In 2D centaur geometries the entropy difference of a modular-conjugate Hawking-pair probe traces an inverse mini-Page curve that bottoms at τ≈β/8, marking when information begins to leave the cosmological horizon.
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abstract
Hawking's 1974 calculation of thermal emission from a classical black hole led to his 1976 proposal that information may be lost from our universe as a pure quantum state collapses gravitationally into a black hole, which then evaporates completely into a mixed state of thermal radiation. Another possibility is that the information is not lost, but is stored in a remnant of the evaporating black hole. A third idea is that the information comes out in nonthermal correlations within the Hawking radiation, which would be expected to occur at too slow a rate, or be too spread out, to be revealed by any nonperturbative calculation.
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In the near-horizon geometry of a black hole, the dynamical Casimir effect is suppressed by a conformal geometric factor and vanishing effective Mach number, causing the transition probability to vanish at the event horizon.
A covariant model of Dirac fermions with an extra Planck-derived term yields the same Einstein-equation collapse as ordinary GR yet permits numerical trajectories that escape the black hole.
citing papers explorer
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The mini-Page Curve in Cosmology
In 2D centaur geometries the entropy difference of a modular-conjugate Hawking-pair probe traces an inverse mini-Page curve that bottoms at τ≈β/8, marking when information begins to leave the cosmological horizon.
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Dynamical Casimir Effect and Vacuum Friction in the Near-Horizon Geometry of a Black Hole
In the near-horizon geometry of a black hole, the dynamical Casimir effect is suppressed by a conformal geometric factor and vanishing effective Mach number, causing the transition probability to vanish at the event horizon.
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Classical limit for Dirac fermions with modified action in the presence of the black hole
A covariant model of Dirac fermions with an extra Planck-derived term yields the same Einstein-equation collapse as ordinary GR yet permits numerical trajectories that escape the black hole.