Schedule Mar 06, 2002
The r-Mode Instability, or: How the Coriolis Force Makes Gravitational Waves
Dr. Ben Owen, University of Wisconsin, Milwaukee
In the past four years there has been considerable excitement in the relativistic astrophysics community over the prospect that some fluid oscillations of rapidly rotating neutron stars are driven unstable by gravitational radiation reaction in astrophysically realistic conditions. This instability has been proposed as an explanation for the relatively slow spins of young neutron stars and those in low-mass x-ray binaries, and has been predicted to produce gravitational waves detectable by LIGO at a rate comparable to that of binary inspirals.

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