Near horizon thermodynamics of hairy black holes from gravitational decoupling

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.

11 pages, 8 figures

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• Hairy Kiselev Black Hole Solutions
• Vaidya and generalized Vaidya solutions by gravitational decoupling
• Gravitational decoupling and aerodynamics: black holes and analog gravity in a jet propulsion lab
• On static and rotating decoupled black holes without inner horizons
• Gravitational wave pulse and memory effects for hairy Kiselev black hole and its analogy with Bondi-Sachs formalism
• Hair imprints of the gravitational decoupling and hairy black hole spectroscopy
• Gravitational decoupling and regular hairy black holes: Geodesic stability, quasinormal modes, and thermodynamic properties
• Quantum Hairy Black Hole Formation and Horizon Quantum Mechanics