Physics
Scientific paper
Sep 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007phrvd..76f4035s&link_type=abstract
Physical Review D, vol. 76, Issue 6, id. 064035
Physics
12
Numerical Relativity, Gravitational Waves: Theory, Relativistic Stars: Structure, Stability, And Oscillations
Scientific paper
We present a formulation for computing equilibria composed of a rotating black hole and a massive self-gravitating torus in general relativity. Such a system is a plausible outcome formed after stellar core collapse of massive and supermassive stars as well as after a merger of a black hole-neutron star binary. In our formulation, the black hole is modeled in the puncture framework. The numerical solutions for equilibria are computed for rapidly rotating black holes and for a wide range of mass ratio of the black hole and torus. The equilibria obtained in this paper can be used for studying nonaxisymmetric instabilities, runaway instability, and magnetorotational instability of a self-gravitating accretion torus around a rotating black hole in numerical relativity. We also remark that the relation among the area, mass, and spin of rotating black holes are slightly modified by the torus.
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