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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Black hole evaporation in a thermalized final-state projection model

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Fabbri, Alessandro; Pérez Cañellas, Armando
Aquest document és un/a article, creat/da en: 2007

Este documento está disponible también en : http://dx.doi.org/10.1103/PhysRevD.75.064009
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.

    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
http://dx.doi.org/10.1103/PhysRevD.75.064009
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