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Solving Einstein's equations for rotating spacetimes: Evolution of relativistic star clusters

Abrahams, Andrew M. and Cook, Gregory B. and Shapiro, Stuart L. and Teukolsky, Saul A. (1994) Solving Einstein's equations for rotating spacetimes: Evolution of relativistic star clusters. Physical Review D, 49 (10). pp. 5153-5164. ISSN 2470-0010.

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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.

Item Type:Article
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URLURL TypeDescription
Teukolsky, Saul A.0000-0001-9765-4526
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.
Funding AgencyGrant Number
NSFAST 91-19475
NSFPHY 90-07834
State of New YorkUNSPECIFIED
Cornell Research InstituteUNSPECIFIED
Issue or Number:10
Classification Code:PACS number(s): 04.25.Dm, 04.20.Jb, 04.30.Db, 97.60.Lf
Record Number:CaltechAUTHORS:20180719-144604603
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:88019
Deposited By: George Porter
Deposited On:19 Jul 2018 22:49
Last Modified:22 Nov 2019 09:58

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