Numeric simulation of relativistic stellar core collapse and the formation of ReissnerNordstroem black holes
Abstract
The time evolution of a set of 22M{sub {center_dot}} unstable charged stars that collapse is computed integrating the EinsteinMaxwell 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 chargetomass 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 chargetomass 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 spacetime of the star is the ReissnerNordstroem solution that matches smoothly with our interior numerical solution; thus the collapsing models form ReissnerNordstroem black holes.
 Authors:
 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; EINSTEINMAXWELL 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 ReissnerNordstroem 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 ReissnerNordstroem 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 ReissnerNordstroem 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 ReissnerNordstroem 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 EinsteinMaxwell 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 chargetomass 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 chargetomass 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 spacetime of the star is the ReissnerNordstroem solution that matches smoothly with our interior numerical solution; thus the collapsing models form ReissnerNordstroem 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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