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Excitation of solar-like oscillations: From PMS to MS stellar models

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Abstract

The amplitude of solar-like oscillations results from a balance between excitation and damping. As in the sun, the excitation is attributed to turbulent motions that stochastically excite thep modes in the uppermost part of the convective zone. We present here a model for the excitation mechanism. Comparisons between modeled amplitudes and helio and stellar seismic constraints are presented and the discrepancies discussed. Finally the possibility and the interest of detecting such stochastically excited modes in pre-main sequence stars are also discussed.

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Authors and Affiliations

  1. Observatoire de Paris, 5 place J. Janssen, 92195, Meudon, France

    R. Samadi, M. -J. Goupil & E. Alecian

  2. Institut d’Astrophysique Spatiale, Orsay, France

    F. Baudin

  3. Center for Turbulence Research, Stanford University NASA Ames Research Center, Moffett Field, USA

    D. Georgobiani

  4. Research School of Astronomy and Astrophysics, Mt. Stromlo Observatory, Weston, Australia

    R. Trampedach

  5. Michigan State University, East Lansing, USA

    R. Stein

  6. Niels Bohr Institut, Copenhagen, Denmark

    å. Nordlund

Authors
  1. R. Samadi
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  2. M. -J. Goupil
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  3. E. Alecian
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  4. F. Baudin
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  5. D. Georgobiani
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  6. R. Trampedach
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  7. R. Stein
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  8. å. Nordlund
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Samadi, R., Goupil, M.J., Alecian, E. et al. Excitation of solar-like oscillations: From PMS to MS stellar models. J Astrophys Astron 26, 171–184 (2005). https://doi.org/10.1007/BF02702325

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  • DOI: https://doi.org/10.1007/BF02702325

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