The role of collapsed matter in the decay of black holes

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. * casadio@bo.infn.it † agiusti@bo.infn.it

Configurational entropy of black hole quantum cores

“…The case of a (slowly and rigidly) rotating ball is left for future development. 11 A similar quantisation for the mass M was found long ago in [44,45] by studying stable configurations of boson stars. As we recalled in the Introduction, equation (2.11) is also reminiscent of Bekenstein's area law [21].…”

“…Several methods for removing the singularity in approaches to quantum gravity have been proposed [2][3][4][5][6][7] and the appearance of a bounce at a minimum radius is generically obtained in semiclassical models [8][9][10]. These results suggest that the role played by matter in the description of black hole formation (and subsequent evolution [11]) is crucial.…”

Long-Range Quantum Gravity

“…We define the Schwarzschild radius as R s = 2GM/c 2 . This means that the classical criticality bound (2) is saturated, namely the black hole is considered as a sort of critical star (see also [65,66]). Putting together Equation (1) and the definition of the Schwarzschild radius, we find that the number of degrees of freedom in the black hole cavity scales as the area, i.e., it scales holographically in the sense previously described:…”

Long-Range Quantum Gravity

“…We define the Schwarzschild radius as R s = 2GM/c 2 . This means that the classical criticality bound (2) is saturated, namely the black hole is considered as a sort of critical star (see also [48,49]). Putting together Eq.…”