Horizon Constraints and Black Hole Entropy

Details Horizon Constraints and Black Hole Entropy Horizon Constraints and Black Hole Entropy

2004-08-16

arxiv.org/abs/hep-th/0408123v3

Class.Quant.Grav.22:1303-1312,2005

Physics

High Energy Physics

High Energy Physics - Theory

11 pages, LaTeX, 1 figure; v2: slightly expanded, minor corrections, new appendix on stretched horizon; v3: new comment on cut

Scientific paper

10.1088/0264-9381/22/7/007

To ask a question about a black hole in quantum gravity, one must restrict initial or boundary data to ensure that a black hole is actually present. For two-dimensional dilaton gravity, and probably a much wider class of theories, I show that the imposition of a spacelike ``stretched horizon'' constraint modifies the algebra of symmetries, inducing a central term. Standard conformal field theory techniques then fix the asymptotic density of states, reproducing the Bekenstein-Hawking entropy. The states responsible for black hole entropy can thus be viewed as ``would-be gauge'' states that become physical because the symmetries are altered.

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