Quantum Geometry and Black Hole Entropy

Details Quantum Geometry and Black Hole Entropy Quantum Geometry and Black Hole Entropy

1997-10-01

arxiv.org/abs/gr-qc/9710007v1

Phys.Rev.Lett. 80 (1998) 904-907

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

Revtex, 8 pages, 1 figure

Scientific paper

10.1103/PhysRevLett.80.904

A `black hole sector' of non-perturbative canonical quantum gravity is introduced. The quantum black hole degrees of freedom are shown to be described by a Chern-Simons field theory on the horizon. It is shown that the entropy of a large non-rotating black hole is proportional to its horizon area. The constant of proportionality depends upon the Immirzi parameter, which fixes the spectrum of the area operator in loop quantum gravity; an appropriate choice of this parameter gives the Bekenstein-Hawking formula S = A/4*l_p^2. With the same choice of the Immirzi parameter, this result also holds for black holes carrying electric or dilatonic charge, which are not necessarily near extremal.

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