  We calculate the dynamical tides raised on a non-rotating solar-type star by
a close stellar or planetary companion. Dissipation arising from a turbulent
viscosity operating in the convection zone and radiative damping in the
radiative core are considered. We compute the torque exerted on the star by a
companion in circular orbit, and determine the potentially observable magnitude
of the tidally induced velocity at the stellar photosphere. These calculations
are compared with the results obtained by assuming that a very small frequency
limit can be taken in order to calculate the tidal response (equilibrium tide).
For a standard solar model, the latter is found to give a relatively poor
approximation at the periods of interest of several days, even when the system
is far from resonance with a normal mode. It is shown that although the
companion may go through a succession of resonances as it spirals in under the
action of the tides, for a fixed spectrum of normal modes its migration is
controlled essentially by the non-resonant interaction. We find that the
turbulent viscosity that is required to provide the observed circularization
rates of main sequence solar-type binaries is about fifty times larger than
that simply estimated from mixing length theory for non-rotating stars. We
discuss the means by which this enhanced viscosity might be realized. These
calculations are applied to 51 Pegasi. We show that the perturbed velocity
induced by the tides at the stellar surface is too small to be observed.
