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1. Radial mode widths in red giant stars spectra observed by Kepler

Author

Vrard Mathieu, Mosser Benoît, and Barban Caroline

Subjects
Physics, QC1-999
Abstract

The Kepler space mission has observed many solar-like pulsators, and helped to decipher their fundamental parameters (e.g: mass, radius, rotation). Most of the achievements recently obtained in that domain result from the analysis of the mode frequencies. However, unique information on non-adiabatic physics derives from the height and width of the modes. In this study, we aim at measuring the mode widths of the pressure modes in thousands of Kepler red giants and to analyze their variations in function of stellar parameters. To achieve that, we used a peakbagging technique on the star radial modes. The results show a relation between the radial mode linewidth and the effective temperature of the star as theoretically predicted. We also unveil a clear dependence with mass and stellar evolution for the radial mode width. This means that the mode damping depends on the evolutionary status of the stars.

Published
2017
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4. Influence of helium ionisation on red giant oscillation spectra

Author

Vrard M., Mosser B., and Barban C.

Subjects
Physics, QC1-999
Abstract

Since its launch in 2009, the space mission Kepler has provided an amount of data of unprecedented quality. In particular, red giants exhibit an oscillation spectrum arranged in a regular pattern called the universal oscillation pattern. Here we analyse and characterize the departures observed from this universal pattern. We measured the deviation for more than one hundred red giants and attribute it to glitches related to the region of second ionisation of helium.

Published
2015
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5. Amplitudes of solar-like oscillations in red giants: Departures from the quasi-adiabatic approximation

Author

Barban C., Ludwig H.-G., Goupil M.J., Dupret M.-A., Belkacem K., Samadi R., Baudin F., and Caffau E.

Subjects
Physics, QC1-999
Abstract

CoRoT and Kepler measurements reveal us that the amplitudes of solar-like oscillations detected in red giant stars scale from stars to stars in a characteristic way. This observed scaling relation is not yet fully understood but constitutes potentially a powerful diagnostic about mode physics. Quasi-adiabatic theoretical scaling relations in terms of mode amplitudes result in systematic and large differences with the measurements performed for red giant stars. The use of a non-adiabatic intensity-velocity relation derived from a non-adiabatic pulsation code significantly reduces the discrepancy with the CoRoT measurements. The origin of the remaining difference is still unknown. Departure from adiabatic eigenfunction is a very likely explanation that is investigated in the present work using a 3D hydrodynamical model of the surface layers of a representative red giant star.

Published
2013
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7. Radial mode widths in red giant stars spectra observed by Kepler

Author

C. Barban, Benoit Mosser, and Mathieu Vrard

Subjects
Physics, 010308 nuclear & particles physics, Red giant, QC1-999, Mode (statistics), Astronomy, Radius, Astrophysics, Effective temperature, Rotation, 01 natural sciences, Spectral line, Stars, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Stellar evolution, Astrophysics::Galaxy Astrophysics
Abstract

The Kepler space mission has observed many solar-like pulsators, and helped to decipher their fundamental parameters (e.g: mass, radius, rotation). Most of the achievements recently obtained in that domain result from the analysis of the mode frequencies. However, unique information on non-adiabatic physics derives from the height and width of the modes. In this study, we aim at measuring the mode widths of the pressure modes in thousands of Kepler red giants and to analyze their variations in function of stellar parameters. To achieve that, we used a peakbagging technique on the star radial modes. The results show a relation between the radial mode linewidth and the effective temperature of the star as theoretically predicted. We also unveil a clear dependence with mass and stellar evolution for the radial mode width. This means that the mode damping depends on the evolutionary status of the stars.

Published
2017

8. Solar-like oscillations in HD 181420: data analysis of 156 days of CoRoT data

Author

Patrick Gaulme, Ian W. Roxburgh, Clara Régulo, Patrick Boumier, Graham A. Verner, Thierry Appourchaux, Jérôme Ballot, Rafael A. García, Savita Mathur, Reza Samadi, Benoit Mosser, C. Catala, M. Auvergne, Eric Michel, Frédéric Baudin, William J. Chaplin, A. Baglin, C. Barban, Sébastien Deheuvels, Hans Bruntt, Yvonne Elsworth, 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 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), 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), School of Physics and Astronomy, University of Birmingham, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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), Instituto de Astrofísica de Canarias (IAC), Astronomy Unit, Queen Mary, and Indian Institute of Astrophysics

Subjects
Physics, Oscillation, Mode (statistics), Spectral density, Astronomy and Astrophysics, Context (language use), Astrophysics, Stars, Amplitude, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Solar-like oscillations, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Main sequence
Abstract

International audience; Context: The estimate of solar-like oscillation properties, such as their frequencies, amplitudes and lifetimes, is challenging because of their low amplitudes and will benefit from long and uninterrupted observing runs. The space telescope CoRoT allows us to obtain high-performance photometric data over a long and quasi continuous period. Among its main targets are stars for which we expect solar-like oscillations. Aims: HD 181420, an F2 main sequence star, has been observed by CoRoT during its first long run covering about 156 days. With this unprecedently high-quality set of data, our aim is to derive the p-mode parameters that can be used to probe the stellar interior. Methods: The CoRoT data obtained on HD 181420 is analysed using a classical Fourier approach for the search for the p mode signature. The p-mode parameters are then derived using global fitting of the power spectrum by a Lorentzian model, as used widely in the solar case. Results: From the p-mode frequencies, the mean value of the large spacing is estimated to be 75 {mu Hz}. The p-mode amplitudes are slightly less than 4 ppm with a line width of about 8 {mu Hz} at the maximum of the p modes. The inclination angle is estimated to be around 45 °. The large mode line-width combined with the observed mode spacing make it difficult to identify the l=2 modes and to estimate the rotational splitting. We explore two scenarios for the identification of the modes.

Published
2009
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9. Asteroseismology and interferometry of the red giant star ϵ Ophiuchi

Author

J. Sturmann, Anwesh Mazumdar, Chris Farrington, L. Sturmann, V. Coudé du Foresto, Rainer Kuschnig, F. Baudin, Caroline Barban, J. M. Matthews, A. Mérand, M. J. Goupil, P. J. Goldfinger, T. ten Brummelaar, H. A. McAlister, S. T. Ridgway, Neal J. Turner, Pierre Kervella, Eric Josselin, Pierre Demarque, Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, European Southern Observatory, Department of Astronomy, Yale University, 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), Pôle Astronomie du LESIA, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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), Center for High Angular Resolution Astronomy, Department of Physics and Astronomy, Georgia State University, Groupe de Recherches Autrichiennes et Allemandes. UHB (GRAAL), MEN : JE2314-Université de Rennes 2 (UR2), Institut für Astronomie, Universität Wien (IfA), Department of Physics and Astronomy, University of British Columbia, and National Optical Astronomy Observatory, Tucson (NOAO)

Subjects
Physics, 010308 nuclear & particles physics, Oscillation, Infrared, Red giant, Phase (waves), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, 01 natural sciences, 7. Clean energy, Asteroseismology, Luminosity, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Angular diameter, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

The GIII red giant star epsilon Oph has been found to exhibit several modes of oscillation by the MOST mission. We interpret the observed frequencies of oscillation in terms of theoretical radial p-mode frequencies of stellar models. Evolutionary models of this star, in both shell H-burning and core He-burning phases of evolution, are constructed using as constraints a combination of measurements from classical ground-based observations (for luminosity, temperature, and chemical composition) and seismic observations from MOST. Radial frequencies of models in either evolutionary phase can reproduce the observed frequency spectrum of epsilon Oph almost equally well. The best-fit models indicate a mass in the range of 1.85 +/- 0.05 Msun with radius of 10.55 +/- 0.15 Rsun. We also obtain an independent estimate of the radius of epsilon Oph using high accuracy interferometric observations in the infrared K' band, using the CHARA/FLUOR instrument. The measured limb darkened disk angular diameter of epsilon Oph is 2.961 +/- 0.007 mas. Together with the Hipparcos parallax, this translates into a photospheric radius of 10.39 +/- 0.07 Rsun. The radius obtained from the asteroseismic analysis matches the interferometric value quite closely even though the radius was not constrained during the modelling., Comment: 11 pages, accepted for publication in Astronomy & Astrophysics

Published
2009
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11. Asteroseismology of Procyon with SOPHIE

Author

B. Mosser, F. Bouchy, M. Martić, T. Appourchaux, C. Barban, G. Berthomieu, R. A. Garcia, J. C. Lebrun, E. Michel, J. Provost, F. Thévenin, S. Turck-Chièze, 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 d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), 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, 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), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Centre National d’Études Spatiales [Paris] (CNES), Université Nice Sophia Antipolis (1965 - 2019) (UNS), and 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)

Subjects
Physics, 010504 meteorology & atmospheric sciences, Spectrometer, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Asteroseismology, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Telescope, Space and Planetary Science, law, 0103 physical sciences, stars: oscillations, radial velocities, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Data reduction
Abstract

This paper reports a 9-night asteroseismic observation program conducted in January 2007 with the new spectrometer Sophie at the OHP 193-cm telescope, on the F5 IV-V target Procyon A. This first asteroseismic program with Sophie was intended to test the performance of the instrument with a bright but demanding asteroseismic target and was part of a multisite network. The Sophie spectra have been reduced with the data reduction software provided by OHP. The Procyon asteroseismic data were then analyzed with statistical tools. The asymptotic analysis has been conducted considering possible curvature in the echelle diagram analysis. These observations have proven the efficient performance of Sophie used as an asteroseismometer, and succeed in a clear detection of the large spacing. An \'echelle diagram based on the 54-$\mu$Hz spacing shows clear ridges. Identification of the peaks exhibits large spacings varying from about 52 $\mu$Hz to 56 $\mu$Hz., Comment: 7 pages, 7 figures

Published
2007
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12. Inferred acoustic rates of solarp modes from several helioseismic instruments

Author

Pierre Gouttebroze, William J. Chaplin, Thierry Appourchaux, Reza Samadi, Caroline Barban, Marie-Jo Goupil, Patrick Boumier, Frédéric Baudin, 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), 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), Pôle Astronomie du LESIA, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Observatório Astronómico, Universidade de Coimbra, Payloads and Advanced Concepts Office, ESA/ESTEC, National Solar Observatory, Tucson, and School of Physics and Astronomy, University of Birmingham

Subjects
Physics, Work (thermodynamics), Signal-to-noise ratio, Space and Planetary Science, Dispersion (optics), Mode (statistics), Astronomy and Astrophysics, Helioseismology, Astrophysics, Solar atmosphere, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Noise (radio), Excitation
Abstract

International audience; Acoustic rates of excitation of solar p modes can be estimated from observations in order to place constraints on the modelling of the excitation process and the layers where it occurs in the star. For several reasons (including a poor signal to noise ratio and mode overlap), this estimation is difficult. In this work, we use three completely independent datasets to obtain robust estimates in the solar case for l=1 modes. We also show that the height in the solar atmosphere where the modes are observed must be taken into account. Our three sets of results are shown to be consistent, particularly in the lower part of the p-mode spectrum (from 1.8 mHz to 2.8 mHz). At higher frequencies, the agreement is not as good, because of a larger dispersion of the measurements and also because of some systematic differences which might be due to observation height estimation or to a systematic influence of the noise.

Published
2005
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13. New grids of ATLAS9 atmospheres

Author

C. Barban, R. Garrido, C. Van't Veer-Menneret, M. J. Goupil, Friedrich Kupka, and Ulrike Heiter

Subjects
Physics, Convection, Stars, Quadratic equation, Square root, Space and Planetary Science, Limb darkening, Metallicity, Photometric system, Astronomy and Astrophysics, Context (language use), Astrophysics
Abstract

Using up-to-date model atmospheres (Heiter et al. 2002) with the turbulent convection approach developed by Canuto et al. (1996, CGM), quadratic, cubic and square root limb darkening coecients (LDC) are calculated with a least square fit method for the Stromgren photometric system. This is done for a sample of solar metallicity models with eective temperatures between 6000 and 8500 K and with logg between 2.5 and 4.5. A comparison is made between these LDC and the ones computed from model atmospheres using the classical mixing length prescription with a mixing length parameter = 1:25 and= 0:5. For CGM model atmospheres, the law which reproduces better the model intensity is found to be the square root one for the u band and the cubic law for thev band. The results are more complex for the b andy bands depending on the temperature and gravity of the model. Similar conclusions are reached for MLT = 0:5 models. As expected much larger dierences are found between CGM and MLT with= 1:25. In a second part, the weighted limb-darkening integrals, b', and their derivatives with respect to temperature and gravity, are then computed using the best limb-darkening law. These integrals are known to be very important in the context of photometric mode identification of non-radial pulsating stars. The eect of convection treatment on these quantities is discussed and as expected dierences in the b' coecients and derivatives computed with CGM and MLT= 0:5 are much smaller than dierences obtained between computations with CGM and MLT = 1:25.

Published
2003
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14. New δ Scuti variable in the Pleiades: HD 23628

Author

E. Michel, B. Servan, Caroline Barban, M. Chevreton, M. M. Hernandez, S. Y. Jiang, Zhongmu Li, A. Fernandez, Juan Antonio Belmonte, F. Pérez Hernández, M. Alvarez, Z. L. Liu, O. Ringot, Juan Carlos Suárez, L. Fox Machado, N. Dolez, Ye Xu, S. Pau, J. R. Fremy, A.-Y. Zhou, 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), Pôle Astronomie du LESIA, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Ingénieurs, Techniciens et Administratifs

Subjects
Physics, K-type main-sequence star, Astronomy, Astronomy and Astrophysics, Astrophysics, Light curve, Spectral line, Stars, Quality (physics), Amplitude, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Pleiades, Open cluster
Abstract

We report here the discovery of very low amplitude oscillations in the Pleiades star HD 23628. The 14-nights high quality light curve designates HD 23628 as a new member of the Scuti stars class. Amplitude spectra indicate a multi-periodic pulsation behaviour, and four pulsation frequencies have been detected so far. The frequency distribution suggests the presence of nonradial modes. Pulsation constant values of the four modes are distributed in the range corresponding to fundamental f to p4 radial modes.

Published
2002
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15. New grids of ATLAS9 atmospheres I: Influence of convection treatments on model structure and on observable quantities

Author

Friedrich Kupka, Wolfram Schmidt, C. van 't Veer-Menneret, Werner W. Weiss, R. Garrido, C. Barban, David Katz, M. J. Goupil, Ulrike Heiter, 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), Pôle Astronomie du LESIA, and 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
Physics, Convection, Plane (geometry), Metallicity, Computation, Astrophysics (astro-ph), Stellar atmosphere, FOS: Physical sciences, Astronomy and Astrophysics, Observable, Astrophysics, Effective temperature, Grid, Computational physics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present several new sets of grids of model stellar atmospheres computed with modified versions of the ATLAS9 code. Each individual set consists of several grids of models with different metallicities ranging from [M/H] = -2.0 to +1.0 dex. The grids range from 4000 to 10000 K in T_eff and from 2.0 to 5.0 dex in logg. The individual sets differ from each other and from previous ones essentially in the physics used for the treatment of the convective energy transport, in the higher vertical resolution of the atmospheres and in a finer grid in the (T_eff, logg) plane. These improvements enable the computation of derivatives of color indices accurate enough for pulsation mode identification. In addition, we show that the chosen vertical resolution is necessary and sufficient for the purpose of stellar interior modelling. To explain the physical differences between the model grids we provide a description of the currently available modifications of ATLAS9 according to their treatment of convection. Our critical analysis of the dependence of the atmospheric structure and observable quantities on convection treatment, vertical resolution and metallicity reveals that spectroscopic and photometric observations are best represented when using an inefficient convection treatment. This conclusion holds whatever convection formulation investigated here is used, i.e. MLT(alpha=0.5), CM and CGM are equivalent. We also find that changing the convection treatment can lead to a change in the effective temperature estimated from Stroemgren color indices from 200 to 400 K., Comment: 20 pages, 10 figures, accepted by A&A

Published
2002
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16. Pulsational frequencies in theδScuti stars V624 Tauri and HD 23194

Author

Zhongmu Li, M. Haywood, F. Pérez Hernández, M. Alvarez, M. Chevreton, Jingnan Guo, H. Planas, Y. Y. Liu, Caroline Barban, B. Servan, Juan Antonio Belmonte, A. Fernandez, E. Michel, L. Fox-Machado, N. Dolez, S. Pau, 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), Pôle Astronomie du LESIA, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Ingénieurs, Techniciens et Administratifs

Subjects
Physics, Stars, [SDU]Sciences of the Universe [physics], Space and Planetary Science, K-type main-sequence star, Cluster (physics), Astronomy, Astronomy and Astrophysics, Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Pleiades
Abstract

The results of the tenth multi-site campaign of the STEPHI network are reported. The δ Scuti stars V624 Tau (HD 23156) and HD 23194, belonging to the Pleiades cluster, were observed photometrically for 34 days on three continents during 1999 November–December. An overall run of 343 hours of data was collected. Seven frequencies for V624 Tau and two frequencies for HD 23194 have been found above a 99% confidence level. These results greatly improve those found in previous studies with much less data. A preliminary comparison of observed and theoretical frequencies suggests that both stars may oscillate with radial and non-radial p modes of radial orders typical among δ Scuti stars.

Published
2002
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17. δScuti stars in Praesepe

Author

M. Breger, M. Chevreton, S. Frandsen, Torben Arentoft, T. H. Dall, Z. Kołaczkowski, Sz. Barcza, C. Barban, Róbert Szabó, C. Sterken, T. Medupe, J. Nuspl, J. A. Belmonte, Mário J. P. F. G. Monteiro, J. M. Benko, G. Kopacki, S. N. Udovichenko, A. Pigulski, F. J. G. Pinheiro, E. Michel, and S. K. Gupta

Subjects
Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics, Photometry (optics), Stars, Amplitude, Character (mathematics), Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Open cluster
Abstract

We present the results of the multisite dierential CCD photometry for the two Scuti stars, BN and BV Cnc, in the open cluster Praesepe. The main objective was to identify the character of the pulsation modes in BN Cnc deriving their accurate periods, amplitudes and phases. These parameters are essential for the mode identication which uses combined photometric and spectroscopic data and is presented in the second article. For BN Cnc, six pulsation modes with amplitudes above the detection limit (0.5 mmag) were detected. Using the same CCD frames it was possible to verify the presence of the four pulsation modes in BV Cnc, the faintest of Scuti stars in Praesepe. It is shown that in this very low-amplitude pulsator, substantial amplitude variations are seen between 1997 and 1998.

Published
2001
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19. Amplitudes of solar-like oscillations in red giants: Departures from the quasi-adiabatic approximation

Author

Marc-Antoine Dupret, C. Barban, Frédéric Baudin, Kevin Belkacem, M. J. Goupil, Elisabetta Caffau, Hans-Günter Ludwig, Reza Samadi, 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 d'Astrophysique, Géophysique et Océanographie, Université de Liège, Zentrum für Astronomie der Universität Heidelberg (ZAH), 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Physique stellaire et galactique, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Red giant, QC1-999, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Eigenfunction, Adiabatic theorem, Stars, Amplitude, Astrophysics::Solar and Stellar Astrophysics, Solar-like oscillations, Astrophysics::Earth and Planetary Astrophysics, Adiabatic process, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Scaling, Astrophysics::Galaxy Astrophysics
Abstract

International audience; CoRoT and Kepler measurements reveal us that the amplitudes of solar-like oscillations detected in red giant stars scale from stars to stars in a characteristic way. This observed scaling relation is not yet fully understood but constitutes potentially a powerful diagnostic about mode physics. Quasi-adiabatic theoretical scaling relations in terms of mode amplitudes result in systematic and large differences with the measurements performed for red giant stars. The use of a non-adiabatic intensity-velocity relation derived from a non-adiabatic pulsation code significantly reduces the discrepancy with the CoRoT measurements. The origin of the remaining difference is still unknown. Departure from adiabatic eigenfunction is a very likely explanation that is investigated in the present work using a 3D hydrodynamical model of the surface layers of a representative red giant star.

Published
2013
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20. Mixed modes in red-giant stars observed with CoRoT

Author

K. Belkacem, M. J. Goupil, Frédéric Baudin, Eric Michel, Reza Samadi, Michel Auvergne, C. Barban, Marc-Antoine Dupret, Andrea Miglio, J. De Ridder, Benoit Mosser, Y. P. Elsworth, Paul G. Beck, Josefina Montalbán, Saskia Hekker, Annie Baglin, Claude Catala, Alfred F. Noels, 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), Etoile, 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)-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), Institut d'Astrophysique, Géophysique et Océanographie, Université de Liège, Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, 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), School of Physics and Astronomy, University of Birmingham, and Low Energy Astrophysics (API, FNWI)

Subjects
Red giant, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 7. Clean energy, Gravitation, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Envelope (mathematics), education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Oscillation, Autocorrelation, Astronomy and Astrophysics, Light curve, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Context. The CoRoT mission has provided thousands of red-giant light curves. The analysis of their solar-like oscillations allows us to characterize their stellar properties. Aims: Up to now, the global seismic parameters of the pressure modes have been unable to distinguish red-clump giants from members of the red-giant branch. As recently done with Kepler red giants, we intend to analyze and use the so-called mixed modes to determine the evolutionary status of the red giants observed with CoRoT. We also aim at deriving different seismic characteristics depending on evolution. Methods: The complete identification of the pressure eigenmodes provided by the red-giant universal oscillation pattern allows us to aim at the mixed modes surrounding the l = 1 expected eigenfrequencies. A dedicated method based on the envelope autocorrelation function is proposed to analyze their period separation. Results: We have identified the mixed-mode signature separation thanks to their pattern that is compatible with the asymptotic law of gravity modes. We have shown that, independent of any modeling, the g-mode spacings help to distinguish the evolutionary status of a red-giant star. We then report the different seismic and fundamental properties of the stars, depending on their evolutionary status. In particular, we show that high-mass stars of the secondary clump present very specific seismic properties. We emphasize that stars belonging to the clump were affected by significant mass loss. We also note significant population and/or evolution differences in the different fields observed by CoRoT.

Published
2011
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21. Models of red giants in the CoRoT asteroseismology fields combining asteroseismic and spectroscopic constraints

Author

Lagarde, N., primary, Miglio, A., additional, Eggenberger, P., additional, Morel, T., additional, Montalbán, J., additional, Mosser, B., additional, Rodrigues, T. S., additional, Girardi, L., additional, Rainer, M., additional, Poretti, E., additional, Barban, C., additional, Hekker, S., additional, Kallinger, T., additional, Valentini, M., additional, Carrier, F., additional, Hareter, M., additional, Mantegazza, L., additional, Elsworth, Y., additional, Michel, E., additional, and Baglin, A., additional

Published
2015
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23. Mixed modes in red giants: a window on stellar evolution

Author

Mosser, B., primary, Benomar, O., additional, Belkacem, K., additional, Goupil, M. J., additional, Lagarde, N., additional, Michel, E., additional, Lebreton, Y., additional, Stello, D., additional, Vrard, M., additional, Barban, C., additional, Bedding, T. R., additional, Deheuvels, S., additional, Chaplin, W. J., additional, De Ridder, J., additional, Elsworth, Y., additional, Montalban, J., additional, Noels, A., additional, Ouazzani, R. M., additional, Samadi, R., additional, White, T. R., additional, and Kjeldsen, H., additional

Published
2014
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24. Mixed modes in red giants: a window on stellar evolution

Author

Mathieu Vrard, M. J. Goupil, Y. P. Elsworth, Reza Samadi, S. Deheuvels, Hans Kjeldsen, Othman Benomar, William J. Chaplin, Timothy R. White, Arlette Noels, Timothy R. Bedding, Dennis Stello, C. Barban, Kevin Belkacem, Eric Michel, J. De Ridder, Benoit Mosser, Josefina Montalbán, Yveline Lebreton, R. M. Ouazzani, Nadège Lagarde, 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), School of Physics and Astronomy [Birmingham], University of Birmingham [Birmingham], Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, and Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS)

Subjects
oscillations [stars], FOS: Physical sciences, Window (geology), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Kepler, Astrophysics::Solar and Stellar Astrophysics, Asymptotic giant branch, Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, interiors [stars], [PHYS]Physics [physics], Physics, stars, evolution, oscillations, interiors, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Subgiant, Astronomy and Astrophysics, Red-giant branch, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, evolution [stars], Astrophysics::Earth and Planetary Astrophysics, Stage (hydrology)
Abstract

The detection of oscillations with a mixed character in subgiants and red giants allows us to probe the physical conditions in their cores. With these mixed modes, we aim at determining seismic markers of stellar evolution. Kepler asteroseismic data were selected to map various evolutionary stages and stellar masses. Seismic evolutionary tracks were then drawn with the combination of the frequency and period spacings. We measured the asymptotic period spacing for more than 1170 stars at various evolutionary stages. This allows us to monitor stellar evolution from the main sequence to the asymptotic giant branch and draw seismic evolutionary tracks. We present clear quantified asteroseismic definitions that characterize the change in the evolutionary stages, in particular the transition from the subgiant stage to the early red giant branch, and the end of the horizontal branch.The seismic information is so precise that clear conclusions can be drawn independently of evolution models. The quantitative seismic information can now be used for stellar modeling, especially for studying the energy transport in the helium-burning core or for specifying the inner properties of stars entering the red or asymptotic giant branches. Modeling will also allow us to study stars that are identified to be in the helium-subflash stage, high-mass stars either arriving or quitting the secondary clump, or stars that could be in the blue-loop stage., Accepted In A&A (Letter) 5 pages

Published
2014
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25. Differential asteroseismic study of seismic twins observed by CoRoT

Author

Ozel, N., primary, Mosser, B., additional, Dupret, M. A., additional, Bruntt, H., additional, Barban, C., additional, Deheuvels, S., additional, García, R. A., additional, Michel, E., additional, Samadi, R., additional, Baudin, F., additional, Mathur, S., additional, Régulo, C., additional, Auvergne, M., additional, Catala, C., additional, Morel, P., additional, and Pichon, B., additional

Published
2013
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27. Asymptotic and measured large frequency separations

Author

Mosser, B., primary, Michel, E., additional, Belkacem, K., additional, Goupil, M. J., additional, Baglin, A., additional, Barban, C., additional, Provost, J., additional, Samadi, R., additional, Auvergne, M., additional, and Catala, C., additional

Published
2013
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30. Spin down of the core rotation in red giants

Author

Mosser, B., primary, Goupil, M. J., additional, Belkacem, K., additional, Marques, J. P., additional, Beck, P. G., additional, Bloemen, S., additional, De Ridder, J., additional, Barban, C., additional, Deheuvels, S., additional, Elsworth, Y., additional, Hekker, S., additional, Kallinger, T., additional, Ouazzani, R. M., additional, Pinsonneault, M., additional, Samadi, R., additional, Stello, D., additional, García, R. A., additional, Klaus, T. C., additional, Li, J., additional, Mathur, S., additional, and Morris, R. L., additional

Published
2012
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32. Probing the core structure and evolution of red giants using gravity-dominated mixed modes observed withKepler

Author

Mosser, B., primary, Goupil, M. J., additional, Belkacem, K., additional, Michel, E., additional, Stello, D., additional, Marques, J. P., additional, Elsworth, Y., additional, Barban, C., additional, Beck, P. G., additional, Bedding, T. R., additional, De Ridder, J., additional, García, R. A., additional, Hekker, S., additional, Kallinger, T., additional, Samadi, R., additional, Stumpe, M. C., additional, Barclay, T., additional, and Burke, C. J., additional

Published
2012
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33. Modelling a high-mass red giant observed by CoRoT

Author

Baudin, F., primary, Barban, C., additional, Goupil, M. J., additional, Samadi, R., additional, Lebreton, Y., additional, Bruntt, H., additional, Morel, T., additional, Lefèvre, L., additional, Michel, E., additional, Mosser, B., additional, Carrier, F., additional, De Ridder, J., additional, Hatzes, A., additional, Hekker, S., additional, Kallinger, T., additional, Auvergne, M., additional, Baglin, A., additional, and Catala, C., additional

Published
2012
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34. Characterization of the power excess of solar-like oscillations in red giants withKepler

Author

Mosser, B., primary, Elsworth, Y., additional, Hekker, S., additional, Huber, D., additional, Kallinger, T., additional, Mathur, S., additional, Belkacem, K., additional, Goupil, M. J., additional, Samadi, R., additional, Barban, C., additional, Bedding, T. R., additional, Chaplin, W. J., additional, García, R. A., additional, Stello, D., additional, De Ridder, J., additional, Middour, C. K., additional, Morris, R. L., additional, and Quintana, E. V., additional

Published
2011
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35. Amplitudes and lifetimes of solar-like oscillations observed by CoRoT (Corrigendum)

Author

Baudin, F., primary, Barban, C., additional, Belkacem, K., additional, Hekker, S., additional, Morel, T., additional, Samadi, R., additional, Benomar, O., additional, Goupil, M.-J., additional, Carrier, F., additional, Ballot, J., additional, Deheuvels, S., additional, De Ridder, J., additional, Hatzes, A. P., additional, Kallinger, T., additional, and Weiss, W. W., additional

Published
2011
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36. Mixed modes in red-giant stars observed with CoRoT

Author

Mosser, B., primary, Barban, C., additional, Montalbán, J., additional, Beck, P. G., additional, Miglio, A., additional, Belkacem, K., additional, Goupil, M. J., additional, Hekker, S., additional, De Ridder, J., additional, Dupret, M. A., additional, Elsworth, Y., additional, Noels, A., additional, Baudin, F., additional, Michel, E., additional, Samadi, R., additional, Auvergne, M., additional, Baglin, A., additional, and Catala, C., additional

Published
2011
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38. The universal red-giant oscillation pattern

Author

Mosser, B., primary, Belkacem, K., additional, Goupil, M. J., additional, Michel, E., additional, Elsworth, Y., additional, Barban, C., additional, Kallinger, T., additional, Hekker, S., additional, De Ridder, J., additional, Samadi, R., additional, Baudin, F., additional, Pinheiro, F. J. G., additional, Auvergne, M., additional, Baglin, A., additional, and Catala, C., additional

Published
2010
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40. Red-giant seismic properties analyzed with CoRoT

Author

Mosser, B., primary, Belkacem, K., additional, Goupil, M.-J., additional, Miglio, A., additional, Morel, T., additional, Barban, C., additional, Baudin, F., additional, Hekker, S., additional, Samadi, R., additional, De Ridder, J., additional, Weiss, W., additional, Auvergne, M., additional, and Baglin, A., additional

Published
2010
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41. Interferometric radius and limb darkening of the asteroseismic red giantη Serpentis with the CHARA Array

Author

Mérand, A., primary, Kervella, P., additional, Barban, C., additional, Josselin, E., additional, Brummelaar, T. A. ten, additional, McAlister, H. A., additional, Coudé du Foresto, V., additional, Ridgway, S. T., additional, Turner, N., additional, Sturmann, J., additional, Sturmann, L., additional, Goldfinger, P. J., additional, and Farrington, C., additional

Published
2010
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42. Seismic and spectroscopic characterization of the solar-like pulsating CoRoT target HD 49385

Author

Deheuvels, S., primary, Bruntt, H., additional, Michel, E., additional, Barban, C., additional, Verner, G., additional, Régulo, C., additional, Mosser, B., additional, Mathur, S., additional, Gaulme, P., additional, Garcia, R. A., additional, Boumier, P., additional, Appourchaux, T., additional, Samadi, R., additional, Catala, C., additional, Baudin, F., additional, Baglin, A., additional, Auvergne, M., additional, Roxburgh, I. W., additional, and Pérez Hernández, F., additional

Published
2010
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44. Non-radial oscillations in the red giant HR 7349 measured by CoRoT

Author

Carrier, F., primary, De Ridder, J., additional, Baudin, F., additional, Barban, C., additional, Hatzes, A. P., additional, Hekker, S., additional, Kallinger, T., additional, Miglio, A., additional, Montalbán, J., additional, Morel, T., additional, Weiss, W. W., additional, Auvergne, M., additional, Baglin, A., additional, Catala, C., additional, Michel, E., additional, and Samadi, R., additional

Published
2009
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45. A fresh look at the seismic spectrum of HD49933: analysis of 180 days of CoRoT photometry

Author

Benomar, O., primary, Baudin, F., additional, Campante, T. L., additional, Chaplin, W. J., additional, García, R. A., additional, Gaulme, P., additional, Toutain, T., additional, Verner, G. A., additional, Appourchaux, T., additional, Ballot, J., additional, Barban, C., additional, Elsworth, Y., additional, Mathur, S., additional, Mosser, B., additional, Régulo, C., additional, Roxburgh, I. W., additional, Auvergne, M., additional, Baglin, A., additional, Catala, C., additional, Michel, E., additional, and Samadi, R., additional

Published
2009
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46. Solar-like oscillations in HD 181420: data analysis of 156 days of CoRoT data

Author

Barban, C., primary, Deheuvels, S., additional, Baudin, F., additional, Appourchaux, T., additional, Auvergne, M., additional, Ballot, J., additional, Boumier, P., additional, Chaplin, W. J., additional, García, R. A., additional, Gaulme, P., additional, Michel, E., additional, Mosser, B., additional, Régulo, C., additional, Roxburgh, I. W., additional, Verner, G., additional, Baglin, A., additional, Catala, C., additional, Samadi, R., additional, Bruntt, H., additional, Elsworth, Y., additional, and Mathur, S., additional

Published
2009
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47. Solar-like oscillations with low amplitude in the CoRoT target HD 181906

Author

García, R. A., primary, Régulo, C., additional, Samadi, R., additional, Ballot, J., additional, Barban, C., additional, Benomar, O., additional, Chaplin, W. J., additional, Gaulme, P., additional, Appourchaux, T., additional, Mathur, S., additional, Mosser, B., additional, Toutain, T., additional, Verner, G. A., additional, Auvergne, M., additional, Baglin, A., additional, Baudin, F., additional, Boumier, P., additional, Bruntt, H., additional, Catala, C., additional, Deheuvels, S., additional, Elsworth, Y., additional, Jiménez-Reyes, S. J., additional, Michel, E., additional, Pérez Hernández, F., additional, Roxburgh, I. W., additional, and Salabert, D., additional

Published
2009
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48. The CoRoT target HD 175726: an active star with weak solar-like oscillations

Author

Mosser, B., primary, Michel, E., additional, Appourchaux, T., additional, Barban, C., additional, Baudin, F., additional, Boumier, P., additional, Bruntt, H., additional, Catala, C., additional, Deheuvels, S., additional, García, R. A., additional, Gaulme, P., additional, Regulo, C., additional, Roxburgh, I., additional, Samadi, R., additional, Verner, G., additional, Auvergne, M., additional, Baglin, A., additional, Ballot, J., additional, Benomar, O., additional, and Mathur, S., additional

Published
2009
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50. Asteroseismology and interferometry of the red giant star ϵ Ophiuchi

Author

Mazumdar, A., primary, Mérand, A., additional, Demarque, P., additional, Kervella, P., additional, Barban, C., additional, Baudin, F., additional, Coudé du Foresto, V., additional, Farrington, C., additional, Goldfinger, P. J., additional, Goupil, M.-J., additional, Josselin, E., additional, Kuschnig, R., additional, McAlister, H. A., additional, Matthews, J., additional, Ridgway, S. T., additional, Sturmann, J., additional, Sturmann, L., additional, ten Brummelaar, T. A., additional, and Turner, N., additional

Published
2009
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