Entanglement revivals in evaporating black holes survive only when radiation intervals are larger than a critical length set by the exponential of the black-hole scrambling time.
Semiclassical Approach to Black Hole Evaporation
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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.
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fields
hep-th 2years
2026 2roles
background 2representative citing papers
Semiclassical black hole evaporation in four dimensions produces a thunderbolt singularity signaling breakdown of the effective theory at large distances.
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Entanglement Revivals and Scrambling for Evaporating Black Holes
Entanglement revivals in evaporating black holes survive only when radiation intervals are larger than a critical length set by the exponential of the black-hole scrambling time.
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Breakdown of Semiclassical Gravity in Four-Dimensional Black Hole Evaporation
Semiclassical black hole evaporation in four dimensions produces a thunderbolt singularity signaling breakdown of the effective theory at large distances.