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In gravity, Bekenstein-Hawking entropy is an entropy assigned to black hole, on the basis of laws of thermodynamics and observers outside black hole. It striking property is that it is proportional to the surface area of the balck hole’s horizon.
In the context of string theory BH entropy is explained by a version of the AdS/CFT correspondence. Here every black brane solution in supergravity is the strong-coupling limit of a D-brane worldvolume QFT. After KK-reduction these black brane configurations become ordinary black holes. The entropy of the D-brane worldvolume theories on the event horizon turns out to coincide with the BH entropy of the corresponding black hole.
Detailed computations exist in particular for D1-brane/D5-brane systems. This is parts of the AdS/CFT correspondence. See (AGMOO, chapter 5).
See also string theory results applied elsewhere.
Another way to derive Bekenstein-Hawking entropy in string theory is by computing the entropy of weakly coupled open strings on D-brane configurations in flat Minkowski space which transmute as the coupling constant is increased to given (supersymmetric) black hole configurations. More on this is at black holes in string theory.
gravitational entropy
Bekenstein-Hawing entropy
Basic introductory accounts include
Robert Wald, The Thermodynamics of Black Holes (arXiv:gr-qc/9912119)
Jacob Bekenstein, Bekenstein-Hawking entropy, (2008), Scholarpedia, 3(10):7375
Further developments are in
A related controversial article that spawned a lot of discussion is
A survey of interpretation of black holes in string theory is in Chapter 5 of
See also
Discussions of the interpreation of BH entropy as entanglement entropy? include