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Oscillations of rapidly rotating superfluid stars

Oscillations of rapidly rotating superfluid stars
Oscillations of rapidly rotating superfluid stars
Using time evolutions of the relevant linearized equations, we study non-axisymmetric oscillations of rapidly rotating and superfluid neutron stars. We consider perturbations of Newtonian axisymmetric background configurations and account for the presence of superfluid components via the standard two-fluid model. Within the Cowling approximation, we are able to carry out evolutions for uniformly rotating stars up to the mass-shedding limit. This leads to the first detailed analysis of superfluid neutron star oscillations in the fast rotation regime, where the star is significantly deformed by the centrifugal force. For simplicity, we focus on background models where the two fluids (superfluid neutrons and protons) corotate, are in ?-equilibrium and co-exist throughout the volume of the star. We construct sequences of rotating stars for two analytical model equations of state. These models represent relatively simple generalizations of single fluid, polytropic stars. We study the effects of entrainment, rotation and symmetry energy on non-radial oscillations of these models. Our results show that entrainment and symmetry energy can have a significant effect on the rotational splitting of non-axisymmetric modes. In particular, the symmetry energy modifies the inertial mode frequencies considerably in the regime of fast rotation.
methods: numerical, stars: neutron, stars: oscillation, stars: rotation
0035-8711
951-963
Passamonti, A.
d9c7544a-5b0e-4230-9caa-f5a9a6fe9f13
Haskell, B.
a3c09067-6932-45cc-902d-3b7117ec848d
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Passamonti, A.
d9c7544a-5b0e-4230-9caa-f5a9a6fe9f13
Haskell, B.
a3c09067-6932-45cc-902d-3b7117ec848d
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304

Passamonti, A., Haskell, B. and Andersson, N. (2009) Oscillations of rapidly rotating superfluid stars. Monthly Notices of the Royal Astronomical Society, 396 (2), 951-963. (doi:10.1111/j.1365-2966.2009.14751.x).

Record type: Article

Abstract

Using time evolutions of the relevant linearized equations, we study non-axisymmetric oscillations of rapidly rotating and superfluid neutron stars. We consider perturbations of Newtonian axisymmetric background configurations and account for the presence of superfluid components via the standard two-fluid model. Within the Cowling approximation, we are able to carry out evolutions for uniformly rotating stars up to the mass-shedding limit. This leads to the first detailed analysis of superfluid neutron star oscillations in the fast rotation regime, where the star is significantly deformed by the centrifugal force. For simplicity, we focus on background models where the two fluids (superfluid neutrons and protons) corotate, are in ?-equilibrium and co-exist throughout the volume of the star. We construct sequences of rotating stars for two analytical model equations of state. These models represent relatively simple generalizations of single fluid, polytropic stars. We study the effects of entrainment, rotation and symmetry energy on non-radial oscillations of these models. Our results show that entrainment and symmetry energy can have a significant effect on the rotational splitting of non-axisymmetric modes. In particular, the symmetry energy modifies the inertial mode frequencies considerably in the regime of fast rotation.

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More information

Published date: June 2009
Keywords: methods: numerical, stars: neutron, stars: oscillation, stars: rotation

Identifiers

Local EPrints ID: 151303
URI: http://eprints.soton.ac.uk/id/eprint/151303
ISSN: 0035-8711
PURE UUID: 4b432794-7199-4ba3-b0cf-f93a8d83153f
ORCID for N. Andersson: ORCID iD orcid.org/0000-0001-8550-3843

Catalogue record

Date deposited: 10 May 2010 10:58
Last modified: 09 Jan 2022 02:57

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Contributors

Author: A. Passamonti
Author: B. Haskell
Author: N. Andersson ORCID iD

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