Rotational modes of relativistic stars: numerical results
Rotational modes of relativistic stars: numerical results
We study the inertial modes of slowly rotating, fully relativistic compact stars. The equations that govern perturbations of both barotropic and nonbarotropic models are discussed, but we present numerical results only for the barotropic case. For barotropic stars all inertial modes are a hybrid of axial and polar perturbations. We use a spectral method to solve for such modes of various polytropic models. Our main attention is on modes that can be driven unstable by the emission of gravitational waves. Hence, we calculate the gravitational-wave growth time scale for these unstable modes and compare the results to previous estimates obtained in Newtonian gravity (i.e. using post-Newtonian radiation formulas). We find that the inertial modes are slightly stabilized by relativistic effects, but that previous conclusions concerning, e.g., the unstable r modes remain essentially unaltered when the problem is studied in full general relativity.
124010-[23pp]
Lockitch, Keith H.
e5c44256-3ae5-42e8-989b-f5d07683c3ba
Friedman, John L.
b27c1258-264f-4ec7-89e1-d02939b7dd66
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
2003
Lockitch, Keith H.
e5c44256-3ae5-42e8-989b-f5d07683c3ba
Friedman, John L.
b27c1258-264f-4ec7-89e1-d02939b7dd66
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Lockitch, Keith H., Friedman, John L. and Andersson, Nils
(2003)
Rotational modes of relativistic stars: numerical results.
Physical Review D, 68 (12), .
(doi:10.1103/PhysRevD.68.124010).
Abstract
We study the inertial modes of slowly rotating, fully relativistic compact stars. The equations that govern perturbations of both barotropic and nonbarotropic models are discussed, but we present numerical results only for the barotropic case. For barotropic stars all inertial modes are a hybrid of axial and polar perturbations. We use a spectral method to solve for such modes of various polytropic models. Our main attention is on modes that can be driven unstable by the emission of gravitational waves. Hence, we calculate the gravitational-wave growth time scale for these unstable modes and compare the results to previous estimates obtained in Newtonian gravity (i.e. using post-Newtonian radiation formulas). We find that the inertial modes are slightly stabilized by relativistic effects, but that previous conclusions concerning, e.g., the unstable r modes remain essentially unaltered when the problem is studied in full general relativity.
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Published date: 2003
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Local EPrints ID: 29452
URI: http://eprints.soton.ac.uk/id/eprint/29452
ISSN: 1550-7998
PURE UUID: 067fde5b-a8e1-4799-a37e-95b775044b72
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Date deposited: 12 May 2006
Last modified: 16 Mar 2024 03:02
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Author:
Keith H. Lockitch
Author:
John L. Friedman
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