Pulsation modes for increasingly relativistic polytropes
Pulsation modes for increasingly relativistic polytropes
We present the results of a numerical study of the fluid f, p and the gravitational w modes for increasingly relativistic non-rotating polytropes. The results for f and w modes are in good agreement with previous data for uniform density stars, which supports an understanding of the nature of the gravitational wave modes based on the uniform density data. We show that the p modes can become extremely long-lived for some relativistic stars. This effect is attributed to the change in the perturbed density distribution as the star becomes more compact.
radiation mechanisms: non-thermal, stars: neutron
493-496
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Kokkotas, Kostas D.
0b8bb98a-a65f-434b-855b-ec5b488b4a96
1998
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Kokkotas, Kostas D.
0b8bb98a-a65f-434b-855b-ec5b488b4a96
Andersson, Nils and Kokkotas, Kostas D.
(1998)
Pulsation modes for increasingly relativistic polytropes.
Monthly Notices of the Royal Astronomical Society, 297 (2), .
(doi:10.1046/j.1365-8711.1998.01541.x).
Abstract
We present the results of a numerical study of the fluid f, p and the gravitational w modes for increasingly relativistic non-rotating polytropes. The results for f and w modes are in good agreement with previous data for uniform density stars, which supports an understanding of the nature of the gravitational wave modes based on the uniform density data. We show that the p modes can become extremely long-lived for some relativistic stars. This effect is attributed to the change in the perturbed density distribution as the star becomes more compact.
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Published date: 1998
Keywords:
radiation mechanisms: non-thermal, stars: neutron
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Local EPrints ID: 29420
URI: http://eprints.soton.ac.uk/id/eprint/29420
ISSN: 1365-2966
PURE UUID: 6f0c062f-e043-4100-866e-adfb7e6cf012
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Date deposited: 07 Feb 2007
Last modified: 16 Mar 2024 03:01
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Author:
Kostas D. Kokkotas
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