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Viscosity driven instability in rotating relativistic stars

Viscosity driven instability in rotating relativistic stars
Viscosity driven instability in rotating relativistic stars
We investigate the viscosity driven instability in rotating relativistic stars by means of an iterative approach. We focus on polytropic rotating equilibrium stars and impose a m=2 perturbation in the lapse. We vary both the stiffness of the equation of state and the compactness of the star to study those effects on the value of the threshold. For a uniformly rotating star, the criterion T/W, where T is the rotational kinetic energy and W is the gravitational binding energy, mainly depends on the compactness of the star and takes values around 0.13–0.16, which differ slightly from that of Newtonian incompressible stars (~0.14). For differentially rotating stars, the critical value of T/W is found to span the range 0.17-0.25. This is significantly larger than the uniformly rotating case with the same compactness of the star. Finally we discuss a possibility of detecting gravitational waves from viscosity driven instability with ground-based interferometers.
1550-7998
084006-[13pp]
Saijo, Motoyuki
f2128aae-e896-4290-a382-d413c868a617
Gourgoulhon, Eric
38f91cd6-a44c-429d-98eb-128d92bb3e74
Saijo, Motoyuki
f2128aae-e896-4290-a382-d413c868a617
Gourgoulhon, Eric
38f91cd6-a44c-429d-98eb-128d92bb3e74

Saijo, Motoyuki and Gourgoulhon, Eric (2006) Viscosity driven instability in rotating relativistic stars. Physical Review D, 74 (8), 084006-[13pp]. (doi:10.1103/PhysRevD.74.084006).

Record type: Article

Abstract

We investigate the viscosity driven instability in rotating relativistic stars by means of an iterative approach. We focus on polytropic rotating equilibrium stars and impose a m=2 perturbation in the lapse. We vary both the stiffness of the equation of state and the compactness of the star to study those effects on the value of the threshold. For a uniformly rotating star, the criterion T/W, where T is the rotational kinetic energy and W is the gravitational binding energy, mainly depends on the compactness of the star and takes values around 0.13–0.16, which differ slightly from that of Newtonian incompressible stars (~0.14). For differentially rotating stars, the critical value of T/W is found to span the range 0.17-0.25. This is significantly larger than the uniformly rotating case with the same compactness of the star. Finally we discuss a possibility of detecting gravitational waves from viscosity driven instability with ground-based interferometers.

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Published date: 15 October 2006

Identifiers

Local EPrints ID: 43617
URI: http://eprints.soton.ac.uk/id/eprint/43617
ISSN: 1550-7998
PURE UUID: d651170c-f21a-4178-8303-10e1c2f86ee6

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Date deposited: 30 Jan 2007
Last modified: 27 Jun 2022 17:02

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Contributors

Author: Motoyuki Saijo
Author: Eric Gourgoulhon

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