The effect of viscosity on neutron star oscillations

Abstract

The rate at which neutron star oscillations are damped by the presence of viscosity and thermal conductivity in the neutron matter is computed. Fully relativistic equations are used to describe the neutron star oscillations, the best available expressions are used for the dissipation coefficients in neutron matter, and the effects of superfluidity on these dissipation mechanisms are approximated. Damping times are computed for a range of neutron star masses and temperatures, and a variety of equations of state are used to describe the highest density portion of the neutron matter. The time scales computed here are used to improve previous estimates of the maximum rotation rate of neutron stars.