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• W2012806360 abstract "We present a numerical code designed to study astrophysical phenomena involving dynamical spacetimes containing black holes in the presence of relativistic hydrodynamic matter. We present evolutions of the collapse of a fluid star from the onset of collapse to the settling of the resulting black hole to a final stationary state. In order to evolve stably after the black hole forms, we excise a region inside the hole before a singularity is encountered. This excision region is introduced after the appearance of an apparent horizon, but while a significant amount of matter remains outside the hole. We test our code by evolving accurately a vacuum Schwarzschild black hole, a relativistic Bondi accretion flow onto a black hole, Oppenheimer-Snyder dust collapse, and the collapse of nonrotating and rotating stars. These systems are tracked reliably for hundreds of M following excision, where M is the mass of the black hole. We perform these tests both in axisymmetry and in full 3+1 dimensions. We then apply our code to study the effect of the stellar spin parameter J/M^2 on the final outcome of gravitational collapse of rapidly rotating n = 1 polytropes. We find that a black hole forms only if J/M^2<1, in agreement with previous simulations. When J/M^2>1, the collapsing star forms a torus which fragments into nonaxisymmetric clumps, capable of generating appreciable ``splash'' gravitational radiation." @default.
• W2012806360 created "2016-06-24" @default.
• W2012806360 creator A5034590981 @default.
• W2012806360 creator A5050217771 @default.
• W2012806360 creator A5087240601 @default.
• W2012806360 date "2004-05-18" @default.
• W2012806360 modified "2023-09-23" @default.
• W2012806360 title "Relativistic hydrodynamic evolutions with black hole excision" @default.
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• W2012806360 doi "https://doi.org/10.1103/physrevd.69.104016" @default.
• W2012806360 hasPublicationYear "2004" @default.

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