Published May 15, 1994
| Published
Journal Article
Open
Solving Einstein's equations for rotating spacetimes: Evolution of relativistic star clusters
Abstract
A numerical relativity code designed to evolve rotating axisymmetric spacetimes is constructed. Both polarization states of gravitational radiation can be tracked. The source of the gravitational field is chosen to be a configuration of collisionless particles. The code is used to evaluate the stability of polytropic and toroidal star clusters. The formation of Kerr black holes by the collapse of unstable clusters is demonstrated. Unstable clusters with J/(M^2) < 1 collapse to black holes, while those with J/(M^2) > 1 collapse to new equilibrium configurations.
Additional Information
© 1994 American Physical Society. (Received 7 September 1993) This work was supported by National Science Foundation Grants Nos. AST 91-19475 and PHY 90-07834. Computations were performed at the Cornell Center for Theory and Simulation in Science and Engineering, which is supported in part by the National Science Foundation, IBM Corporation, New York State, and the Cornell Research Institute.Attached Files
Published - PhysRevD.49.5153.pdf
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PhysRevD.49.5153.pdf
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Additional details
- Eprint ID
- 88019
- Resolver ID
- CaltechAUTHORS:20180719-144604603
- AST 91-19475
- NSF
- PHY 90-07834
- NSF
- IBM Corp.
- State of New York
- Cornell Research Institute
- Created
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2018-07-19Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field