Black-hole horizons in modified space-time structures arising from canonical quantum gravity

TL;DR

This paper investigates how quantum gravity modifications affect black hole horizons, revealing a mass threshold and small changes to Hawking radiation, with implications for black hole entropy calculations.

Contribution

It reformulates horizon definitions canonically in modified space-times and develops second-order perturbation theory to include matter back-reaction.

Findings

Identifies a mass threshold for black holes in quantum gravity models.

Finds small modifications to Hawking radiation due to quantum corrections.

Provides insights into horizon conditions relevant for black hole entropy computations.

Abstract

Several properties of canonical quantum gravity modify space-time structures, sometimes to the degree that no effective line elements exist to describe the geometry. An analysis of solutions, for instance in the context of black holes, then requires new insights. In this article, standard definitions of horizons in spherical symmetry are first reformulated canonically, and then evaluated for solutions of equations and constraints modified by inverse-triad corrections of loop quantum gravity. When possible, a space-time analysis is performed which reveals a mass threshold for black holes and small changes to Hawking radiation. For more general conclusions, canonical perturbation theory is developed to second order to include back-reaction from matter. The results shed light on the questions of whether renormalization of Newton's constant or other modifications of horizon conditions should be taken into account in computations of black-hole entropy in loop quantum gravity.