  We compute the rates P at which energy is injected into the p modes for a set
of 3D simulations of outer layers of stars.
  We found that Pmax - the maximum in P - scales as (L/M)^s where s is the
slope of the power law, L and M are the luminosity and the mass of the 1D
stellar models associated with the simulations. The slope is found to depend
significantly on the adopted representation for the turbulent eddy-time
correlation function, chi_k. According to the expected performances of COROT,
it will likely be possible to measure Pmax as a function of L/M and to
constrain the properties of stellar turbulence as the turbulent eddy
time-correlation.
