  The acoustic power injected by turbulent convection into solar-like
oscillations depends on the details of the turbulent spectrum. A theoretical
formulation for the oscillation power is developed which generalizes previous
ones. The formulation is first calibrated on a solar model in such a way as to
reproduce the solar seismic data. This allows to investigate different
assumptions about the stellar turbulent spectrum. We next explore consequences
of the assumed turbulent description for some potentially solar-like
oscillating stars. Large differences are found in the oscillation power of a
given star when using different turbulent spectra as well as in a star to star
comparison. Space seismic observations of such stars will be valuable for
discriminating between several turbulent models.
