Implications of the r-mode instability of rotating relativistic stars

Details Implications of the r-mode instability of rotating relativistic stars Implications of the r-mode instability of rotating relativistic stars

2001-02-28

arxiv.org/abs/gr-qc/0102114v2

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

20 pages LaTeX2e (stylefile included), 6 eps figures. Review to appear in the proceedings of the 9th Marcel Grossman Meeting,

Scientific paper

Several recent surprises appear dramatically to have improved the likelihood that the spin of rapidly rotating, newly formed neutron stars (and, possibly, of old stars spun up by accretion) is limited by a nonaxisymmetric instability driven by gravitational waves. Except for the earliest part of the spin-down, the axial l=m=2 mode (an r-mode) dominates the instability, and the emitted waves may be observable by detectors with the sensitivity of LIGO II. A review of these hopeful results is followed by a discussion of constraints on the instability set by dissipative mechanisms, including viscosity, nonlinear saturation, and energy loss to a magnetic field driven by differential rotation.

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