  There are no good predictions for the amplitudes expected from solar-like
oscillations in other stars. In the absence of a definitive model for
convection, which is thought to be the mechanism that excites these
oscillations, the amplitudes for both velocity and luminosity measurements must
be estimated by scaling from the Sun. In the case of luminosity measurements,
even this is difficult because of disagreement over the solar amplitude.
  This last point has lead us to investigate whether the luminosity amplitude
of oscillations (dL/L) can be derived from the velocity amplitude v_osc. Using
linear theory and observational data, we show that p-mode oscillations in a
large sample of pulsating stars satisfy
  (dL/L)_bol proportional to v_osc/T_eff. Using this relationship, together
with the best estimate of v_osc(Sun) = (23.4 +/- 1.4) cm/s, we estimate the
luminosity amplitude of solar oscillations at 550 nm to be dL/L = (4.7 +/- 0.3)
ppm.
  Next we discuss how to scale the amplitude of solar-like (i.e.,
convectively-powered) oscillations from the Sun to other stars. The only
predictions come from model calculations by (Christensen-Dalsgaard & Frandsen,
Sol. Phys. 82, 469). However, their grid of stellar models is not dense enough
to allow amplitude predictions for an arbitrary star. Nevertheless, although
convective theory is complicated, we might expect that the general properties
of convection -- including oscillation amplitudes -- should change smoothly
through the colour-magnitude diagram. Indeed, we find that the velocity
amplitudes predicted by the model
