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The Endpoint of Hawking Evaporation
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The formation and semi-classical evaporation of two-dimensional black holes is studied in an exactly solvable model. Above a certain threshold energy flux, collapsing matter forms a singularity inside an apparent horizon. As the black hole evaporates the apparent horizon recedes and meets the singularity in a finite proper time. The singularity emerges naked and future evolution of the geometry requires boundary conditions to be imposed there. There is a natural choice of boundary conditions which match the evaporated black hole solution onto the linear dilaton vacuum. Below the threshold energy flux no horizon forms and boundary conditions can be imposed where infalling matter is reflected from a time-like naked singularity. All information is recovered at spatial infinity in this case.
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Cited by 3 Pith papers
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Entanglement Revivals and Scrambling for Evaporating Black Holes
Increasing black hole scrambling time in JT and RST evaporating geometries suppresses and eliminates late-time entanglement revivals in 2d CFT mutual information for disjoint intervals, interpolating between quasipart...
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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.
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Entanglement Revivals and Scrambling for Evaporating Black Holes
Black hole scrambling suppresses and eventually eliminates late-time entanglement revivals in CFT mutual information for disjoint intervals, with spikes vanishing when interval lengths become exponential in the scramb...
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