Owen, Benjamin J.; Lindblom, Lee Gravitational radiation from the \(r\)-mode instability. (English) Zbl 0997.83512 Classical Quantum Gravity 19, No. 7, 1247-1253 (2002). Summary: The instability in the \(r\)-modes of rotating neutron stars can (in principle) emit substantial amounts of Gravitational Radiation (GR) which might be detectable by LIGO and similar detectors. Estimates are given here of the detectability of this GR based on the nonlinear simulations of the \(r\)-mode instability by Lindblom, Tohline and Vallisneri. The burst of GR produced by the instability in the rapidly rotating \(1.4M_\odot\) neutron star in this simulation is fairly monochromatic with frequency near 960 Hz and duration about 100 s. A simple analytical expression is derived here for the optimal signal-to-noise ratio \(S/N\) for detecting the GR from this type of source. For an object located at a distance of 20 Mpc we estimate the optimal \(S/N\) to be in the range 1.2-12.0 depending on the LIGO II configuration. Cited in 1 Document MSC: 83C35 Gravitational waves 83B05 Observational and experimental questions in relativity and gravitational theory Keywords:gravitational radiation; compact stars PDFBibTeX XMLCite \textit{B. J. Owen} and \textit{L. Lindblom}, Classical Quantum Gravity 19, No. 7, 1247--1253 (2002; Zbl 0997.83512) Full Text: DOI arXiv