Stars with substantial outer convective envelopes are expected to
exhibit p-mode oscillations just as we observe on the Sun.
We investigate how the excitation and damping rates of the oscillations,
and hence the amplitudes of the resonant modes, might
scale with stellar mass, particularly for later-type stars with
masses somewhat smaller than that 1 M_o. We show how, with not
unreasonable sized space-borne detectors, oscillations of such stars
can be measured and we review the astrophysics that will be achieved with
such a space mission.