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Temperature dependent pulsations of superfluid neutron stars

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.
0035-8711
1776-1790
Gusakov, M.E.
4559ce25-3c6c-457b-b994-161194e66c56
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
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), 1776-1790. (doi:10.1111/j.1365-2966.2006.10982.x).

Record type: Article

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

Identifiers

Local EPrints ID: 48196
URI: http://eprints.soton.ac.uk/id/eprint/48196
ISSN: 0035-8711
PURE UUID: f5f1eec5-a152-4398-a6f4-974a9971c2e0
ORCID for N. Andersson: ORCID iD orcid.org/0000-0001-8550-3843

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Date deposited: 04 Sep 2007
Last modified: 28 Apr 2022 01:43

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Contributors

Author: M.E. Gusakov
Author: N. Andersson ORCID iD

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