Near horizon thermodynamics of hairy black holes from gravitational decoupling

TL;DR

This paper explores the thermodynamics and horizon structure of hairy black holes created via gravitational decoupling, analyzing their stability, remanence, and Hawking radiation with quantum corrections.

Contribution

It provides a detailed analysis of the thermodynamics of hairy black holes from gravitational decoupling, including quantum corrections to Hawking radiation and stability considerations.

Findings

Hairy parameters influence black hole thermodynamics.

Horizon location can match Schwarzschild, but near-horizon physics differ.

Quantum corrections affect Hawking radiation emission.

Abstract

The horizon structure and thermodynamics of hairy spherically symmetric black holes generated by the gravitational decoupling method are carefully investigated. The temperature and heat capacity of the black hole is determined, as well as how the hairy parameters affect the thermodynamics. It allows the analysis of the thermal stability and the possible existence of a remanent black hole. We also calculate the Hawking radiation corrected by the generalized uncertainty principle. For such we consider the emission of fermions and apply the tunneling method to the generalized Dirac equation. It shows that, despite the horizon location being the same of the Schwarzschild one for a suitable choice of parameters, the physical phenomena happening near the horizon of both black holes are qualitatively different.