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Title: Numeric simulation of relativistic stellar core collapse and the formation of Reissner-Nordstroem black holes

Abstract

The time evolution of a set of 22M{sub {center_dot}} unstable charged stars that collapse is computed integrating the Einstein-Maxwell equations. The model simulates the collapse of a spherical star that had exhausted its nuclear fuel and has or acquires a net electric charge in its core while collapsing. When the charge-to-mass ratio is Q/{radical}(G)M{>=}1, the star does not collapse but spreads. On the other hand, a different physical behavior is observed with a charge-to-mass ratio of 1>Q/{radical}(G)M>0.1. In this case, the collapsing matter forms a bubble enclosing a lower density core. We discuss an immediate astrophysical consequence of these results that is a more efficient neutrino trapping during the stellar collapse and an alternative mechanism for powerful supernova explosions. The outer space-time of the star is the Reissner-Nordstroem solution that matches smoothly with our interior numerical solution; thus the collapsing models form Reissner-Nordstroem black holes.

Authors:
;  [1]
  1. Department of Applied Mathematics, Instituto de Matematica, Estatistica e Computacao Cientifica, Universidade Estadual de Campinas, Campinas, Sao Paulo (Brazil)
Publication Date:
OSTI Identifier:
20933280
Resource Type:
Journal Article
Resource Relation:
Journal Name: Physical Review. D, Particles Fields; Journal Volume: 75; Journal Issue: 2; Other Information: DOI: 10.1103/PhysRevD.75.024020; (c) 2007 The American Physical Society; Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; BLACK HOLES; COMPUTERIZED SIMULATION; EINSTEIN-MAXWELL EQUATIONS; ELECTRIC CHARGES; MASS; NEUTRINOS; NUCLEAR FUELS; NUMERICAL SOLUTION; RELATIVISTIC RANGE; SUPERNOVAE

Citation Formats

Ghezzi, Cristian R., and Letelier, Patricio S.. Numeric simulation of relativistic stellar core collapse and the formation of Reissner-Nordstroem black holes. United States: N. p., 2007. Web. doi:10.1103/PHYSREVD.75.024020.
Ghezzi, Cristian R., & Letelier, Patricio S.. Numeric simulation of relativistic stellar core collapse and the formation of Reissner-Nordstroem black holes. United States. doi:10.1103/PHYSREVD.75.024020.
Ghezzi, Cristian R., and Letelier, Patricio S.. Mon . "Numeric simulation of relativistic stellar core collapse and the formation of Reissner-Nordstroem black holes". United States. doi:10.1103/PHYSREVD.75.024020.
@article{osti_20933280,
title = {Numeric simulation of relativistic stellar core collapse and the formation of Reissner-Nordstroem black holes},
author = {Ghezzi, Cristian R. and Letelier, Patricio S.},
abstractNote = {The time evolution of a set of 22M{sub {center_dot}} unstable charged stars that collapse is computed integrating the Einstein-Maxwell equations. The model simulates the collapse of a spherical star that had exhausted its nuclear fuel and has or acquires a net electric charge in its core while collapsing. When the charge-to-mass ratio is Q/{radical}(G)M{>=}1, the star does not collapse but spreads. On the other hand, a different physical behavior is observed with a charge-to-mass ratio of 1>Q/{radical}(G)M>0.1. In this case, the collapsing matter forms a bubble enclosing a lower density core. We discuss an immediate astrophysical consequence of these results that is a more efficient neutrino trapping during the stellar collapse and an alternative mechanism for powerful supernova explosions. The outer space-time of the star is the Reissner-Nordstroem solution that matches smoothly with our interior numerical solution; thus the collapsing models form Reissner-Nordstroem black holes.},
doi = {10.1103/PHYSREVD.75.024020},
journal = {Physical Review. D, Particles Fields},
number = 2,
volume = 75,
place = {United States},
year = {Mon Jan 15 00:00:00 EST 2007},
month = {Mon Jan 15 00:00:00 EST 2007}
}
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