Abstract
We review (anti)evaporation phenomena within the context of quantum gravity and extended theories of gravity. The (anti)evaporation effect is an instability of the black hole horizon discovered in many different scenarios: quantum dilaton-gravity, f ( R ) -gravity, f ( T ) -gravity, string-inspired black holes, and brane-world cosmology. Evaporating and antievaporating black holes seem to have completely different thermodynamical features compared to standard semiclassical black holes. The purpose of this review is to provide an introduction to conceptual and technical aspects of (anti)evaporation effects, while discussing problems that are still open.
Highlights
The long-standing idea to extend the standard model of Einsteinian gravity—general relativity (GR)—
We review aspects of the instabilities of a class of black hole solutions, which appear universally in these aforementioned classes of extended theories of gravity, and are dubbedevaporation instabilities. (Anti)evaporation phenomena consist of the exponentially decreasing radius of the black hole horizon
These were first discovered by Bousso and Hawking within the context of quantum dilaton-gravity (e.g., Ref. [18]), and elaborated in Refs. [19,20,21]
Summary
The long-standing idea to extend the standard model of Einsteinian gravity—general relativity (GR)—. (Anti)evaporation phenomena consist of the exponentially (growing) decreasing radius of the black hole horizon These were first discovered by Bousso and Hawking within the context of quantum dilaton-gravity Evaporation and antievaporation are related to a dynamical decreasing and increasing of the black hole horizon radius in time. These instabilities may be provoked by several different dynamical origins. Let us consider the condition for a black hole horizon (∇φ)2 = 0 Substituting in this latter relation Equation (16), we obtain a simple system of differential equations; i.e.,. We review some basic aspects of evaporation and antievaporation in f ( R)-gravity [22,23,24], taking into account the Nariai metric and extremal Reissner–Nodrström black holes. Either an increase or a decrease of φ correspond to a dynamical displacement of the horizon
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