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# Logarithmic correction to the Bekenstein-Hawking entropy

The Institute of Mathematical Sciences, Chennai 600 113, India.
Physical Review Letters (Impact Factor: 7.94). 03/2000; DOI:10.1103/PhysRevLett.84.5255
Source: arXiv

ABSTRACT The exact formula derived by us earlier for the entropy of a four dimensional non-rotating black hole within the quantum geometry formulation of the event horizon in terms of boundary states of a three dimensional Chern-Simons theory, is reexamined for large horizon areas. In addition to the {\it semiclassical} Bekenstein-Hawking contribution to the area obtained earlier, we find a contribution proportional to the logarithm of the area together with subleading corrections that constitute a series in inverse powers of the area.

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##### Article: Mechanics of Isolated Horizons
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ABSTRACT: A set of boundary conditions defining an undistorted, non-rotating isolated horizon are specified in general relativity. A space-time representing a black hole which is itself in equilibrium but whose exterior contains radiation admits such a horizon. However, the definition is applicable in a more general context, such as cosmological horizons. Physically motivated, (quasi-)local definitions of the mass and surface gravity of an isolated horizon are introduced and their properties analyzed. Although their definitions do not refer to infinity, these quantities assume their standard values in the static black hole solutions. Finally, using these definitions, the zeroth and first laws of black hole mechanics are established for isolated horizons. Comment: 56 pages, LaTeX2e, 7 eps figures Revised version with an improved treatment of the phase space
Classical and Quantum Gravity 07/1999; · 3.56 Impact Factor