Semiclassical Approach to Black Hole Evaporation

TL;DR

This paper explores black hole evaporation using semiclassical methods in two different 2D models, revealing that the approximation fails before naked singularities form, with implications for understanding black hole remnants.

Contribution

It compares two distinct 2D black hole models to analyze evaporation, demonstrating the semiclassical approximation's limitations near singularities.

Findings

Semiclassical approximation breaks down before naked singularity formation.

Results are consistent across different 2D models.

Evaporation process shows qualitative agreement with exactly solved models.

Abstract

Black hole evaporation may lead to massive or massless remnants, or naked singularities. This paper investigates this process in the context of two quite different two dimensional black hole models. The first is the original CGHS model, the second is another two dimensional dilaton-gravity model, but with properties much closer to physics in the real, four dimensional, world. Numerical simulations are performed of the formation and subsequent evaporation of black holes and the results are found to agree qualitatively with the exactly solved modified CGHS models, namely that the semiclassical approximation breaks down just before a naked singularity appears.