Gravitational waves from freely precessing neutron stars
Gravitational waves from freely precessing neutron stars
In this paper we model the gravitational wave emission of a freely precessing neutron star. The aim is to estimate likely source strengths, as a guide for gravitational wave astronomers searching for such signals. We model the star as a partly elastic, partly fluid body with quadrupolar deformations of its moment of inertia tensor. The angular amplitude of the free precession is limited by the finite breaking strain of the star's crust. The effect of internal dissipation on the star is important, with the precession angle being rapidly damped in the case of a star with an oblate deformation. We then go on to study detailed scenarios where free precession is created and/or maintained by some astrophysical mechanism. We consider the effects of accretion torques, electromagnetic torques, glitches and stellar encounters. We find that the mechanisms considered are either too weak to lead to a signal detectable by an Advanced LIGO interferometer, or occur too infrequently to give a reasonable event rate. We therefore conclude that, using our stellar model at least, free precession is not a good candidate for detection by the forthcoming laser interferometers.
203-220
Jones, D.I.
b8f3e32c-d537-445a-a1e4-7436f472e160
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
2002
Jones, D.I.
b8f3e32c-d537-445a-a1e4-7436f472e160
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Jones, D.I. and Andersson, N.
(2002)
Gravitational waves from freely precessing neutron stars.
Monthly Notices of the Royal Astronomical Society, 331 (1), .
(doi:10.1046/j.1365-8711.2002.05180.x).
Abstract
In this paper we model the gravitational wave emission of a freely precessing neutron star. The aim is to estimate likely source strengths, as a guide for gravitational wave astronomers searching for such signals. We model the star as a partly elastic, partly fluid body with quadrupolar deformations of its moment of inertia tensor. The angular amplitude of the free precession is limited by the finite breaking strain of the star's crust. The effect of internal dissipation on the star is important, with the precession angle being rapidly damped in the case of a star with an oblate deformation. We then go on to study detailed scenarios where free precession is created and/or maintained by some astrophysical mechanism. We consider the effects of accretion torques, electromagnetic torques, glitches and stellar encounters. We find that the mechanisms considered are either too weak to lead to a signal detectable by an Advanced LIGO interferometer, or occur too infrequently to give a reasonable event rate. We therefore conclude that, using our stellar model at least, free precession is not a good candidate for detection by the forthcoming laser interferometers.
This record has no associated files available for download.
More information
Published date: 2002
Identifiers
Local EPrints ID: 40539
URI: http://eprints.soton.ac.uk/id/eprint/40539
ISSN: 1365-2966
PURE UUID: 6f62afd6-a55a-456f-b7d6-268cb78ffd17
Catalogue record
Date deposited: 04 Jul 2006
Last modified: 16 Mar 2024 03:06
Export record
Altmetrics
Download statistics
Downloads from ePrints over the past year. Other digital versions may also be available to download e.g. from the publisher's website.
View more statistics
