The Simplest Determination of the Thermodynamical Characteristics of Schwarzschild, Kerr Andreissner-Nordstrom Black Hole

TL;DR

This paper presents a simple, original method to determine key thermodynamical properties of Schwarzschild, Kerr, and Reissner-Nordstrom black holes, based on a quantization assumption related to horizon circumference.

Contribution

It introduces a novel, straightforward approach to derive black hole thermodynamics using a quantization condition inspired by Bohr's atomic model.

Findings

Derived Bekenstein-Hawking entropy for various black holes.

Established quantization of horizon surface area.

Calculated Hawking temperature using simple algebraic equations.

Abstract

In this work, generalizing our previous results, we determine in an original and the simplest way three most important thermodynamical characteristics (Bekenstein-Hawking entropy, Bekenstein quantization of the entropy or (outer) horizon surface area and Hawking temperature) of Schwarzschild, Kerr and Reissner-Nordstrom black hole. We start physically by assumption that circumference of black hole (outer) horizon holds the natural (integer) number of corresponding reduced Compton's wave length and use mathematically only simple algebraic equations. (It is conceptually similar to Bohr's quantization postulate in Bohr's atomic model interpreted by de Broglie relation.)