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Physics of Black Holes pp 177–208Cite as

Numerical Simulations of Black Hole Formation

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Part of the book series: Lecture Notes in Physics ((LNP,volume 769))

Abstract

Using recent advance in numerical relativity, three-dimensional simulations of the formation of black holes through gravitational collapse of rotating stars have been performed with unprecedented accuracy. In the case of rotating neutron stars, unstable to quasi-radial oscillations, the complete transition from one stationary solution of Einstein’s equations to another, including the formation of horizons and gravitational wave emission has been demonstrated. In the case of differentially rotating supermassive stars, non-axisymmetric dynamical instabilities can lead to fragmentation and prompt collapse to supermassive black holes. Here, we present a summary of recent, detailed numerical simulations by Baiotti et al.

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  1. Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece

    N. Stergioulas

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  1. Dept. of Physics, National Technical University, Zografou Campus, 157 80 Athens, Greece

    Eleftherios Papantonopoulos

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Stergioulas, N. (2009). Numerical Simulations of Black Hole Formation. In: Papantonopoulos, E. (eds) Physics of Black Holes. Lecture Notes in Physics, vol 769. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-88460-6_5

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