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Hamiltonian treatment of the gravitational collapse of thin shells

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Autor dc.contributor.author Crisostomo J.
Autor dc.contributor.author Olea R.
Fecha Ingreso dc.date.accessioned 2014-04-05T00:14:03Z
Fecha Disponible dc.date.available 2014-04-05T00:14:03Z
Fecha en Repositorio dc.date.issued 2014-04-04
dc.identifier 10.1103/PhysRevD.69.104023
dc.description.abstract A Hamiltonian treatment of the gravitational collapse of thin shells is presented. The direct integration of the canonical constraints reproduces the standard shell dynamics for a number of known cases. The formalism is applied in detail to three-dimensional spacetime and the properties of the (2+ 1)-dimensional charged black hole collapse are further elucidated. The procedure is also extended to deal with rotating solutions in three dimensions. The general form of the equations providing the shell dynamics implies the stability of black holes, as they cannot be converted into naked singularities by any shell collapse process. © 2004 The American Physical Society. en_US
dc.source Physical Review D
Link Descarga dc.source.uri http://www.scopus.com/inward/record.url?eid=2-s2.0-3142590881&partnerID=40&md5=2760acc77f08814d22eecab4cfe8d8ba
Title dc.title Hamiltonian treatment of the gravitational collapse of thin shells en_US
Tipo dc.type Article


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