Four Quantum Conservation Laws for Black Hole Stationary Equilibrium Radiation Processes

TL;DR

This paper extends classical thermodynamics to quantum regimes for Kerr-Newman black holes, deriving four quantum conservation laws and confirming the Bekenstein-Hawking entropy relation, linking classical and quantum black hole properties.

Contribution

It introduces four quantum conservation laws for black hole equilibrium radiation and rigorously establishes the Bekenstein-Hawking entropy relation.

Findings

Four quantum conservation laws derived for Kerr-Newman black holes.

Exact proof of the Bekenstein-Hawking entropy relation.

Black hole classical entropy originates from quantum entropy of internal field quanta.

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 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.