Oscillation power as a test of stellar turbulence : Scanning the HR diagram

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.