Amplitudes and lifetimes of solar-like oscillations observed by CoRoT

Red-giant versus main-sequence stars

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

    Research output: Contribution to journalArticle

    Abstract

    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.

    Original languageEnglish (US)
    Article numberA84
    JournalAstronomy and Astrophysics
    Volume529
    DOIs
    StatePublished - Apr 13 2011

    Fingerprint

    solar oscillations
    giant stars
    main sequence stars
    oscillation
    life (durability)
    scaling laws
    oscillations
    red giant stars
    asteroseismology
    mass ratios
    diagram
    diagrams
    luminosity
    trends
    stars
    temperature

    Keywords

    • Asteroseismology
    • Methods: data analysis
    • Stars: oscillations

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

    Cite this

    Amplitudes and lifetimes of solar-like oscillations observed by CoRoT : Red-giant versus main-sequence stars. / Baudin, F.; Barban, C.; Belkacem, K.; Hekker, S.; Morel, T.; Samadi, R.; Benomar, Othman; Goupil, M. J.; Carrier, F.; Ballot, J.; Deheuvels, S.; De Ridder, J.; Hatzes, A. P.; Kallinger, T.; Weiss, W. W.

    In: Astronomy and Astrophysics, Vol. 529, A84, 13.04.2011.

    Research output: Contribution to journalArticle

    Baudin, F, Barban, C, Belkacem, K, Hekker, S, Morel, T, Samadi, R, Benomar, O, Goupil, MJ, Carrier, F, Ballot, J, Deheuvels, S, De Ridder, J, Hatzes, AP, Kallinger, T & Weiss, WW 2011, 'Amplitudes and lifetimes of solar-like oscillations observed by CoRoT: Red-giant versus main-sequence stars', Astronomy and Astrophysics, vol. 529, A84. https://doi.org/10.1051/0004-6361/201014037
    Baudin, F. ; Barban, C. ; Belkacem, K. ; Hekker, S. ; Morel, T. ; Samadi, R. ; Benomar, Othman ; Goupil, M. J. ; Carrier, F. ; Ballot, J. ; Deheuvels, S. ; De Ridder, J. ; Hatzes, A. P. ; Kallinger, T. ; Weiss, W. W. / Amplitudes and lifetimes of solar-like oscillations observed by CoRoT : Red-giant versus main-sequence stars. In: Astronomy and Astrophysics. 2011 ; Vol. 529.
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    abstract = "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.",
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    T1 - Amplitudes and lifetimes of solar-like oscillations observed by CoRoT

    T2 - Red-giant versus main-sequence stars

    AU - Baudin, F.

    AU - Barban, C.

    AU - Belkacem, K.

    AU - Hekker, S.

    AU - Morel, T.

    AU - Samadi, R.

    AU - Benomar, Othman

    AU - Goupil, M. J.

    AU - Carrier, F.

    AU - Ballot, J.

    AU - Deheuvels, S.

    AU - De Ridder, J.

    AU - Hatzes, A. P.

    AU - Kallinger, T.

    AU - Weiss, W. W.

    PY - 2011/4/13

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    N2 - 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.

    AB - 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.

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    KW - Methods: data analysis

    KW - Stars: oscillations

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