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

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

2007-07-23

arxiv.org/abs/0707.3318v1

J.Phys.A41:164063,2008

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

8 pages, Latex file with IOP macros, prepared for the QFEXT07 Conference, Leipzig, September 2007

Scientific paper

10.1088/1751-8113/41/16/164063

Recent 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.

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