Gravitational-wave emission from rotating gravitational collapse

Details Gravitational-wave emission from rotating gravitational collapse Gravitational-wave emission from rotating gravitational collapse

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985phrvl..55..891s&link_type=abstract

Physical Review Letters (ISSN 0031-9007), vol. 55, Aug. 19, 1985, p. 891-894.

Statistics

Computation

164

Black Holes (Astronomy), Computational Astrophysics, Einstein Equations, Gravitational Collapse, Gravitational Waves, Stellar Rotation, Computational Grids, Computerized Simulation, Hydrodynamic Coefficients, Relativistic Effects

Scientific paper

The authors present results for the gravitational radiation from the collapse to a black hole of rotating relativistic polytropes. The wave form closely resembles that emitted by a test particle infalling into a black hole, but the amplitude is reduced and opposite in sign. Less than 0.07% of the star's mass is converted to gravitational-wave energy. With sufficient rotation, the star bounces and no black hole forms. These results were obtained with a fully general-relativistic computer code that evolves rotating axisymmetric configurations and directly computes their gravitational-radiation emission.

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