Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aps..apr.h1001l&link_type=abstract
American Physical Society, April Meeting, April 28 - May 1, 2001 Washington, DC Bulletin of the American Physical Society, Vol.
Astronomy and Astrophysics
Astrophysics
Scientific paper
Gravitational radiation drives an instability in the r-modes of rotating stars. This instability is strong enough to cause the amplitude of these modes to grow on a timescale of tens of seconds in rapidly rotating neutron stars. Gravitational radiation emitted by these modes removes angular momentum from the star, causing it to spin down to a relatively small angular velocity on a timescale thought to be about one year. I will discuss at a pedagogical level the mechanism of gravitational radiation instability in rotating stars, the r-modes, and our present understanding of the competing dissipation mechanisms in neutron stars. I will also discuss the astrophysical implications of this mechanism for young neutron stars, and for older systems such as low mass x-ray binaries. Our current understanding of the prospects for directly detecting the gravitational radiation emitted during a spindown event will also be discussed.
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