Abstract
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 quantumconservation laws on the KNBH equilibrium radiation process are derived. TheBekenstein–Hawking relation S = A/4 is exactly established. It can be inferredthat the classical entropy of black hole arises from the quantum entropy of fieldquanta or quasiparticles inside the hole.
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Wu, S.Q., Cai, X. Four Quantum Conservation Laws for Black Hole Stationary Equilibrium Radiation Processes. International Journal of Theoretical Physics 39, 2215–2220 (2000). https://doi.org/10.1023/A:1003707930057
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DOI: https://doi.org/10.1023/A:1003707930057