Radial geodesics as a microscopic origin of black hole entropy. I: Confined under the Schwarzschild horizon

TL;DR

This paper explores how specific radial geodesics confined within a Schwarzschild black hole horizon can account for black hole entropy, linking microscopic particle trajectories to macroscopic thermodynamic properties.

Contribution

It introduces a novel microscopic model of black hole entropy based on confined radial geodesics and their associated actions, providing a new perspective on black hole thermodynamics.

Findings

Confined radial geodesics form a thermal ensemble at Hawking temperature.

Black hole entropy is derived from the action of particles along these geodesics.

The model connects microscopic trajectories to macroscopic entropy in the large mass limit.

Abstract

Causal radial geodesics with a positive interval in the Schwarzschild metric include a subset of trajectories completely confined under a horizon, which compose a thermal statistical ensemble with the Hawking-Gibbons temperature. The Bekenstein--Hawking entropy is given by an action at corresponding geodesics of particles with a summed mass equal to that of black hole in the limit of large mass.