Black hole evaporation in a spherically symmetric non-commutative space-time

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dc.creatorDi Grezia, Elisabetta
dc.creatorEsposito, Giampiero
dc.creatorMiele, Gennaro
dc.date2007-07-23
dc.date.accessioned2026-07-07T11:18:02Z
dc.date.available2026-07-07T11:18:02Z
dc.descriptionRecent work in the literature has studied the quantum-mechanical decay of a Schwarzschild-like black hole, formed by gravitational collapse, into almost-flat space-time and weak radiation at a very late time. The relevant quantum amplitudes have been evaluated for bosonic and fermionic fields, showing that no information is lost in collapse to a black hole. On the other hand, recent developments in noncommutative geometry have shown that, in general relativity, the effects of non-commutativity can be taken into account by keeping the standard form of the Einstein tensor on the left-hand side of the field equations and introducing a modified energy-momentum tensor as a source on the right-hand side. Relying on the recently obtained non-commutativity effect on a static, spherically symmetric metric, we have considered from a new perspective the quantum amplitudes in black hole evaporation. The general relativity analysis of spin-2 amplitudes has been shown to be modified by a multiplicative factor F depending on a constant non-commutativity parameter and on the upper limit R of the radial coordinate. Limiting forms of F have been derived which are compatible with the adiabatic approximation.
dc.description8 pages, Latex file with IOP macros, prepared for the QFEXT07 Conference, Leipzig, September 2007
dc.identifierhttps://arxiv.org/abs/0707.3318
dc.identifierhttp://arxiv.org/abs/0707.3318
dc.identifierJ.Phys.A41:164063,2008
dc.identifierdoi:10.1088/1751-8113/41/16/164063
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/193206
dc.subjectGeneral Relativity and Quantum Cosmology
dc.titleBlack hole evaporation in a spherically symmetric non-commutative space-time
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