In the moving mirror analog of black hole evaporation, restoring information by vacuum entanglement requires emitting at least as many late-time inertial particles as Hawking particles, and for real black holes this is energetically impossible.
On the partner particles for moving mirror radiation and black hole evaporation
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abstract
The partner mode with respect to a vacuum state for a given mode (like that corresponding to one of the thermal particles emitted by a black hole) is defined and calculated. The partner modes are explicitly calculated for a number of cases, in particular for the modes corresponding to a particle detector being excited by turn-on/turn-off transients, or with the thermal particles emitted by the accelerated mirror model for black hole evaporation. One of the key results is that the partner mode in general is just a vacuum fluctuation, and one can have the partner mode be located in a region where the state cannot be distinguished from the vacuum state by any series of local measurements, including the energy density. I.e., "information" (the correlations with the thermal emissions) need not be associated with any energy transport. The idea that black holes emit huge amounts of energy in their last stages because of all the information which must be emitted under the assumption of black-hole unitarity is found not necessarily to be the case.
fields
gr-qc 1years
2019 1verdicts
ACCEPT 1representative citing papers
citing papers explorer
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The Particle and Energy Cost of Entanglement of Hawking Radiation with the Final Vacuum State
In the moving mirror analog of black hole evaporation, restoring information by vacuum entanglement requires emitting at least as many late-time inertial particles as Hawking particles, and for real black holes this is energetically impossible.