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  A new numerical approach to the oscillation modes of relativistic stars

Andersson, N., Kokkotas, K. D., & Schutz, B. F. (1995). A new numerical approach to the oscillation modes of relativistic stars. Monthly Notices of the Royal Astronomical Society, 274, 1039-1048.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0013-731F-0 Version Permalink: http://hdl.handle.net/11858/00-001M-0000-0013-7322-6
Genre: Journal Article

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Andersson, Nils1, Author
Kokkotas, Kostas D.1, Author
Schutz, Bernard F.2, 3, Author              
Affiliations:
1External Organizations, escidoc:persistent22              
2Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, Golm, DE, escidoc:24013              
3External Organizations, Department of Physics and Astronomy, University of Wales College of Cardiff, escidoc:persistent22              

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 Abstract: The oscillation modes of a simple polytropic stellar model are studied. Using a new numerical approach (based on integration for complex coordinates) to the problem for the stellar exterior we have computed the eigenfrequencies of the highly damped w modes. The results obtained agree well with recent ones of Leins, Nollert & Soffel. Specifically, we are able to explain why several modes in this regime of the complex frequency plane could not be identified within the WKB approach of Kokkotas & Schutz. Furthermore, we have established that the 'kink' that was a prominent feature of the spectra of Kokkotas & Schutz, but which did not appear in the results of Leins et al., was a numerical artefact. Using our new numerical code we are also able to compute, for the first time, several of the slowly damped (p) modes for the considered stellar models. For very compact stars we find, somewhat surprisingly, that the damping of these modes does not decrease monotonically as one proceeds to higher oscillation frequencies. The existence of low-order modes that damp away much faster than anticipated may have implications for questions regarding stellar stability and the lifetime of gravitational-wave sources. The present results illustrate the accuracy and reliability of the complex-coordinate method and indicate that the method could prove to be of great use also in problems involving rotating stars. There is no apparent reason why the complex-coordinate approach should not extend to rotating stars, whereas it is accepted that all previous methods will fail to do so.

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 Dates: 1995-01-041995-03-08
 Publication Status: Published in print
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 Rev. Method: Peer
 Identifiers: eDoc: 60218
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Title: Monthly Notices of the Royal Astronomical Society
Source Genre: Journal
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Pages: - Volume / Issue: 274 Sequence Number: - Start / End Page: 1039 - 1048 Identifier: ISSN: 0035-8711