Black Hole evaporation in a thermalized final-state projection model

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dc.creatorFabbri, A.
dc.creatorPerez, A.
dc.date2006-11-14
dc.date.accessioned2026-07-07T10:42:36Z
dc.date.available2026-07-07T10:42:36Z
dc.descriptionWe 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 analyse the evaporation process in the quasi-static 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.description7 pages, 1 figure
dc.identifierhttps://arxiv.org/abs/hep-th/0611152
dc.identifierhttp://arxiv.org/abs/hep-th/0611152
dc.identifierPhys.Rev.D75:064009,2007
dc.identifierdoi:10.1103/PhysRevD.75.064009
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/182003
dc.subjectHigh Energy Physics - Theory
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectQuantum Physics
dc.titleBlack Hole evaporation in a thermalized final-state projection model
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