Schedule Aug 2, 2000
Conditions for Persistent Gravitational Radiation from Accreting Neutron Stars
Robert Wagoner (Stanford Univ)
The gravitational-wave and accretion driven evolution of neutron stars in LMXBs is studied. If the viscosity is independent of temperature (as for mutual friction), the amplitude of an r-mode (and the angular velocity of the neutron star) oscillates about its equilibrium value (roughly 10^{-5}) with a period of a few hundred years (for the maximum accretion rate). But the energy of of the oscillation (and thus the amount of over- and undershooting of the equilibrium amplitude) increases by a fractional amount per cycle of order the maximum amplitude (roughly 10^{-4}). The amplitude is greater than the equilibrium value for approximately 10 % of the cycle. The oscillation of the neutron star temperature is also computed. For temperature-dependent viscosity, the stability of the equilibrium is studied.

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