Gravitationalwave emission from rotating gravitational collapse
Abstract
We 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 gravitationalwave energy. With sufficient rotation, the star bounces and no black hole forms. These results were obtained with a fully generalrelativistic computer code that evolves rotating axisymmetric configurations and directly computes their gravitationalradiation emission.
 Publication:

Physical Review Letters
 Pub Date:
 August 1985
 DOI:
 10.1103/PhysRevLett.55.891
 Bibcode:
 1985PhRvL..55..891S
 Keywords:

 Black Holes (Astronomy);
 Computational Astrophysics;
 Einstein Equations;
 Gravitational Collapse;
 Gravitational Waves;
 Stellar Rotation;
 Computational Grids;
 Computerized Simulation;
 Hydrodynamic Coefficients;
 Relativistic Effects;
 Astrophysics;
 95.30.Sf;
 04.30.+x;
 97.60.s;
 Relativity and gravitation;
 Late stages of stellar evolution