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We calculate the dynamical tides raised on a non-rotating solar-type star bya close stellar or planetary companion. Dissipation arising from a turbulentviscosity operating in the convection zone and radiative damping in theradiative core are considered. We compute the torque exerted on the star by acompanion in circular orbit, and determine the potentially observable magnitudeof the tidally induced velocity at the stellar photosphere. These calculationsare compared with the results obtained by assuming that a very small frequencylimit 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 poorapproximation at the periods of interest of several days, even when the systemis far from resonance with a normal mode. It is shown that although thecompanion may go through a succession of resonances as it spirals in under theaction of the tides, for a fixed spectrum of normal modes its migration iscontrolled essentially by the non-resonant interaction. We find that theturbulent viscosity that is required to provide the observed circularizationrates of main sequence solar-type binaries is about fifty times larger thanthat simply estimated from mixing length theory for non-rotating stars. Wediscuss the means by which this enhanced viscosity might be realized. Thesecalculations are applied to 51 Pegasi. We show that the perturbed velocityinduced by the tides at the stellar surface is too small to be observed.

On the Tidal Interaction of a Solar‐Type Star with an Orbiting Companion: Excitation ofg‐Mode Oscillation and Orbital Evolution