  A 3D simulation of the upper part of the solar convective zone is used to
derive constraints about the averaged and dynamic properties of solar turbulent
convection. Theses constraints are then used to compute the acoustic energy
supply rate P(nu) injected into the solar radial oscillations according to the
theoretical expression in Samadi & Goupil (2001). The result is compared with
solar seismic data. Assuming, as it is usually done, a gaussian model for the
frequency (nu) component chi_k(nu) of the model of turbulence, it is found that
the computed P(nu) is underestimated compared with the solar seismic data by a
factor ~ 2.5. A frequency analysis of the solar simulation shows that the
gaussian model indeed does not correctly model chi_k(nu) in the frequency range
where the acoustic energy injected into the solar p-modes is important (nu ~ 2
- 4 mHz). One must consider an additional non-gaussian component for chi_k(nu)
to reproduce its behavior. Computed values of P obtained with this non-gaussian
component reproduce better the solar seismic observations. This non-gaussian
component leads to a Reynolds stress contribution of the same order than the
one arising from the advection of the turbulent fluctuations of entropy by the
turbulent motions.
