Dynamical EoW branes in rotating BTZ black holes are mapped to JT gravity, yielding BCFT thermodynamics and indicating possible interior transitions between single and double-joint configurations.
The entropy of hawking radiation
7 Pith papers cite this work, alongside 717 external citations. Polarity classification is still indexing.
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A black hole can be converted into a visible quantum system of D-branes and strings by moving it slowly through a suitably chosen varying-dilaton background that avoids adiabatic breakdown, spacetime collapse, and premature evaporation.
A spherically symmetric charged black hole evaporating via Hawking radiation can remain regular, with neither a singularity nor a Cauchy horizon, due to electromagnetic repulsion and energy-condition violation.
Modular quantization of a single holographic CFT reproduces exact Hartle-Hawking correlators of smooth BTZ black holes in the semiclassical limit while yielding non-smooth stretched-horizon descriptions at finite GN.
The paper argues flat minima are an illusion and that a reparameterization-invariant 'weakness' score predicts generalization where raw sharpness fails.
A new action for entanglement entropy in AdS3/CFT2 derives gravity equations, reduces to a string worldsheet, reproduces bit threads, and unifies several quantum gravity conjectures.
Lowering the quintessence state parameter w_q in Kiselev black holes produces ultra-slow evaporation distinct from PFDM and Horndeski cases, offering a possible constraint on w_q.
citing papers explorer
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Rotating End of the World
Dynamical EoW branes in rotating BTZ black holes are mapped to JT gravity, yielding BCFT thermodynamics and indicating possible interior transitions between single and double-joint configurations.
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How to Expose a Black Hole
A black hole can be converted into a visible quantum system of D-branes and strings by moving it slowly through a suitably chosen varying-dilaton background that avoids adiabatic breakdown, spacetime collapse, and premature evaporation.
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Radiating black holes in general relativity need not be singular
A spherically symmetric charged black hole evaporating via Hawking radiation can remain regular, with neither a singularity nor a Cauchy horizon, due to electromagnetic repulsion and energy-condition violation.
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Modular quantization and black holes
Modular quantization of a single holographic CFT reproduces exact Hartle-Hawking correlators of smooth BTZ black holes in the semiclassical limit while yielding non-smooth stretched-horizon descriptions at finite GN.
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Are Flat Minima an Illusion?
The paper argues flat minima are an illusion and that a reparameterization-invariant 'weakness' score predicts generalization where raw sharpness fails.
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Toward a worldsheet theory of entanglement entropy
A new action for entanglement entropy in AdS3/CFT2 derives gravity equations, reduces to a string worldsheet, reproduces bit threads, and unifies several quantum gravity conjectures.
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Kiselev black hole and the ultra-slow evaporating behavior
Lowering the quintessence state parameter w_q in Kiselev black holes produces ultra-slow evaporation distinct from PFDM and Horndeski cases, offering a possible constraint on w_q.