The University of Southampton
University of Southampton Institutional Repository

Lagrangian perturbation theory of nonrelativistic superfluid stars

Lagrangian perturbation theory of nonrelativistic superfluid stars
Lagrangian perturbation theory of nonrelativistic superfluid stars
We develop a Lagrangian perturbation framework for rotating non-relativistic superfluid neutron stars. This leads to the first generalization of classic work on the stability properties of rotating stars to models that account for the presence of potentially weakly coupled superfluid components. Our analysis is based on the standard two-fluid model expected to be relevant for the conditions that prevail in the outer core of mature neutron stars. We discuss the implications of our results for dynamic and secular instabilities of a simple neutron star model in which the two fluids are allowed to assume different (uniform) rotation rates.
0035-8711
918-928
Comer, G.L.
f2c1746c-8638-4268-94f0-e5d4375f0358
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Grosart, K.
28b596cf-e3eb-4e68-b218-22a40af9274f
Comer, G.L.
f2c1746c-8638-4268-94f0-e5d4375f0358
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Grosart, K.
28b596cf-e3eb-4e68-b218-22a40af9274f

Comer, G.L., Andersson, N. and Grosart, K. (2004) Lagrangian perturbation theory of nonrelativistic superfluid stars. Monthly Notices of the Royal Astronomical Society, 355 (4), 918-928. (doi:10.1111/j.1365-2966.2004.08370.x).

Record type: Article

Abstract

We develop a Lagrangian perturbation framework for rotating non-relativistic superfluid neutron stars. This leads to the first generalization of classic work on the stability properties of rotating stars to models that account for the presence of potentially weakly coupled superfluid components. Our analysis is based on the standard two-fluid model expected to be relevant for the conditions that prevail in the outer core of mature neutron stars. We discuss the implications of our results for dynamic and secular instabilities of a simple neutron star model in which the two fluids are allowed to assume different (uniform) rotation rates.

Full text not available from this repository.

More information

Published date: December 2004

Identifiers

Local EPrints ID: 29461
URI: https://eprints.soton.ac.uk/id/eprint/29461
ISSN: 0035-8711
PURE UUID: fc24f5e7-9fc8-4bd3-ad5f-a091e3d645b7
ORCID for N. Andersson: ORCID iD orcid.org/0000-0001-8550-3843

Catalogue record

Date deposited: 11 May 2006
Last modified: 18 May 2019 00:37

Export record

Altmetrics

Download statistics

Downloads from ePrints over the past year. Other digital versions may also be available to download e.g. from the publisher's website.

View more statistics

Atom RSS 1.0 RSS 2.0

Contact ePrints Soton: eprints@soton.ac.uk

ePrints Soton supports OAI 2.0 with a base URL of https://eprints.soton.ac.uk/cgi/oai2

This repository has been built using EPrints software, developed at the University of Southampton, but available to everyone to use.

We use cookies to ensure that we give you the best experience on our website. If you continue without changing your settings, we will assume that you are happy to receive cookies on the University of Southampton website.

×