Four Quantum Conservation Laws for Black Hole Stationary Equilibrium Radiation Processes

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dc.creatorWu, S. Q.
dc.creatorCai, X.
dc.date2000-09-12
dc.date.accessioned2026-07-07T04:10:30Z
dc.date.available2026-07-07T04:10:30Z
dc.descriptionThe 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 ${\cal{S}}={\cal{A}}/4$ 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.
dc.description7 pages, no figure, Revtex in 12pt
dc.identifierhttps://arxiv.org/abs/hep-th/0009088
dc.identifierhttp://arxiv.org/abs/hep-th/0009088
dc.identifierInt.J.Theor.Phys. 39 (2000) 2215-2220
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/50233
dc.subjectHigh Energy Physics - Theory
dc.titleFour Quantum Conservation Laws for Black Hole Stationary Equilibrium Radiation Processes
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