Thermodynamics and Evaporation of the 2+1-D Black Hole

Details Thermodynamics and Evaporation of the 2+1-D Black Hole Thermodynamics and Evaporation of the 2+1-D Black Hole

1994-03-13

arxiv.org/abs/gr-qc/9403027v1

Phys.Rev. D51 (1995) 1728-1732

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

11 pages, TAUP 2141/94, Latex

Scientific paper

10.1103/PhysRevD.51.1728

The properties of canonical and microcanonical ensembles of a black hole with thermal radiation and the problem of black hole evaporation in 3-D are studied. In 3-D Einstein-anti-de Sitter gravity we have two relevant mass scales, $m_c=1/G$, and $m_p=(\hbar^2\Lambda/G)^{1/3}$, which are particularly relevant for the evaporation problem. It is argued that in the `weak coupling' regime $\Lambda<(\hbar G)^{-2}$, the end point of an evaporating black hole formed with an initial mass $m_0>m_p$, is likely to be a stable remnant in equilibrium with thermal radiation. The relevance of these results for the information problem and for the issue of back reaction is discussed. In the `strong coupling' regime, $\Lambda>(\hbar G)^{-2}$ a full fledged quantum gravity treatment is required. Since the total energy of thermal states in anti-de Sitter space with reflective boundary conditions at spatial infinity is bounded and conserved, the canonical and microcanonical ensembles are well defined. For a given temperature or energy black hole states are locally stable. In the weak coupling regime black hole states are more probable then pure radiation states.

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