{ "id": "0909.4035", "version": "v2", "published": "2009-09-22T16:30:42.000Z", "updated": "2009-12-10T14:10:48.000Z", "title": "Gravitational wave emission from rotating superfluid neutron stars", "authors": [ "D. I. Jones" ], "comment": "19 pages, 2 figures. Typos corrected, a few clarifications and a figure added. To appear in MNRAS", "categories": [ "astro-ph.SR", "gr-qc" ], "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 $\\Omega$ and its first harmonic, $2\\Omega$. This contrasts with the conventional case where there is no pinned superfluidity, where either only the $2\\Omega$ 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 $\\Omega$ and $2\\Omega$ harmonics are searched for, even in targeted searches for waves from known pulsars which aren't observed to precess. Observation of such a two-component signal would provide evidence in favour of pinned superfluidity inside the star.", "revisions": [ { "version": "v2", "updated": "2009-12-10T14:10:48.000Z" } ], "analyses": { "keywords": [ "gravitational wave emission", "rotating superfluid neutron stars", "rotating deformed neutron star", "stellar spin frequency", "gravitational wave searches" ], "tags": [ "journal article" ], "publication": { "doi": "10.1111/j.1365-2966.2009.16059.x", "journal": "Monthly Notices of the Royal Astronomical Society", "year": 2010, "month": "Mar", "volume": 402, "number": 4, "pages": 2503 }, "note": { "typesetting": "TeX", "pages": 19, "language": "en", "license": "arXiv", "status": "editable", "inspire": 831892, "adsabs": "2010MNRAS.402.2503J" } } }