  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.
