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Gravitational Radiation from Nonaxisymmetric Instability in a Rotating Star

J. L. Houser·J. M. Centrella·S. C. Smith
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Abstract

We 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 $ΔJ/J \sim 0.7\%$.

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BibTeXRIS

J. L. Houser, J. M. Centrella, S. C. Smith. 1994-09-27. Gravitational Radiation from Nonaxisymmetric Instability in a Rotating Star. https://doi.org/10.1103/physrevlett.72.1314

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