  The turbulent viscosity of convection is believed to circularize the orbits
of close binary stars. When the tidal period is shorter than the turnover time
of the largest eddies, turbulent viscosity is believed to be suppressed. The
degree of suppression is disputed. We re-examine these beliefs via direct
perturbative calculations, linearizing the fluid equations on a turbulent
background, and by numerical integration of a chaotic dynamical system subject
to periodic forcing. We find that (i) dissipation of rapid tides is severely
suppressed; and (ii) turbulent convection does not circularize binaries while
the stars are on the main sequence. The latter conclusion seems secure (though
weaker) even without the former.
