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  Gravitational waves from pulsating stars: Evolving the perturbation equations for a relativistic star

Allen, G., Andersson, N., Kokkotas, K. D., & Schutz, B. F. (1998). Gravitational waves from pulsating stars: Evolving the perturbation equations for a relativistic star. Physical Review D., 58(12): 124012. doi:10.1103/PhysRevD.58.124012.

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Datensatz-Permalink: http://hdl.handle.net/11858/00-001M-0000-0013-7478-F Versions-Permalink: http://hdl.handle.net/11858/00-001M-0000-0013-747B-9
Genre: Zeitschriftenartikel

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e124012.pdf (Verlagsversion), 199KB
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 Urheber:
Allen, Gabrielle1, 2, Autor
Andersson, Nils3, 4, Autor
Kokkotas, Kostas D.1, 5, Autor
Schutz, Bernard F.6, Autor              
Affiliations:
1MPI for Gravitational Physics, Max Planck Society, Golm, DE, escidoc:24007              
2External Organizations, Department of Physics and Astronomy, University of Wales College of Cardiff, Cardiff CF2 3YB, United Kingdom, escidoc:persistent22              
3External Organizations, Department of Physics, Washington University, St Louis, Missouri 63130 , escidoc:persistent22              
4External Organizations, Institut für Astronomie und Astrophysik, Universität Tübingen, D-72076 Tübingen, Germany , escidoc:persistent22              
5External Organizations, Department of Physics, Aristotle University of Thessaloniki, Thessaloniki 54006, Greece, escidoc:persistent22              
6Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, Golm, DE, escidoc:24013              

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Schlagwörter: gr-qc
 Zusammenfassung: We consider the perturbations of a relativistic star as an initial-value problem. Having discussed the formulation of the problem (the perturbation equations and the appropriate boundary conditions at the center and the surface of the star) in detail, we evolve the equations numerically from several different sets of initial data. In all the considered cases, we find that the resulting gravitational waves carry the signature of several of the star’s pulsation modes. Typically, the fluid f mode, the first two p modes, and the slowest damped gravitational w mode are present in the signal. If such mode signals, from coalescing neutron stars or following a supernova, can be detected by future gravitational-wave antennae, one can hope to infer detailed information about neutron stars. Since a perturbation evolution should adequately describe the late time behavior of a dynamically excited neutron star, the present work can also be used as a benchmark test for future fully nonlinear simulations.

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 Datum: 1998-11-17
 Publikationsstatus: Online publiziert
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Titel: Physical Review D.
Genre der Quelle: Zeitschrift
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Ort, Verlag, Ausgabe: Lancaster, Pa. : Published for the American Physical Society by the American Institute of Physics
Seiten: - Band / Heft: 58 (12) Artikelnummer: 124012 Start- / Endseite: - Identifikator: ISSN: 1089-4918