  Acoustic power and oscillation amplitudes of radial oscillations computed for
a solar model are compared with solar seismic observations. The oscillations
are assumed stochastically excited by turbulence. The numerical computations
are based upon a theoretical formulation of the power going into solar like
oscillation modes as proposed by Samadi et al. (2000) in a companion paper.
This formulation allows to investigate several assumptions concerning
properties of the stellar turbulence. We find that the entropy source plays a
dominant role in the stochastic excitation compared with the Reynold stress
source in agreement with Goldreich et al. (1994). We consider several turbulent
kinetic energy spectra suggested by different observations of the solar
granulation. Differences between turbulent spectra manifest themselves by large
differences in the computed oscillation powers at high oscillation frequency.
Two free parameters which are introduced in the description of the turbulence
enter the expression for the acoustic power. These parameters are adjusted in
order to fit to the solar observations of the surface velocity oscillations.
The best fit is obtained with the kinetic energy spectrum deduced from the
observations of the solar granulation by Nesis et al. (1993); the corresponding
adjusted parameters are found to be compatible with the theoretical upper limit
which can be set on these parameters. The adopted theoretical approach improves
the agreement between solar seismic observations and numerical results.
