Gravitational Radiation from Nonaxisymmetric Instability in a Rotating Star
| Autor: | S. C. Smith, Joan Centrella, Janet L. Houser |
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| Jazyk: | angličtina |
| Rok vydání: | 1994 |
| Předmět: |
Physics
Angular momentum 010308 nuclear & particles physics Gravitational wave Star (game theory) Astrophysics (astro-ph) FOS: Physical sciences General Physics and Astronomy General Relativity and Quantum Cosmology (gr-qc) Astrophysics Radius Astrophysics::Cosmology and Extragalactic Astrophysics Compact star 01 natural sciences General Relativity and Quantum Cosmology Amplitude 0103 physical sciences Quadrupole 010303 astronomy & astrophysics Energy (signal processing) |
| Popis: | 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 $\Delta E/M \sim 0.1\%$ and radiate angular momentum $\Delta J/J \sim 0.7\%$. Comment: 16 pages, LaTeX with REVTEX macros, reprints available - send mailing address to scott@eagle.drexel.edu. Published: PRL 72, 1314 (1994) |
| Databáze: | OpenAIRE |
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