Black hole thermodynamics from quantum gravity

Abstract

The semiclassical approximation is studied on hypersurfaces approaching the union of future null infinity and the event horizon on a large class of four dimensional black hole backgrounds. Quantum fluctuations in the background geometry are shown to lead to a breakdown of the semiclassical approximation in these models. The boundary of the region where the semiclassical approximation breaks down is used to define a `stretched horizon'. It is shown that the same effect that brings about the breakdown in semiclassical evolution associates a temperature and an entropy to the region behind the stretched horizon, and identifies the microstates that underlie the thermodynamical properties. The temperature defined in this way is equal to that of the black hole and the entropy is equal to the Bekenstein entropy up to a factor of order unity.

Latex, 18 pages, no figures

References in corpus (11)

• Evanescent Black Holes
• The Stretched Horizon and Black Hole Complementarity
• The Gravitational Hamiltonian, Action, Entropy, and Surface Terms
• Entropy, Area, and Black Hole Pairs
• Action and Entropy of Extreme and Non-Extreme Black Holes
• Strings, Black Holes and Lorentz Contraction
• The Off-Shell Black Hole
• Black Hole Horizons and Complementarity
• Breakdown of the semiclassical approximation at the black hole horizon
• A Note on the Semi-Classical Approximation in Quantum Gravity
• Quantum gravity effects at a black hole horizon

Cited by in corpus (6)

• Quantum Work and Information Geometry of a Quantum Myers-Perry Black Hole
• Quantum Thermodynamics of an ${\alpha }^{\prime }$-Corrected Reissner-Nordström Black Hole
• Quantum Thermodynamics of an M2-M5 Brane System
• Quantum Thermodynamics of a Quantum Sized AdS Black Hole
• Information Theoretical Approach to Detecting Quantum Gravitational Corrections
• Quantum gravity effects at a black hole horizon