Excitation of Radial P-Modes in the Sun and Stars     

Robert Stein  Dali Georgobiani  Regner Trampedach  Hans-Günter Ludwig  Åke Nordlund 《Solar physics》2004,220(2):229-242

P-mode oscillations in the Sun and stars are excited stochastically by Reynolds stress and entropy fluctuations produced by convection in their outer envelopes. The excitation rate of radial oscillations of stars near the main sequence from K to F and a subgiant K IV star have been calculated from numerical simulations of their surface convection zones. P-mode excitation increases with increasing effective temperature (until envelope convection ceases in the F stars) and also increases with decreasing gravity. The frequency of the maximum excitation decreases with decreasing surface gravity.  相似文献   

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

R. Samadi  M. -J. Goupil  E. Alecian  F. Baudin  D. Georgobiani  R. Trampedach  R. Stein  å. Nordlund 《Journal of Astrophysics and Astronomy》2005,26(2-3):171-184

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.  相似文献   

Convection in stellar models     

R. Trampedach 《Astrophysics and Space Science》2010,328(1-2):213-219

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