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.
Audio for this talk requires sound hardware, and RealPlayer or RealAudio
by RealNetworks.
Begin continuous audio for the whole talk:
high bandwidth or low bandwidth.
(Or, right-click to download the whole audio file.)
To begin viewing slides, click on the first slide below.
Author entry (protected)