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Black hole evaporation in a thermalized final-state projection model

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Black hole evaporation in a thermalized final-state projection model

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dc.contributor.author Fabbri, Alessandro
dc.contributor.author Pérez Cañellas, Armando
dc.date.accessioned 2014-02-18T12:19:52Z
dc.date.available 2014-02-18T12:19:52Z
dc.date.issued 2007
dc.identifier.citation Fabbri, Alessandro Pérez Cañellas, Armando 2007 Black hole evaporation in a thermalized final-state projection model Physical Review D 75 6 064009-1 064009-4
dc.identifier.uri http://hdl.handle.net/10550/33039
dc.description.abstract We propose a modified version of the Horowitz-Maldacena final-state boundary condition based upon a matter-radiation thermalization hypothesis on the Black Hole interior, which translates into a particular entangled state with thermal Schmidt coefficients. We investigate the consequences of this proposal for matter entering the horizon, as described by a Canonical density matrix characterized by the matter temperature T. The emitted radiation is explicitly calculated and is shown to follow a thermal spectrum with an effective temperature T-eff. We analyze the evaporation process in the quasistatic approximation, highlighting important differences in the late stages with respect to the usual semiclassical evolution, and calculate the fidelity of the emitted Hawking radiation relative to the infalling matter.
dc.relation.ispartof Physical Review D, 2007, vol. 75, num. 6, p. 064009-1-064009-4
dc.subject Astronomia
dc.title Black hole evaporation in a thermalized final-state projection model
dc.type journal article es_ES
dc.date.updated 2014-02-18T12:19:52Z
dc.identifier.doi 10.1103/PhysRevD.75.064009
dc.identifier.idgrec 041266
dc.rights.accessRights open access es_ES
dc.identifier.url 10.1103/PhysRevD.75.064009

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