), and Direction de Recherche Technologique (CEA) (DRT (CEA))
Subjects: [PHYS]Physics [physics], [PHYS.MECA.MEMA]Physics [physics]/Mechanics [physics]/Mechanics of materials [physics.class-ph], [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], [SPI.MECA.MEMA]Engineering Sciences [physics]/Mechanics [physics.med-ph]/Mechanics of materials [physics.class-ph], [PHYS.MECA.GEME]Physics [physics]/Mechanics [physics]/Mechanical engineering [physics.class-ph], [SPI.MECA.MEFL]Engineering Sciences [physics]/Mechanics [physics.med-ph]/Fluids mechanics [physics.class-ph]
Abstract: AFF; International audience
Published: 2014

20. Differential asteroseismic study of seismic twins observed by CoRoT

Author: Ozel, N., Mosser, B., Dupret, M. A., Bruntt, H., Barban, C., Deheuvels, S., García, R. A., Michel, E., Samadi, R., Baudin, F., Mathur, S., Régulo, C., Auvergne, M., Catala, C., Morel, Pierre, Pichon, B., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: techniques: photometric, Astrophysics::Solar and Stellar Astrophysics, stars: individual: HD 181420, Astrophysics::Earth and Planetary Astrophysics, stars: evolution, asteroseismology, stars: interiors, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], stars: individual: HD 175272
Abstract: International audience; Context. The CoRoT short asteroseismic runs give us the opportunity to observe a large variety of late-type stars through their solar-like oscillations. We report the observation and modeling of the F5V star HD 175272.Aims. Our aim is to define a method for extracting as much information as possible from a noisy oscillation spectrum. Methods. We followed a differential approach that consists of using a well-known star as a reference to characterize another star. We used classical tools such as the envelope autocorrelation function to derive the global seismic parameters of the star. We compared HD 175272 with HD 181420 through a linear approach, because they appear to be asteroseismic twins.Results. The comparison with the reference star enables us to substantially enhance the scientific output for HD 175272. First, we determined its global characteristics through a detailed seismic analysis of HD 181420. Second, with our differential approach, we measured the difference of mass, radius and age between HD 175272 and HD 181420.Conclusions. We have developed a general method able to derive asteroseismic constraints on a star even in case of low-quality data. This method can be applied to stars with interesting properties but low signal-to-noise ratio oscillation spectrum, such as stars hosting an exoplanet or members of a binary system.
Published: 2013

21. Microstructures and Textures in a Cu-Ni-Si Alloy Processed by High-Pressure Torsion

Author: A.Y. Khereddine, F.H. Larbi, H. Azzeddine, T. Baudin, F. Brisset, A.L. Helbert, M.H. Mathon, M. Kawasaki, D. Bradai and T.G. Langdon
Published: 2013

22. CoRoT Observations of O Stars: Diverse Origins of Variability

Author: Blomme, R., Briquet, M., Degroote, P., Mahy, L., Aerts, Conny, Cuypers, J., Godart, M., Gosset, E., Hareter, M., Montalban, J., Morel, T., Nieva, M.F., Noels, A., Oreiro, R., Poretti, E., Przybilla, N., Rainer, M., Rauw, G., Schiller, F., Simon-Diaz, S., Smolders, K., Ventura, P., Vučković, M., Auvergne, M., Baglin, A., Baudin, F., Catala, C., Michel, E., Samadi, R., Rubert, C., St-Louis, N., Moffat, A.F.J., Drissen, L., and Drissen, L.
Subjects: Astronomy, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astronomical Society of the Pacific Conference Series
Abstract: Contains fulltext : 111302.pdf (Author’s version preprint ) (Open Access) Contains fulltext : 111302.pdf (Publisher’s version ) (Closed access)
Published: 2013

23. An in-depth study of HD 174966 with CoRoT photometry and HARPS spectroscopy. Large separation as a new observable for ��Sct stars

Author: Hern��ndez, A. Garc��a, Moya, A., Michel, E., Su��rez, J. C., Poretti, E., Mart��n-Ru��z, S., Amado, P. J., Garrido, R., Rodr��guez, E., Rainer, M., Uytterhoeven, K., Rodrigo, C., Solano, E., Rod��n, J. R., Mathias, P., Rolland, A., Auvergne, M., Baglin, A., Baudin, F., Catala, C., and Samadi, R.
Subjects: Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: The aim of this work was to use a multi-approach technique to derive the most accurate values possible of the physical parameters of the ��Sct star HD174966. In addition, we searched for a periodic pattern in the frequency spectra with the goal of using it to determine the mean density of the star. First, we extracted the frequency content from the CoRoT light curve. Then, we derived the physical parameters of HD174966 and carried a mode identification out from the spectroscopic and photometric observations. We used this information to look for the models fulfilling all the conditions and discussed the inaccuracies of the method because of the rotation effects. In a final step, we searched for patterns in the frequency set using a Fourier transform, discussed its origin and studied the possibility of using the periodicity to obtain information about the physical parameters of the star. A total of 185 peaks were obtained from the Fourier analysis of the CoRoT light curve, being almost all reliable pulsating frequencies. From the spectroscopic observations, 18 oscillation modes were detected and identified, and the inclination angle ($62.5^{\circ}$$^{+7.5}_{-17.5}$) and the rotational velocity of the star (142 km/s) were estimated. From the multi-colour photometric observations, 3 frequencies were detected, which correspond to the main ones in the CoRoT light curve. We looked for periodicities within the 185 frequencies and found a periodic pattern ~64 ��Hz. Using the inclination angle, the rotational velocity and an Echelle diagram, showing a double comb outside the asymptotic regime, we concluded that the periodicity corresponds to a large separation structure. The periodic pattern allowed us to discriminate models from a grid, finding that the value of the mean density is achieved with a 6% uncertainty. So, the pattern could be used as a new observable for A-F type stars., 15 pages, 10 figures, 6 tables
Published: 2013
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24. Evaluation of Titanium Direct Bonding MechanismStudy of crystal-crucible detachment: GaSb in SiO2

Author: Baudin, F., Delaye, V., Guedj, C., Chevalier, N., Mariolle, D., Imbert, B., Fabbri, J.M., Di Cioccio, L., Brechet, Y., Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Science et Ingénierie des Matériaux et Procédés (SIMaP), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [CHIM.MATE]Chemical Sciences/Material chemistry
Abstract: International audience; Direct metal bonding represents an advanced joining technology that allows vertical stacking with electrical conduction and even heat dissipation. For most metals used as bonding layers, direct bonding when operating under ambient conditions involves metal oxides. The bonding interface saddles with a trapped oxide layer that might affect electrical conduction and even complete sealing of bonding interface. Titanium especially because of its high affinity with oxygen makes oxide free direct bonding very difficult. In the mean time, the remarkable getter effect of Ti matrix allows the dissolution of oxygen during post bonding annealing. In this paper, the bonding limits with regards to the titanium thickness have been investigated. The key role of layer roughness on the bonding quality and energy has been pointed out. A titanium thickness below 10 nm appears as a limit for an oxide free bonding in our conditions. (C) 2013 The Electrochemical Society.
Published: 2013

25. CoRoT Observations of O Stars: Diverse Origins of Variability

Author: Blomme, R., Briquet, M., Degroote, P., Mahy, L., Aerts, C., Cuypers, J., Godart, M., Gosset, E., Hareter, M., Montalban, J., Morel, T., Nieva, M. F., Noels, A., Oreiro, R., Poretti, E., Przybilla, N., Rainer, M., Rauw, G., Schiller, F., Simon-Diaz, S., Smolders, K., Ventura, P., Vučković, M., Auvergne, M., Baglin, A., Baudin, F., Catala, C., Michel, E., Samadi, R., Blomme, Briquet, Degroote, Mahy, Aerts, Cuypers, Godart, Gosset, Hareter, Montalban, Morel, Nieva, M. F., Noels, Oreiro, Poretti, Przybilla, Rainer, Rauw, Schiller, Simon-Diaz, Smolders, Ventura, Vučković, Auvergne, Baglin, Baudin, Catala, Michel, and Samadi
Published: 2012

26. Amplitudes of solar-like oscillations in red giant stars

Author: Samadi, R., Belkacem, K., Dupret, M.-A., Ludwig, H.-G., Baudin, F., Caffau, E., Goupil, M.-J., Barban, C., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), and Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
Subjects: [PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2012

27. Damping rates of solar-like oscillations across the HR diagram

Author: Belkacem, K., Dupret, M., Baudin, F., Appourchaux, T., Marques, J., Samadi, R., Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire d'automatique et de génie des procédés (LAGEP), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École Supérieure de Chimie Physique Électronique de Lyon (CPE)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Université de Lyon-Université de Lyon-École Supérieure Chimie Physique Électronique de Lyon-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2012

28. CoRoT's view on variable B8/9 stars: spots versus pulsations. Evidence for differential rotation in HD 174648

Author: Degroote, P., Acke, B., Samadi, R., Aerts, C., Kurtz, D. W., Noels, A., Miglio, A., Montalbxe1n, J., Bloemen, S., Baglin, A., Baudin, F., Catala, C., Michel, E., Auvergne, M., Degroote, Acke, Samadi, Aerts, Kurtz, D. W., Noels, Miglio, Montalbxe1n, Bloemen, Baglin, Baudin, Catala, Michel, and Auvergne
Published: 2011

29. Investigation of three red giants observed in the CoRoT seismo field

Author: Hekker, S., Morel, T., Mazumdar, A., Baudin, F., Poretti, E., and Rainer, M.
Subjects: Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Three red giants (HD 49566 (G5III), HD 169370 (K0III) and HD 169751 (K2III)) have been observed in the CoRoT seismo field and additional ground-based spectra have been acquired. We present preliminary results of a detailed study of these stars using the observational constraints from the spectra and CoRoT data, and models from the YREC stellar evolution code., 2 pages, 1 table, 1 figure, proceedings for the second CoRoT symposium
Published: 2011

30. Variability in the CoRoT photometry of three hot O-type stars. HD 46223, HD 46150, and HD 46966

Author: Blomme, R., Mahy, L., Catala, C., Cuypers, J., Gosset, E., Godart, M., Montalban, J., Ventura, P., Rauw, G., Morel, T., Degroote, P., Aerts, C., Noels, A., Michel, E., Baudin, F., Baglin, A., Auvergne, M., Samadi, R., Blomme, Mahy, Catala, Cuypers, Gosset, Godart, Montalban, Ventura, Rauw, Morel, Degroote, Aerts, Noels, Michel, Baudin, Baglin, Auvergne, and Samadi
Published: 2011

31. The underlying physical meaning of the $\nu_{\rm max}-\nu_{\rm c}$ relation

Author: Belkacem, K., Goupil, M. J., Dupret, M. A., Samadi, R., Baudin, F., Noels, A., and Mosser, B.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract: Asteroseismology of stars that exhibit solar-like oscillations are enjoying a growing interest with the wealth of observational results obtained with the CoRoT and Kepler missions. In this framework, scaling laws between asteroseismic quantities and stellar parameters are becoming essential tools to study a rich variety of stars. However, the physical underlying mechanisms of those scaling laws are still poorly known. Our objective is to provide a theoretical basis for the scaling between the frequency of the maximum in the power spectrum ($\nu_{\rm max}$) of solar-like oscillations and the cut-off frequency ($\nu_{\rm c}$). Using the SoHO GOLF observations together with theoretical considerations, we first confirm that the maximum of the height in oscillation power spectrum is determined by the so-called \emph{plateau} of the damping rates. The physical origin of the plateau can be traced to the destabilizing effect of the Lagrangian perturbation of entropy in the upper-most layers which becomes important when the modal period and the local thermal relaxation time-scale are comparable. Based on this analysis, we then find a linear relation between $\nu_{\rm max}$ and $\nu_{\rm c}$, with a coefficient that depends on the ratio of the Mach number of the exciting turbulence to the third power to the mixing-length parameter., Comment: 8 pages, 11 figures. Accepted in A&A
Published: 2011

32. CoRoT observations of O stars: diverse origins of variability

Author: Blomme, R., Briquet, M., Degroote, P., Mahy, L., Aerts, C., Cuypers, J., Godart, M., Gosset, E., Hareter, M., Montalban, J., Morel, T., Nieva, M. F., Noels, A., Oreiro, R., Poretti, E., Przybilla, N., Rainer, M., Gregor Rauw, Schiller, F., Simon-Diaz, S., Smolders, K., Ventura, P., Vučković, M., Auvergne, M., Baglin, A., Baudin, F., Catala, C., Michel, E., and Samadi, R.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Six O-type stars were observed continuously by the CoRoT satellite during a 34.3-day run. The unprecedented quality of the data allows us to detect even low-amplitude stellar pulsations in some of these stars (HD 46202 and the binaries HD 46149 and Plaskett's star). These cover both opacity-driven modes and solar-like stochastic oscillations, both of importance to the asteroseismological modelling of O stars. Additional effects can be seen in the CoRoT light curves, such as binarity and rotational modulation. Some of the hottest O-type stars (HD 46223, HD 46150 and HD 46966) are dominated by the presence of red-noise: we speculate that this is related to a sub-surface convection zone., Comment: 5 pages, 3 figures, conference paper. To be published in "Four decades of Research on Massive Stars", Astronomical Society of the Pacific. Eds. C. Robert, N. St-Louis and L. Drissen
Published: 2011
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33. A quantitative analysis of stellar activity based on CoRoT photometric data

Author: Hulot, J. C., Baudin, F., Samadi, R., and Goupil, M. J.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: The CoRoT satellite has made available high precision photometric observations of a large number of stars of different spectral types. Continuous photometric time series allow the characterization of stellar microvariability in a systematic way. We determine an index indicating the level of activity, derived from photometric data, for a large sample of stars with different color temperatures. We also assess to what extent this index can be related to an estimated Rossby number for stars whose rotation period can be estimated. We also estimate a characteristic lifetime of the surface heterogeneities. Our work is based on the Fourier analysis of stellar light curves. We analyzed the Fourier power spectra of 430 selected light curves obtained by CoRoT during three observation runs. The low-frequency contribution of the stellar variability is modelled by a "generalized semi-lorentzian" profile. An activity index is derived from the fitted amplitude and width of the semi-lorentzian model. Some of the Fourier spectra exhibit a rotational modulation which enables the determination of the rotation period. In addition, a convective turnover time is derived from a grid of stellar models, so that a Rossby number can be estimated. A characteristic lifetime of the phenomena causing the observed power at low frequency is assessed from the fitted model of the power spectrum and is compared to the rotation period. Higher values of the microvariability index are observed among the coolest stars from our sample. 28 light curves show a clear rotational modulation. The estimated Rossby number of most of the observed stars with a rotational modulation is less than 1. The activity index decreases with increasing Rossby number. The quality of the CoRoT data enables the determination of the characteristic lifetime of active structures. It is shown to increase with the rotation period., Comment: second revised version submitted to A&A on April 11, 2011 10 pages, 8 figures
Published: 2011
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34. Red Giants observed with CoRoT

Author: Hekker, S., Ridder, J., Baudin, F., Barban, C., Carrier, F., Hatzes, A. P., Thomas Kallinger, and Weiss, W. W.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Physics::Space Physics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract: Observations of red (G-K)-giant stars with the CoRoT satellite provide unprecedented information on the stochastically excited oscillations in these stars. The long time series of nearly uninterrupted high-cadence and high-precision photometry revealed the presence of non-radial modes with long lifetimes, which opens the possibility to perform asteroseismology on these stars. Also, the large number of red giants, for which solar-like oscillations are now observed, allows for a more statistical investigation of the characteristics of solar-like oscillations in red giants., Proc. 'Stellar Pulsation: Challenges for theory and observation'; eds Joyce Ann Guzik, Paul A. Bradley; AIP Conf. Proc., Vol. 1170, pp. 127-131 (2009)
Published: 2010

35. Amplitude variations of the CoRoT Be star 102719279

Author: Gutiérrez-Soto, J., Semaan, T., Garrido, R., Baudin, F., Hubert, A. -M., and Neiner, C.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: The Be star 102719279 is an interesting target observed with CoRoT during two runs, giving us the possibility to study the stability of the detected frequencies and to search for any correlation with outburts, as it was recently found in the Be star HD 49330 (Huat et al. 2009). The light curve of the star 102719279 shows fadings, multiperiodicity, stable and transient frequencies, etc. The short-term variations of the light curve are probably produced by non-radial pulsations together with some material that is ejected from the star, which produces the transient frequency. It is should be noted that the two main frequencies are synchronized and have the maximum amplitude just before the outburst., Comment: 4 pages, 4 figures, Astronomische Nachrichten, HELASIV conference, Lanzarote, February 2010, submitted
Published: 2010
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36. The CoRoT target HD 49933: 2- Comparison of theoretical mode amplitudes with observations

Author: Samadi, R., Ludwig, H. -G., Belkacem, K., Goupil, M. J., Benomar, O., Mosser, B., Dupret, M. -A., Baudin, F., Appourchaux, T., and Michel, E.
Subjects: Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: From the seismic data obtained by CoRoT for the star HD 49933 it is possible, as for the Sun, to constrain models of the excitation of acoustic modes by turbulent convection. We compare a stochastic excitation model described in Paper I (arXiv:0910.4027) with the asteroseismology data for HD 49933, a star that is rather metal poor and significantly hotter than the Sun. Using the mode linewidths measured by CoRoT for HD 49933 and the theoretical mode excitation rates computed in Paper I, we derive the expected surface velocity amplitudes of the acoustic modes detected in HD 49933. Using a calibrated quasi-adiabatic approximation relating the mode amplitudes in intensity to those in velocity, we derive the expected values of the mode amplitude in intensity. Our amplitude calculations are within 1-sigma error bars of the mode surface velocity spectrum derived with the HARPS spectrograph. The same is found with the mode amplitudes in intensity derived for HD 49933 from the CoRoT data. On the other hand, at high frequency, our calculations significantly depart from the CoRoT and HARPS measurements. We show that assuming a solar metal abundance rather than the actual metal abundance of the star would result in a larger discrepancy with the seismic data. Furthermore, calculations that assume the ``new'' solar chemical mixture are in better agreement with the seismic data than those that assume the ``old'' solar chemical mixture. These results validate, in the case of a star significantly hotter than the Sun and Alpha Cen A, the main assumptions in the model of stochastic excitation. However, the discrepancies seen at high frequency highlight some deficiencies of the modelling, whose origin remains to be understood., 8 pages, 3 figures (B-W and color), accepted for publication in Astronomy & Astrophysics. Corrected typo in Eq. (4). Updated references. Language improvements
Published: 2009

37. VizieR Online Data Catalog: Supervised classification of CoRoT variables (Debosscher+, 2009)

Author: Debosscher, J., Sarro, L.~m., Lopez, M., Deleuil, M., Aerts, C., Auvergne, M., Baglin, A., Baudin, F., Chadid, M., Charpinet, S., Cuypers, J., de Ridder, J., Garrido, R., Hubert, A.~m., Janot-Pacheco, E., Jorda, L., Kaiser, Andreas, Kallinger, T., Kollath, Z., Maceroni, C., Mathias, P., Michel, E., Moutou, C., Neiner, C., Ollivier, M., Samadi, R., Solano, E., Surace, C., Vandenbussche, B., Weiss, W.~w., Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituut voor Sterrenkunde [Leuven], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Division technique INSU/SDU (DTI), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Royal Observatory of Belgium [Brussels] (ROB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Astronomia, Geofisica e Ciencias Atmosfericas (IAGCAUSP), Universidade de São Paulo = University of São Paulo (USP), Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Institute for Astronomy [Vienna], University of Vienna [Vienna], Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Spanish Virtual Observatory - Observatorio Virtual Español (SVO), and Spanish Virtual Observatory - Observatorio Virtual Español
Subjects: [INFO]Computer Science [cs], Stars: variable, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; Light curve parameters and classification results are presented for all the objects measured in the first four CoRoT observing runs: IRa01, SRc01, LRc01, and LRa01. The information presented here should allow scientists to make candidate lists of their objects of study and to obtain some basic light curve information. We recall that we did not perform detailed light curve modelling, only a basic one, sufficient for producing variability class memberships for each target. We refer to the paper for a detailed description of the light curve parameters, and the classification results. It is strongly advised to read the paper prior to using the results presented here. (4 data files).
Published: 2009

38. VizieR Online Data Catalog: Supervised classification of CoRoT variables (Debosscher+, 2009)

Author: Debosscher, J., Sarro, L.~m., Lopez, M., Deleuil, M., Aerts, C., Auvergne, M., Baglin, A., Baudin, F., Chadid, M., Charpinet, S., Cuypers, J., de Ridder, J., Garrido, R., Hubert, A.~m., Janot-Pacheco, E., Jorda, L., Kaiser, Andreas, Kallinger, T., Kollath, Z., Maceroni, C., Mathias, P., Michel, E., Moutou, C., Neiner, C., Ollivier, M., Samadi, R., Solano, E., Surace, C., Vandenbussche, B., Weiss, W.~w., Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituut voor Sterrenkunde [Leuven], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Division technique INSU/SDU (DTI), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Royal Observatory of Belgium [Brussels] (ROB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Astronomia, Geofisica e Ciencias Atmosfericas (IAGCAUSP), Universidade de São Paulo = University of São Paulo (USP), Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Institute for Astronomy [Vienna], University of Vienna [Vienna], Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Spanish Virtual Observatory - Observatorio Virtual Español (SVO), and Spanish Virtual Observatory - Observatorio Virtual Español
Subjects: [INFO]Computer Science [cs], Stars: variable, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; Light curve parameters and classification results are presented for all the objects measured in the first four CoRoT observing runs: IRa01, SRc01, LRc01, and LRa01. The information presented here should allow scientists to make candidate lists of their objects of study and to obtain some basic light curve information. We recall that we did not perform detailed light curve modelling, only a basic one, sufficient for producing variability class memberships for each target. We refer to the paper for a detailed description of the light curve parameters, and the classification results. It is strongly advised to read the paper prior to using the results presented here. (4 data files).
Published: 2009

39. VizieR Online Data Catalog: Supervised classification of CoRoT variables (Debosscher+, 2009)

Author: Debosscher, J., Sarro, L.~M., Lopez, M., Deleuil, M., Aerts, C., Auvergne, M., Baglin, A., Baudin, F., Chadid, M., Charpinet, S., Cuypers, J., De Ridder, J., Garrido, R., Hubert, A.~M., Janot-Pacheco, E., Jorda, L., Kaiser, Andreas, Kallinger, T., Kollath, Z., Maceroni, C., Mathias, P., Michel, E., Moutou, C., Neiner, C., Ollivier, M., Samadi, R., Solano, E., Surace, C., Vandenbussche, B., Weiss, W.~W., Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Instituut voor Sterrenkunde [Leuven], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National des Sciences de l'Univers (INSU/SPU), Centre National de la Recherche Scientifique (CNRS), Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Royal Observatory of Belgium [Brussels] (ROB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Astronomia, Geofisica e Ciencias Atmosfericas (IAGCAUSP), Universidade de São Paulo (USP), Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Institute for Astronomy [Vienna], University of Vienna [Vienna], Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Spanish Virtual Observatory - Observatorio Virtual Español (SVO), and Spanish Virtual Observatory - Observatorio Virtual Español
Subjects: [INFO]Computer Science [cs], Stars: variable, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; Light curve parameters and classification results are presented for all the objects measured in the first four CoRoT observing runs: IRa01, SRc01, LRc01, and LRa01. The information presented here should allow scientists to make candidate lists of their objects of study and to obtain some basic light curve information. We recall that we did not perform detailed light curve modelling, only a basic one, sufficient for producing variability class memberships for each target. We refer to the paper for a detailed description of the light curve parameters, and the classification results. It is strongly advised to read the paper prior to using the results presented here. (4 data files).
Published: 2009

40. VizieR Online Data Catalog: Supervised classification of CoRoT variables (Debosscher+, 2009)

Author: Debosscher, J., Sarro, L.~M., Lopez, M., Deleuil, M., Aerts, C., Auvergne, M., Baglin, A., Baudin, F., Chadid, M., Charpinet, S., Cuypers, J., De Ridder, J., Garrido, R., Hubert, A.~M., Janot-Pacheco, E., Jorda, L., Kaiser, Andreas, Kallinger, T., Kollath, Z., Maceroni, C., Mathias, P., Michel, E., Moutou, C., Neiner, C., Ollivier, M., Samadi, R., Solano, E., Surace, C., Vandenbussche, B., Weiss, W.~W., Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Instituut voor Sterrenkunde [Leuven], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National des Sciences de l'Univers (INSU/SPU), Centre National de la Recherche Scientifique (CNRS), Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Royal Observatory of Belgium [Brussels] (ROB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Astronomia, Geofisica e Ciencias Atmosfericas (IAGCAUSP), Universidade de São Paulo (USP), Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Institute for Astronomy [Vienna], University of Vienna [Vienna], Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Spanish Virtual Observatory - Observatorio Virtual Español (SVO), and Spanish Virtual Observatory - Observatorio Virtual Español
Subjects: [INFO]Computer Science [cs], Stars: variable, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; Light curve parameters and classification results are presented for all the objects measured in the first four CoRoT observing runs: IRa01, SRc01, LRc01, and LRa01. The information presented here should allow scientists to make candidate lists of their objects of study and to obtain some basic light curve information. We recall that we did not perform detailed light curve modelling, only a basic one, sufficient for producing variability class memberships for each target. We refer to the paper for a detailed description of the light curve parameters, and the classification results. It is strongly advised to read the paper prior to using the results presented here. (4 data files).
Published: 2009

41. VizieR Online Data Catalog: Supervised classification of CoRoT variables (Debosscher+, 2009)

Author: Debosscher, J., Sarro, L.~m., Lopez, M., Deleuil, M., Aerts, C., Auvergne, M., Baglin, A., Baudin, F., Chadid, M., Charpinet, S., Cuypers, J., de Ridder, J., Garrido, R., Hubert, A.~m., Janot-Pacheco, E., Jorda, L., Kaiser, Andreas, Kallinger, T., Kollath, Z., Maceroni, C., Mathias, P., Michel, E., Moutou, C., Neiner, C., Ollivier, M., Samadi, R., Solano, E., Surace, C., Vandenbussche, B., Weiss, W.~w., Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituut voor Sterrenkunde [Leuven], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Division technique INSU/SDU (DTI), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Royal Observatory of Belgium [Brussels] (ROB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Astronomia, Geofisica e Ciencias Atmosfericas (IAGCAUSP), Universidade de São Paulo = University of São Paulo (USP), Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Institute for Astronomy [Vienna], University of Vienna [Vienna], Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Spanish Virtual Observatory - Observatorio Virtual Español (SVO), and Spanish Virtual Observatory - Observatorio Virtual Español
Subjects: [INFO]Computer Science [cs], Stars: variable, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; Light curve parameters and classification results are presented for all the objects measured in the first four CoRoT observing runs: IRa01, SRc01, LRc01, and LRa01. The information presented here should allow scientists to make candidate lists of their objects of study and to obtain some basic light curve information. We recall that we did not perform detailed light curve modelling, only a basic one, sufficient for producing variability class memberships for each target. We refer to the paper for a detailed description of the light curve parameters, and the classification results. It is strongly advised to read the paper prior to using the results presented here. (4 data files).
Published: 2009

42. Automated supervised classification of variable stars in the CoRoT programme. Method and application to the first four exoplanet fields

Author: Debosscher, J., Sarro, L. M., Lxf3pez, M., Deleuil, M., Aerts, C., Auvergne, M., Baglin, A., Baudin, F., Chadid, M., Charpinet, S., Cuypers, J., De Ridder, J., Garrido, R., Hubert, A. M., Janot-Pacheco, E., Jorda, L., Kaiser, A., Kallinger, T., Kollath, Z., Maceroni, C., Mathias, P., Michel, E., Moutou, C., Neiner, C., Ollivier, M., Samadi, R., Solano, E., Surace, C., Vandenbussche, B., Weiss, W. W., Debosscher, Sarro, L. M., Lxf3pez, Deleuil, Aerts, Auvergne, Baglin, Baudin, Chadid, Charpinet, Cuypers, De Ridder, Garrido, Hubert, A. M., Janot-Pacheco, Jorda, Kaiser, Kallinger, Kollath, Maceroni, Mathias, Michel, Moutou, Neiner, Ollivier, Samadi, Solano, Surace, Vandenbussche, Weiss, and W. W.
Published: 2009

43. HD 50844: the new look of Delta Sct stars from CoRoT space photometry

Author: Poretti, E., Michel, E., Garrido, R., Lefevre, L., Mantegazza, L., Rainer, M., Rodriguez, E., Uytterhoeven, K., Pedro José Amado, Martin-Ruiz, S., Moya, A., Niemczura, E., Suarez, J. C., Zima, W., Baglin, A., Auvergne, M., Baudin, F., Catala, C., Samadi, R., Alvarez, M., Mathias, P., Paparo, M., Papics, P., and Plachy, E.
Subjects: Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: It has also been suggested that the detection of a wealth of very low amplitude modes in Delta Sct stars was only a matter of signal--to--noise ratio. Access to this treasure, impossible from the ground, is one of the scientific aims of the space mission CoRoT, a space mission developed and operated by CNES. This work presents the results obtained on HD 50844: the 140,016 datapoints were analysed using independent approaches and several checks performed. A level of 10^{-5} mag was reached in the amplitude spectra of the CoRoT timeseries. The frequency analysis of the CoRoT timeseries revealed hundreds of terms in the frequency range 0--30 d^{-1}. All the cross--checks confirmed this new result. The initial guess that Delta Sct stars have a very rich frequency content is confirmed. The spectroscopic mode identification gives theoretical support since very high--degree modes (up to ell=14) are identified. We also prove that cancellation effects are not sufficient in removing the flux variations associated to these modes at the noise level of the CoRoT measurements. The ground--based observations indicate that HD 50844 is an evolved star that is slightly underabundant in heavy elements, located on the Terminal Age Main Sequence. Probably due to this unfavourable evolutionary status, no clear regular distribution is observed in the frequency set. The predominant term (f_1=6.92 d^{-1}) has been identified as the fundamental radial mode combining ground-based photometric and spectroscopic data. This work is also based on observations made with ESO telescopes under the ESO Large Programme LP178.D-0361 and on data collected at the Observatorio de Sierra Nevada, at the Observatorio Astronomico Nacional San Pedro Martir, and at the Piszkesteto Mountain Station of Konkoly Observatory., 10 pages, 11 figures. Accepted for publication in Astronomy & Astrophysics
Published: 2009

44. The B0.5IVe CoRoT target HD 49 330. I. Photometric analysis from CoRoT data

Author: Huat, A.L., Hubert, A.M., Floquet, M., Neiner, C., Frémat, Y., Gutiérrez Soto, Juan, Baudin, F., Andrade, L., De Batz, B., Diago Nebot, Pascual David, Emilio, M., Espinosa-Lara, F., Fabregat Llueca, Juan, Janot-Pacheco, E., Leroy, B., Martayan, C., Semaan, T., Suso, J., Michel, E., and Samadi, R.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astronomia, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Ciència Ensenyament
Abstract: Context. Be stars undergo outbursts producing a circumstellar disk from the ejected material. The beating of non-radial pulsations has been put forward as a possible mechanism of ejection. Aims. We analyze the pulsational behavior of the early B0.5IVe star HD 49330 observed during the first CoRoT long run towards the Galactical anticenter (LRA1). This Be star is located close to the lower edge of the β Cephei instability strip in the HR diagram and showed a 0.03 mag outburst during the CoRoT observations. It is thus an ideal case for testing the aforementioned hypothesis. Methods. We analyze the CoRoT light curve of HD 49330 usin g Fourier methods and non-lin ear least square fitting. Results. In this star, we find pulsation modes typical of β Cep stars (p modes) and SPB stars (g modes) with amplitude variations along the run directly correlated with the outburst. These results provide new clues about the origin of the Be phenomenon as well as strong constraints on the seismic modelling of Be stars.
Published: 2009

45. Asteroseismic analysis of the CoRoT ��-Scuti star HD174936

Author: Hern��ndez, A. Garc��a, Moya, A., Michel, E., Garrido, R., Su��rez, J. C., Rodr��guez, E., Amado, P. J., Mart��n-Ru��z, S., Rolland, A., Poretti, E., Samadi, R., Baglin, A., Auvergne, M., Catala, C., Lefevre, L., and Baudin, F.
Subjects: Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present an analysis of the ��-Scuti star object HD 174936 (ID 7613) observed by CoRoT during the first short run SRc01 (27 days). A total number of 422 frequencies we are extracted from the light curve using standard prewhitening techniques. This number of frequencies was obtained by considering a spectral significance limit of sig = 10 using the software package SigSpec. Our analysis of the oscillation frequency spectrum reveals a spacing periodicity of around 52 \muHz. Although modes considered here are not in the asymptotic regime, a comparison with stellar models confirms that this signature may stem from a quasi-periodic pattern similar to the so-called large separation in solar-like stars., 7 pages, 7 figures, 2 tables. Accepted for publication in A&A CoRoT Special Feature
Published: 2009
Full Text: View/download PDF

46. Data report: bio- and lithofacies, mineralogy, and organic content of Challenger Mound (Porcupine Seabight, SW Ireland

Author: Leonide, P.S., Floquet, M., Baudin, F., Felderman, T.G., Kano, A., Williams, T., Henriet, J.-P., and Sedimentology
Published: 2009

47. The pulsations of the B5IVe star HD 181 231 observed with CoRoT and ground-based spectroscopy

Author: Neiner, C., Gutiérrez Soto, Juan, Baudin, F., De Batz, B., Frémat, Y., Huat, A.L., Floquet, M., Hubert, A.M., Leroy, B., Diago Nebot, Pascual David, Poretti, E., Carrier, F., Rainer, M., Catala, C., Thizy, O., Buil, C., Ribeiro, J., Andrade, L., Emilio, M., Espinosa-Lara, F., Fabregat Llueca, Juan, Janot-Pacheco, E., Martayan, C., Semaan, T., Suso, J., Baglin, A., Michel, E., and Samadi, R.
Subjects: Astronomia, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Ciència Ensenyament
Abstract: Context. HD 181231 is a B5IVe star, which has been observed with the CoRoT satellite during ∼5 consecutive months and simultaneously from the ground in spectroscopy and spectropolarimetry. Aims. By analysing these data, we aim to detect and characterize as many pulsation frequencies as possible, to search for the presence of beating effects possibly at the origin of the Be phenomenon. Our results will also pr ovide a basis for seismic modelling. Methods. The fundamental parameters of the star are determined from spectral fitting and from the study of the circumstellar emission. The CoRoT photometric data and ground-based spectroscopy are analysed using several Fourier Techniques: CLEAN-NG,PASPER,and TISAFT, as well as a time-frequency technique. A search for a magnetic field is performed by applying the LSD technique to the spectropolarimetric data. Results. We find that HD 181231 is a B5IVe star seen with an inclination of ∼45 degrees. No magnetic field is detected in its photo-sphere. We detect at least 10 independent significant frequencies of variations among the 54 detected frequencies, interpreted in termsof non-radial pulsation modes and rotation. Two longer-term variations are also detected: one at ∼14 days resulting from a beating effect between the two main frequencies of short-term variations, the other at ∼116 days due either to a beating of frequencies or to a zonal pulsation mode. Conclusions. Our analysis of the CoRoT light curve and ground-based spectroscopic data of HD 181231 has led to the determination of the fundamental and pulsational parameters of the star, including beating effects. This will allow a precise seismic modelling of this star.
Published: 2009

48. Transiting exoplanets from the CoRoT space mission VIII. CoRoT-7b: the first super-Earth with measured radius

Author: Leger, A., Rouan, D., Jodi Schneider, Barge, P., Fridlund, M., Samuel, B., Ollivier, M., Guenther, E., Deleuil, M., Deeg Hj, Auvergne, M., Alonso, R., Aigrain, S., Alapini, A., Almenara Jm, Baglin, A., Barbieri, M., Bruntt, H., Pascal Bordé, Bouchy, F., Cabrera, J., Catala, C., Carone, L., Carpano, S., Csizmadia, S., Dvorak, R., Erikson, A., Ferraz-Mello, S., Foing, B., Grasset, O., Fressin, F., Gandolfi, D., Gillon, M., Gondoin, P., Guillot, T., Hatzes, A., Hebrard, G., Jorda, L., Lammer, H., Llebaria, A., Loeillet, B., Mayor, M., Mazeh, T., Moutou, C., Patzold, M., Pont, F., Queloz, D., Rauer, H., Renner, S., Samadi, R., Shporer, A., Sotin, C., Tingley, B., Wuchterl, G., Adda, M., Agogu, P., Appourchaux, T., Ballans, H., Baron, P., Beaufort, T., Bellenger, R., Berlin, R., Bernardi, P., Blouin, D., Baudin, F., Bodin, P., Boisnard, L., Boit, L., Bonneau, F., Borzeix, S., Briet, R., Buey Jt, Butler, B., Cailleau, D., Cautain, R., Chabaud Py, Chaintreuil, S., Chiavassa, F., Costes V, Parrho Vc, Fialho Fd, Decaudin, M., Defise Jm, Djalal, S., Epstein, G., Exil Ge, Faure, C., Fenouillet, T., Gaboriaud, A., Gallic, A., Gamet, P., Gavalda, P., Grolleau, E., Gruneisen, R., Gueguen, L., Guis, V., V. Guivarc'H, Guterman, P., Hallouard, D., Hasiba, J., Heuripeau, F., Huntzinger, G., Hustaix, H., Imad, C., Imbert, C., Johlander, B., Jouret, M., Journoud, P., Karioty, F., Kerjean, L., Lafaille, V., Lafond, L., Lam-Trong, T., Landiech, P., Lapeyrere, V., Larque, T., Laudet, P., Lautier, N., Lecann, H., Lefevre, L., Leruyet, B., Levacher, P., Magnan, A., Mazy, E., Mertens, F., Mesnager Jm, Meunier Jc, Michel Jp, Monjoin, W., Naudet, D., Nguyen-Kim, K., Orcesi Jl, Ottacher, H., Perez, R., Peter, G., Plasson, P., Plesseria Jy, Pontet, B., Pradines, A., Céline Quentin, Reynaud Jl, Rolland, G., Rollenhagen, F., Romagnan, R., Russ, N., Schmidt, R., Schwartz, N., Sebbag, I., Sedes, G., Smit, H., Steller Mb, Sunter, W., Surace, C., Tello, M., Tiphene, D., Toulouse, P., Ulmer, B., Vandermarcq, O., Vergnault, E., Vuillemin, A., Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA)
Subjects: [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2009

49. First asteroseismic results from CoRoT. Veröffentlichungen der Kommission für Astronomie|Communications in Asteroseismology|Communications in Asteroseismology 156 156

Author: Baglin, A., Aerts, C., Barban, C., Catala, C., Michel, E., Baudin, F., Carrier, F., Auvergne, M., Briquet, M., Appourchaux, T., and al, et
Subjects: Mathematics, Physics and Space Research
Published: 2008

50. AsteroFLAG - from the Sun to the Stars

Author: Chaplin, W.J., Appourchaux, T., Arentoft, Torben, Ballot, J., Baudin, F., Bazot, Michael, Bedding, T.R., Christensen-Dalsgaard, Jørgen, Creevey, O.L., Duez, V., Elsworth, Y., Fletcher, S.T., García, R.A., Gough, D.O., Jiménez, A., Jiménez-Reyes, S.J., Houdek, G., Kjeldsen, Hans, Lazrek, M., Leibacher, J.W., Monteiro, M.J.P.F.G., Neiner, C., New, R., Régulo, C., Salabert, D., Samadi, R., Sekii, T., Sousa, S.G., Toutain, T., and Turck-Chièze, S.
Published: 2008

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