Black hole thermodynamics as seen through a microscopic model of a relativistic Bose gas

Abstract

Equations of gravity when projected on spacetime horizons resemble Navier-Stokes equation of a fluid with a specific equation of state [1-3]. We show that this equation of state describes massless ideal relativistic gas. We use these results, and build an explicit and simple molecular model of the fluid living on the Schwarzschild and Reissner-Nordström black hole horizons. For the spin zero Bose gas, our model makes two predictions: (i) The horizon area/entropy is quantized as given by Bekenstein's quantization rule, (ii) The model explains the correct type of proportionality between horizon area and entropy. However, for the physically relevant range of parameters, the proportionality constant is never equal to 1/4.

25 pages, v2: significantly extended v1, Reissner-Nordstrom case included

References in corpus (6)

• The physical interpretation of the spectrum of black hole quasinormal modes
• Lessons from Classical Gravity about the Quantum Structure of Spacetime
• Is gravitational entropy quantized ?
• Entropy density of spacetime and the Navier-Stokes fluid dynamics of null surfaces
• Higher Curvature Gravity and the Holographic fluid dual to flat spacetime
• Horizon spectroscopy in and beyond general relativity

Cited by in corpus (3)

• One-to-one correspondence between entanglement mechanics and black hole thermodynamics
• Hints of quantum gravity from the horizon fluid
• Statistical modeling of the fluid dual to Boulware-Deser Black hole