Horizon constraints and black hole entropy
arXiv:gr-qc/0508071 · doi:10.1088/0264-9381/22/7/007
Abstract
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 as well, the imposition of a "stretched horizon" constraint alters the algebra of symmetries at the horizon, introducing a central term. Standard conformal field theory techniques can then then be used to obtain the asymptotic density of states, reproducing the Bekenstein-Hawking entropy. The microscopic states responsible for black hole entropy can thus be viewed as "would-be pure gauge" states that become physical because the symmetry is altered by the requirement that a horizon exist.
20 pages, to appear in "The Kerr spacetime: rotating black holes in general relativity," edited by S. Scott, M. Visser, and D. Wiltshire (Cambridge University Press)
References in corpus (1)
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