Charged rotating black hole formation from thin shell collapse in three dimensions

Resultado de la investigación: Article

8 Citas (Scopus)

Resumen

The thin shell collapse leading to the formation of charged rotating black holes in three dimensions is analyzed in the light of a recently developed Hamiltonian formalism for these systems. It is proposed to demand, as a way to reconcile the properties of an infinitely extended solenoid in flat space with a magnetic black hole in three dimensions, that the magnetic field should vanish just outside the shell. The adoption of this boundary condition results in an exterior solution with a magnetic field different from zero at a finite distance from the shell. The interior solution is also found and assigns another interpretation, in a different context, to the magnetic solution previously obtained by Clément and Hirschmann and Welch.

Idioma originalEnglish
Páginas (desde-hasta)2649-2665
Número de páginas17
PublicaciónModern Physics Letters A
Volumen20
N.º34
DOI
EstadoPublished - 10 nov 2005

Huella dactilar

solenoids
magnetic fields
boundary conditions
formalism

ASJC Scopus subject areas

  • Nuclear and High Energy Physics
  • Astronomy and Astrophysics

Citar esto

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abstract = "The thin shell collapse leading to the formation of charged rotating black holes in three dimensions is analyzed in the light of a recently developed Hamiltonian formalism for these systems. It is proposed to demand, as a way to reconcile the properties of an infinitely extended solenoid in flat space with a magnetic black hole in three dimensions, that the magnetic field should vanish just outside the shell. The adoption of this boundary condition results in an exterior solution with a magnetic field different from zero at a finite distance from the shell. The interior solution is also found and assigns another interpretation, in a different context, to the magnetic solution previously obtained by Cl{\'e}ment and Hirschmann and Welch.",
keywords = "Classical black holes, Einstein - Maxwell spacetimes, Gravitational collapse",
author = "Rodrigo Olea",
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Charged rotating black hole formation from thin shell collapse in three dimensions. / Olea, Rodrigo.

En: Modern Physics Letters A, Vol. 20, N.º 34, 10.11.2005, p. 2649-2665.

Resultado de la investigación: Article

TY - JOUR

T1 - Charged rotating black hole formation from thin shell collapse in three dimensions

AU - Olea, Rodrigo

PY - 2005/11/10

Y1 - 2005/11/10

N2 - The thin shell collapse leading to the formation of charged rotating black holes in three dimensions is analyzed in the light of a recently developed Hamiltonian formalism for these systems. It is proposed to demand, as a way to reconcile the properties of an infinitely extended solenoid in flat space with a magnetic black hole in three dimensions, that the magnetic field should vanish just outside the shell. The adoption of this boundary condition results in an exterior solution with a magnetic field different from zero at a finite distance from the shell. The interior solution is also found and assigns another interpretation, in a different context, to the magnetic solution previously obtained by Clément and Hirschmann and Welch.

AB - The thin shell collapse leading to the formation of charged rotating black holes in three dimensions is analyzed in the light of a recently developed Hamiltonian formalism for these systems. It is proposed to demand, as a way to reconcile the properties of an infinitely extended solenoid in flat space with a magnetic black hole in three dimensions, that the magnetic field should vanish just outside the shell. The adoption of this boundary condition results in an exterior solution with a magnetic field different from zero at a finite distance from the shell. The interior solution is also found and assigns another interpretation, in a different context, to the magnetic solution previously obtained by Clément and Hirschmann and Welch.

KW - Classical black holes

KW - Einstein - Maxwell spacetimes

KW - Gravitational collapse

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JO - Modern Physics Letters A

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