2000/09/12 by S. Q. Wu, X. Cai
Physics and Astronomy · #hep-th
published as Int.J.Theor.Phys. 39 (2000) 2215-2220 · 7 pages, no figure, Revtex in 12pt
arxiv created 2000/09/12 · arxiv updated 2009/11/30
The classical first law of thermodynamics for a Kerr-Newman black hole (KNBH) is generalized to a law in quantum form on the event horizon. Then four quantum conservation laws on the KNBH equilibrium radiation process are derived. The Bekenstein-Hawking relation \calS=\calA/4 is exactly established. It can be inferred that the classical entropy of black hole arises from the quantum entropy of field quanta or quasi-particles inside the hole.