Conditions for Persistent Gravitational Radiation from Accreting Neutron Stars

Details Conditions for Persistent Gravitational Radiation from Accreting Neutron Stars Conditions for Persistent Gravitational Radiation from Accreting Neutron Stars

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000rmns.proge..15w&link_type=abstract

Presented at the KITP Miniprogram: R-Modes in Neutron Stars, Aug 2, 2000, Kavli Institute for Theoretical Physics, University of

Physics

Scientific paper

The gravitational-wave and accretion driven evolution of neutron stars in LMXBsis studied. If the viscosity is independent of temperature (as for mutualfriction), the amplitude of an r-mode (and the angular velocity of the neutronstar) oscillates about its equilibrium value (roughly 10^{-5}) with a period ofa few hundred years (for the maximum accretion rate). But the energy of of theoscillation (and thus the amount of over- and undershooting of the equilibriumamplitude) increases by a fractional amount per cycle of order the maximumamplitude (roughly 10^{-4}). The amplitude is greater than the equilibriumvalue for approximately 10 % of the cycle. The oscillation of the neutron startemperature is also computed. For temperature-dependent viscosity, the stabilityof the equilibrium is studied.

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