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Gravitational wave emission from rotating superfluid neutron stars

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
0035-8711
2503-2519
Jones, D.I.
b8f3e32c-d537-445a-a1e4-7436f472e160
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, 2503-2519. (doi:10.1111/j.1365-2966.2009.16059.x).

Record type: Article

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: 0035-8711
PURE UUID: 417131de-e6e3-4f3b-b81d-f73a43580bd1
ORCID for D.I. Jones: ORCID iD orcid.org/0000-0002-0117-7567

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Date deposited: 08 Apr 2010 16:03
Last modified: 10 Jan 2022 02:42

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