Gravitational radiation from the r-mode instability

Benjamin J. Owen, Lee Lindblom

Research output: Contribution to journalArticle

31 Scopus citations

Abstract

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 non-linear 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 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.

Original languageEnglish
Pages (from-to)1247-1253
Number of pages7
JournalClassical and Quantum Gravity
Volume19
Issue number7
DOIs
StatePublished - Apr 7 2002

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