  Excitation of solar-like oscillations is attributed to turbulent convection
and takes place at the upper-most part of the outer convective zones.
Amplitudes of these oscillations depend on the efficiency of the excitation
processes as well as on the properties of turbulent convection. We present past
and recent improvements on the modeling of those processes. We show how the
mode amplitudes and mode line-widths can bring information about the turbulence
in the specific cases of the Sun and Alpha Cen A.
