Numeric simulation of relativistic stellar core collapse and the formation of Reissner-Nordstrom space-times

Abstract

The time evolution of a set of 22 Mo unstable charged stars that collapse is computed integrating the Einstein-Maxwell equations. The model simulate the collapse of an spherical star that had exhausted its nuclear fuel and have or acquires a net electric charge in its core while collapsing. When the charge to mass ratio is Q/M >= 1 the star do not collapse and spreads. On the other hand, it is observed a different physical behavior with a charge to mass ratio 1 > Q/ 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-Nordstrom solution that match smoothly with our interior numerical solution, thus the collapsing models forms Reissner-Nordstrom black holes.

13 pages, 13 figures, paper accepted

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Cited by in corpus (13)

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• Probing spacetime noncommutative constant via charged astrophysical black hole lensing
• Gravitational collapse of spherically symmetric plasmas in Einstein-Maxwell spacetimes
• Electron and positron pair production of compact stars
• Charged compact stellar model in Finch-Skea spacetime
• Nonadiabatic charged spherical evolution in the postquasistatic approximation
• Transverse Wave Propagation in Relativistic Two-fluid Plasmas around Reissner-Nordström-de Sitter Black Hole
• Photon emission of extremal Kerr-Newman black holes
• Spherical Gravitating Condensers in General Relativity
• Spherical symmetric dust collapse in a Vector-Tensor gravity
• Topological Phase Transitions in Superfluids Near Black Hole Horizons