Implications of the r-mode instability of rotating relativistic stars
Abstract
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.
Cite
@article{arxiv.gr-qc/0102114,
title = {Implications of the r-mode instability of rotating relativistic stars},
author = {John L. Friedman and Keith H. Lockitch},
journal= {arXiv preprint arXiv:gr-qc/0102114},
year = {2017}
}
Comments
20 pages LaTeX2e (stylefile included), 6 eps figures. Review to appear in the proceedings of the 9th Marcel Grossman Meeting, World Scientific, ed. V. Gurzadyan, R. Jantzen, R. Ruffini