The Oscillations of Rapidly Rotating Newtonian Stellar Models. II. Dissipative Effects
Abstract
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 angularvelocity dependence of these dissipative effects on the l = m fmodes of uniformly rotating polytropes. The importance of the gravitationalradiation driven secular instability in limiting the rotation rate of neutron stars is estimated using these results.
 Publication:

The Astrophysical Journal
 Pub Date:
 May 1991
 DOI:
 10.1086/170039
 Bibcode:
 1991ApJ...373..213I
 Keywords:

 Neutron Stars;
 Rotating Plasmas;
 Stellar Models;
 Stellar Oscillations;
 Stellar Rotation;
 Angular Velocity;
 Computational Astrophysics;
 Gravitational Effects;
 Viscosity;
 Astrophysics;
 HYDRODYNAMICS;
 STARS: NEUTRON;
 STARS: PULSATION;
 STARS: ROTATION