  Solar-like oscillations are stochastically excited by turbulent convection.
In this work we investigate changes in the acoustic oscillation power spectrum
of solar-type stars by varying the treatment of convection in the equilibrium
structure and the properties of the stochastic excitation model. We consider
different stellar models computed with the standard mixing-length description
by Bohm-Vitense (1958) and with a generalized formulation of the mixing-length
approach by Gough (1976, 1977). We calculate the acoustic power generated by
the turbulent convection which is injected stochastically into the acoustic
pulsation modes.
  Large differences in the oscillation powers are obtained depending on the
choice of the assumed convection formulation. We show that the high-quality
data Eddington will provide, will allow us to distinguish between theoretical
predictions of acoustic power spectra obtained with different convection
models.
