The role of the viscous secular instability in rotating neutron stars

Details The role of the viscous secular instability in rotating neutron stars The role of the viscous secular instability in rotating neutron stars

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...317..325l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 317, June 1, 1987, p. 325-332.

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12

Magnetohydrodynamic Stability, Neutron Stars, Secular Variations, Stellar Rotation, Viscosity, Angular Velocity, Gravitational Waves

Scientific paper

For neutron stars colder than about 10 million K, the viscosity of neutron matter is so large that the well-known gravitational radiation secular instability is completely damped out by the viscosity. That instability probably does not play a role, therefore, in limiting the rotation rate of neutron stars (including possibly the 'millisecond pulsar' PSR 1937 + 214) that were spun up by accretion after they had already cooled. This paper examines the other classic secular instability, which is driven by viscosity. It is shown that the viscosity-driven secular instability can limit the rotation rate of neutron stars colder than about 100,000 K. Stars with temperatures between about 100,000 and 10 million K appear to be stable to both secular instabilities.

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