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Quantum Geometry and Black Hole Entropy

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arxiv gr-qc/9710007 v1 pith:R33NSO5Z submitted 1997-10-01 gr-qc hep-th

A. Ashtekar , J. Baez , A. Corichi , K. Krasnov This is my paper
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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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Cited by 11 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Expansion operators in spherically symmetric loop quantum gravity

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    For the Simpson-Visser regular black hole, the heat capacity diverges at a = √2 m, but the claimed quantum entropy corrections are internally inconsistent: the 1/a² term has the wrong sign and the remnant-entropy form...

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  11. Black Holes, Entanglement and Decoherence

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    Satishchandran reviews three equivalent mechanisms by which black holes and other Killing horizons decohere nearby quantum superpositions, via interior entanglement, soft radiation, and fluctuating multipoles.

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