stars: oscillations; methods: data analysis; asteroseismology
Abstract :
[en] Context. The advent of space-borne missions such as CoRoT or Kepler providing photometric data has brought new possibilities for asteroseismology across the H-R diagram. Solar-like oscillations are now observed in many stars, including red giants and main-sequence stars.
Aims: Based on several hundred identified pulsating red giants, we aim to characterize their oscillation amplitudes and widths. These observables are compared with those of main-sequence stars in order to test trends and scaling laws for these parameters for main-sequence stars and red giants.
Methods: An automated fitting procedure is used to analyze several hundred Fourier spectra. For each star, a modeled spectrum is fitted to the observed oscillation spectrum, and mode parameters are derived.
Results: Amplitudes and widths of red-giant solar-like oscillations are estimated for several hundred modes of oscillation. Amplitudes are relatively high (several hundred ppm) and widths relatively small (very few tenths of a μHz).
Conclusions: Widths measured in main-sequence stars show a different variation with the effective temperature from red giants. A single scaling law is derived for mode amplitudes of red giants and main-sequence stars versus their luminosity to mass ratio. However, our results suggest that two regimes may also be compatible with the observations.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Baudin, F.; Institut d'Astrophysique Spatiale, CNRS, Université Paris XI, 91405, Orsay Cedex, France
Barban, C.; LESIA, Université Pierre et Marie Curie, Université Denis Diderot, Obs. de Paris, 92195, Meudon Cedex, France
Belkacem, K.; Institut d'Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août 17, 4000, Liège, Belgium ; LESIA, Université Pierre et Marie Curie, Université Denis Diderot, Obs. de Paris, 92195, Meudon Cedex, France
Hekker, S.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium ; School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK ; Astronomical Institute "Anton Pannekoek", University of Amsterdam, Science Park 904, 1098 XH, Amsterdam, The Netherlands
Morel, Thierry ; Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE)
Samadi, R.; LESIA, Université Pierre et Marie Curie, Université Denis Diderot, Obs. de Paris, 92195, Meudon Cedex, France
Benomar, O.; Institut d'Astrophysique Spatiale, CNRS, Université Paris XI, 91405, Orsay Cedex, France
Goupil, M*-J; LESIA, Université Pierre et Marie Curie, Université Denis Diderot, Obs. de Paris, 92195, Meudon Cedex, France
Carrier, F.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
Ballot, J.; Institut de Recherche en Astrophysique et Planétologie, CNRS, Université de Toulouse, 31400, Toulouse, France
Deheuvels, S.; LESIA, Université Pierre et Marie Curie, Université Denis Diderot, Obs. de Paris, 92195, Meudon Cedex, France
De Ridder, J.; Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
Hatzes, A. P.; Thüringer Landessternwarte, 07778, Tautenburg, Germany
Kallinger, T.; University of Vienna, Institute for Astronomy,, Türkenschanzstrasse 17, 1180, Vienna, Austria ; Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC, V6T 1Z1, Canada
Weiss, W. W.; University of Vienna, Institute for Astronomy,, Türkenschanzstrasse 17, 1180, Vienna, Austria
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