THE OSCILLATIONS OF RAPIDLY ROTATING NEWTONIAN STELLAR MODELS .2. DISSIPATIVE EFFECTS

A method is described for determining the dissipative effects of viscosity and gravitational radiation on the modes of rapidly rotating Newtonian stellar models. Integral formulae for the dissipative imaginary parts of the frequencies (i.e., the damping or growth times) of these modes are derived. These expressions are evaluated numerically to determine the angular-velocity dependence of these dissipative effects on the l = m f-modes of uniformly rotating polytropes. The importance of the gravitational-radiation driven secular instability in limiting the rotation rate of neutron stars is estimated using these results.