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

R. Samadi | Zendy; M. J. Goupil | Zendy; E. Alécian | Zendy; F. Baudin | Zendy; D. Georgobiani | Zendy; Regner Trampedach | Zendy; R. F. Stein | Zendy; Åke Nordlund | Zendy

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

Author(s) -

R. Samadi,

M. J. Goupil,

E. Alécian,

F. Baudin,

D. Georgobiani,

Regner Trampedach,

R. F. Stein,

Åke Nordlund

Publication year - 2005

Publication title -

journal of astrophysics and astronomy

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 0.631

H-Index - 35

eISSN - 0973-7758

pISSN - 0250-6335

DOI - 10.1007/bf02702325

Subject(s) - physics , excitation , amplitude , astrophysics , stars , excited state , convection , turbulence , standard solar model , computational physics , convection zone , helioseismology , atomic physics , mechanics , optics , quantum mechanics , neutrino , solar neutrino , magnetic field , neutrino oscillation

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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