Microscopic Model building for Black Hole Membranes from Constraints of Symmetry

TL;DR

This paper constructs a microscopic model for black hole horizon fluids using symmetry constraints and integrable models, linking fluid dynamics, entropy quantization, and conformal field theory descriptions of black holes.

Contribution

It introduces a novel microscopic model based on the eight vertex Baxter model satisfying horizon symmetries and viscosity constraints, connecting black hole physics with integrable systems.

Findings

Model reproduces the bulk viscosity coefficient.

Derives Bekenstein's entropy quantization.

Suggests black-hole perturbations relate to perturbed CFTs.

Abstract

Einstein equations projected on black-hole horizons give rise to the equations of motion of a viscous fluid. This suggests a way to understand the microscopic degrees of freedom on the black-hole horizon by focusing on the physics of this fluid. In this talk, we shall approach this problem by building a crude microscopic model for the Horizon-fluid(HF) corresponding to asymptotically flat black-holes in 3+1 dimensions. The symmetry requirement for our model is that it should incorporate the S1 diffeo-symmetry on the black-hole horizon. The second constraint comes from the demand that the correct value of the Coefficient of the Bulk Viscosity of the HF can be deduced from the model. Both these requirements can be satisfied by an adoption of the eight vertex Baxter model on a S2 surface. We show that the adiabatic entropy quantisation proposed by Bekenstein also follows from this model. Finally, we argue the results obtained so far suggest that a perturbed black-hole can be described by a CFT perturbed by relevant operators and discuss the physical implications.