Entropy of quasiblack holes

Details Entropy of quasiblack holes Entropy of quasiblack holes

2009-04-10

arxiv.org/abs/0904.1741v2

Phys.Rev.D81:064012,2010

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

20 pages, no figures. We thank the editors and referees A, B, and C of Physical Review Letters and Physical Review D for helpi

Scientific paper

10.1103/PhysRevD.81.064012

We trace the origin of the black hole entropy S replacing a black hole by a quasiblack hole. Let the boundary of a static body approach its own gravitational radius, in such a way that a quasihorizon forms. We show that if the body is thermal with the temperature taking the Hawking value at the quasihorizon limit, it follows, in the nonextremal case, from the first law of thermodynamics that the entropy approaches the Bekenstein-Hawking value S=A/4. In this setup, the key role is played by the surface stresses on the quasihorizon and one finds that the entropy comes from the quasihorizon surface. Any distribution of matter inside the surface leads to the same universal value for the entropy in the quasihorizon limit. This can be of some help in the understanding of black hole entropy. Other similarities between black holes and quasiblack holes, such as the mass formulas for both objects had been found previously. We also discuss the entropy for extremal quasiblack holes, a more subtle issue.

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