Excitation of Solar-like Oscillations: From PMS to MS Stellar Models

Davoud-Reza Samadi (1, 2, 3) , Marie-José Goupil (1, 2, 3) , Evelyne Alecian (1, 2, 3) , Frederic Baudin (4) , D. Georgobiani (5) , R. Trampedach (6) , R. Stein (7) , Å. Nordlund (8)

1 Observatoire de Paris
2 LESIA - Laboratoire d'études spatiales et d'instrumentation en astrophysique
3 Pôle Astronomie du LESIA
4 IAS - Institut d'astrophysique spatiale
5 Center for Turbulence Research, Stanford University NASA Ames Research Center
6 Mount Stromlo Observatory, Australian National University
7 Michigan State University
8 Niels Bohr Institute

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 the p modes in the upper-most 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.

Domaines: Astrophysique [astro-ph]

Davoud-Reza Samadi, Marie-José Goupil, Evelyne Alecian, Frederic Baudin, D. Georgobiani, et al.. Excitation of Solar-like Oscillations: From PMS to MS Stellar Models. Journal of Astrophysics and Astronomy, 2005, 26, pp.171. ⟨10.1007/BF02702325⟩. ⟨hal-03785661⟩