# The role of collapsed matter in the decay of black holes

## TL;DR

This paper investigates the final stages of black hole evaporation by considering the role of matter, comparing classicalization and bouncing scenarios, and estimating internal quantum pressure to understand disruption timescales.

## Contribution

It introduces a method to estimate internal quantum pressure from the matter inside black holes, contrasting different models and their predictions for black hole disruption.

## Key findings

- Corpuscular model aligns with semiclassical disruption timescales.
- Black-to-white hole bouncing predicts earlier disruption due to matter effects.
- Matter inside black holes influences the final evaporation stages significantly.

## Abstract

We try to shed some light on the role of matter in the final stages of black hole evaporation from the fundamental frameworks of classicalization and the black-to-white hole bouncing scenario. Despite being based on very different grounds, these two approaches attempt at going beyond the background field method and treat black holes as fully quantum systems rather than considering quantum field theory on the corresponding classical manifolds. They also lead to the common prediction that the semiclassical description of black hole evaporation should break down and the system be disrupted by internal quantum pressure, but they both arrive at this conclusion neglecting the matter that formed the black hole. We instead estimate this pressure from the bootstrapped description of black holes, which allows us to express the total Arnowitt-Deser-Misner mass in terms of the baryonic mass still present inside the black hole. We conclude that, although these two scenarios provide qualitatively similar predictions for the final stages, the corpuscular model does not seem to suggest any sizeable deviation from the semiclassical time scale at which the disruption should occur, unlike the black-to-white hole bouncing scenario. This, in turn, makes the phenomenology of corpuscular black holes more subtle from an astrophysical perspective.