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 (1 Mo < M < 2 Mo). 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 are found for stars in the mass range ~ 1.5-1.6 Mo. 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. 
R. Samadi (1,4), A. Nordlund (2), R.F. Stein (3), M.J. Goupil (4), I.   Roxburgh (1,4) ((1) Astronomy Unit, Queen Mary, Univ...