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

Andrew M. Abrahams; Gregory B. Cook; Stuart L. Shapiro; Saul A. Teukolsky

doi:10.1103/PhysRevD.49.5153

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

Andrew M. Abrahams, Gregory B. Cook, Stuart L. Shapiro, and Saul A. Teukolsky

Phys. Rev. D 49, 5153 – Published 15 May 1994

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 $\frac{J}{M^{2}} < 1$ collapse to black holes, while those with $\frac{J}{M^{2}} > 1$ collapse to new equilibrium configurations.

Received 7 September 1993

DOI:https://doi.org/10.1103/PhysRevD.49.5153

Authors & Affiliations

Andrew M. Abrahams^*, Gregory B. Cook^*, Stuart L. Shapiro^†, and Saul A. Teukolsky^‡

Center for Radiophysics and Space Research, Cornell University, Ithaca, New York 14853

^*Also at the Center for Theory and Simulation in Science and Engineering and Laboratory of Nuclear Studies, Cornell University, Ithaca, NY.
^†Also at the Departments of Astronomy and Physics, Cornell University, Ithaca, NY.
^‡Also at the Departments of Physics and Astronomy, Cornell University, Ithaca, NY.

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Vol. 49, Iss. 10 — 15 May 1994

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Physical Review D

covering particles, fields, gravitation, and cosmology