Saturation of the R-mode Instability

Details Saturation of the R-mode Instability Saturation of the R-mode Instability

2002-02-19

arxiv.org/abs/astro-ph/0202345v2

Astrophys.J.591:1129-1151,2003

Astronomy and Astrophysics

Astrophysics

34 pages. 6 figures. Accepted at ApJ

Scientific paper

10.1086/374657

Rossby waves (r-modes) in rapidly rotating neutron stars are unstable because of the emission of gravitational radiation. We study saturation of this instability by nonlinear transfer of energy to stellar "inertial" oscillation modes. We present detailed calculations of stellar inertial modes in the WKB limit, their linear damping by bulk and shear viscosity, and the nonlinear coupling forces among these modes. The saturation amplitude is derived in the extreme limits of strong or weak driving by radiation reaction, as compared to the damping rate of low order inertial modes. We find the saturation energy is {\it extremely small}, at least four orders of magnitude smaller than that found by previous investigators. We discuss the consequences of this result for spin evolution of young neutron stars, and neutron stars being spun up by accretion in Low Mass X-ray Binaries.We also discuss the detection of these gravitational waves by LIGO.

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