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Gravitational radiation from the r-mode instability

Benjamin J Owen1 and Lee Lindblom2

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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 1.4Modot 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.


PACS

04.80.Nn Gravitational wave detectors and experiments

97.60.Jd Neutron stars

MSC

83C35 Gravitational waves

Subjects

Gravitation and cosmology

Astrophysics and astroparticles

Dates

Issue 7 (7 April 2002)

Received 13 November 2001

Published 11 March 2002



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