Damping times for neutron star oscillations

Details Damping times for neutron star oscillations Damping times for neutron star oscillations

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...363..603c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 363, Nov. 10, 1990, p. 603-611.

Statistics

Computation

60

Computational Astrophysics, Neutron Stars, Stellar Oscillations, Gravitational Waves, Stellar Models, Stellar Rotation, Viscosity

Scientific paper

The frequencies and damping times due to (bulk and shear) viscosity and gravitational radiation reaction are computed for the lowest frequency modes of a wide range of nonrotating fully relativistic neutron star models. These computations generalize previous results by determining the effects of bulk viscosity by examining a large set of modes, and by expanding the sample of neutron star matter equations of state. These damping times play a crucial role in determining the stability of rapidly rotating neutron stars and in any model of periodic astrophysical phenomena that involves a pulsating neutron star.

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