Consequences of the Non Gaussian Character of the Stochastic Excitation for Solar-type Oscillations

Our recent study, based on a 3D numerical simulation, suggested that the stochastic excitation of solar p-modes has a non gaussian nature and a non gaussian model was proposed which results in a good agreement between the computed rate P at which p-modes are excited and the solar seismic observational constraints. In the present work, we study some consequences of this non-gaussian model on the rate P at which p-modes are excited in intermediate mass stars (1M⊙ . M . 2M⊙). The non gaussian model changes substantially the spectrum of P at high frequency compared with the commonly assumed gaussian model. The largest effects on P (ν) are found for stars in the mass range ∼ 1.5 − 1.6 M⊙. They are found large enough that observatins in solar-like oscillating stars observed with space based seismology missions (e.g. COROT) will be able to confirm or reject the gaussian nature of stochastic excitation.