Temperature dependent pulsations of superfluid neutron stars
Temperature dependent pulsations of superfluid neutron stars
We examine radial oscillations of superfluid neutron stars at finite internal temperatures. For this purpose, we generalize the description of relativistic superfluid hydrodynamics to the case of superfluid mixtures. We show that in a neutron star, at hydrostatic and beta-equilibrium, the redshifted temperature gradient is smoothed out by neutron superfluidity (but not by proton superfluidity). We calculate radial oscillation modes of neutron stars assuming 'frozen' nuclear composition in the pulsating matter. The resulting pulsation frequencies show a strong temperature dependence in the temperature range (0.1?1) Tcn, where Tcn is the critical temperature of neutron superfluidity. Combining our results with thermal evolution, we obtain a significant evolution of the pulsation spectrum, associated with highly efficient Cooper pairing neutrino emission, for 20 yr after superfluidity onset.
1776-1790
Gusakov, M.E.
4559ce25-3c6c-457b-b994-161194e66c56
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
November 2006
Gusakov, M.E.
4559ce25-3c6c-457b-b994-161194e66c56
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Gusakov, M.E. and Andersson, N.
(2006)
Temperature dependent pulsations of superfluid neutron stars.
Monthly Notices of the Royal Astronomical Society, 372 (4), .
(doi:10.1111/j.1365-2966.2006.10982.x).
Abstract
We examine radial oscillations of superfluid neutron stars at finite internal temperatures. For this purpose, we generalize the description of relativistic superfluid hydrodynamics to the case of superfluid mixtures. We show that in a neutron star, at hydrostatic and beta-equilibrium, the redshifted temperature gradient is smoothed out by neutron superfluidity (but not by proton superfluidity). We calculate radial oscillation modes of neutron stars assuming 'frozen' nuclear composition in the pulsating matter. The resulting pulsation frequencies show a strong temperature dependence in the temperature range (0.1?1) Tcn, where Tcn is the critical temperature of neutron superfluidity. Combining our results with thermal evolution, we obtain a significant evolution of the pulsation spectrum, associated with highly efficient Cooper pairing neutrino emission, for 20 yr after superfluidity onset.
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Published date: November 2006
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Local EPrints ID: 48196
URI: http://eprints.soton.ac.uk/id/eprint/48196
ISSN: 1365-2966
PURE UUID: f5f1eec5-a152-4398-a6f4-974a9971c2e0
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Date deposited: 04 Sep 2007
Last modified: 16 Mar 2024 03:02
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Author:
M.E. Gusakov
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