Gravitational Radiation from Nonaxisymmetric Instability in a Rotating Star

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dc.creatorHouser, J. L.
dc.creatorCentrella, J. M.
dc.creatorSmith, S. C.
dc.date1994-09-27
dc.date.accessioned2026-07-07T12:33:13Z
dc.date.available2026-07-07T12:33:13Z
dc.descriptionWe present the first calculations of the gravitational radiation produced by nonaxisymmetric dynamical instability in a rapidly rotating compact star. The star deforms into a bar shape, shedding $\sim 4\%$ of its mass and $\sim 17\%$ of its angular momentum. The gravitational radiation is calculated in the quadrupole approximation. For a mass $M \sim 1.4$ M$_{\odot}$ and radius $R \sim 10$ km, the gravitational waves have frequency $\sim 4$ kHz and amplitude $h \sim 2 \times 10^{-22}$ at the distance of the Virgo Cluster. They carry off energy $ΔE/M \sim 0.1\%$ and radiate angular momentum $ΔJ/J \sim 0.7\%$.
dc.description16 pages, LaTeX with REVTEX macros, reprints available - send mailing address to scott@eagle.drexel.edu. Published: PRL 72, 1314 (1994)
dc.identifierhttps://arxiv.org/abs/gr-qc/9409057
dc.identifierhttp://arxiv.org/abs/gr-qc/9409057
dc.identifierPhys.Rev.Lett.72:1314-1317,1994
dc.identifierdoi:10.1103/PhysRevLett.72.1314
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/217050
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectAstrophysics
dc.titleGravitational Radiation from Nonaxisymmetric Instability in a Rotating Star
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