Gravitational wave emission from rotating superfluid neutron stars
Gravitational wave emission from rotating superfluid neutron stars
In this paper, we investigate the effect of a pinned superfluid component on the gravitational wave emission of a steadily rotating deformed neutron star. We show that the superfluid pinning allows the possibility for there to be gravitational wave emission at both the stellar spin frequency ? and its first harmonic, 2?. This contrasts with the conventional case where there is no pinned superfluidity, where either only the 2? harmonic is present or else the star undergoes precession, a feature which is not believed to be common in the known pulsar population. This work motivates the carrying out of gravitational wave searches where both the ? and 2? harmonics are searched for, even in targeted searches for waves from known pulsars which are not observed to precess. Observation of such a two-component signal would provide evidence in favour of pinned superfluidity inside the star.
gravitational waves, stellar dynamics, stars: neutron, pulsars: general, stars: rotation
2503-2519
Jones, D.I.
b8f3e32c-d537-445a-a1e4-7436f472e160
13 October 2009
Jones, D.I.
b8f3e32c-d537-445a-a1e4-7436f472e160
Jones, D.I.
(2009)
Gravitational wave emission from rotating superfluid neutron stars.
Monthly Notices of the Royal Astronomical Society, 402, .
(doi:10.1111/j.1365-2966.2009.16059.x).
Abstract
In this paper, we investigate the effect of a pinned superfluid component on the gravitational wave emission of a steadily rotating deformed neutron star. We show that the superfluid pinning allows the possibility for there to be gravitational wave emission at both the stellar spin frequency ? and its first harmonic, 2?. This contrasts with the conventional case where there is no pinned superfluidity, where either only the 2? harmonic is present or else the star undergoes precession, a feature which is not believed to be common in the known pulsar population. This work motivates the carrying out of gravitational wave searches where both the ? and 2? harmonics are searched for, even in targeted searches for waves from known pulsars which are not observed to precess. Observation of such a two-component signal would provide evidence in favour of pinned superfluidity inside the star.
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Published date: 13 October 2009
Keywords:
gravitational waves, stellar dynamics, stars: neutron, pulsars: general, stars: rotation
Organisations:
Applied Mathematics
Identifiers
Local EPrints ID: 143383
URI: http://eprints.soton.ac.uk/id/eprint/143383
ISSN: 1365-2966
PURE UUID: 417131de-e6e3-4f3b-b81d-f73a43580bd1
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Date deposited: 08 Apr 2010 16:03
Last modified: 14 Mar 2024 02:43
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