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S. W. Hawking, “Black hole explosions”, Nature 248
1975
Earlier work this paper cites.
S. W. Hawking, “Breakdown of Predictability in Gravitational Collapse,” Phys. Rev. D 14
1976
Earlier work this paper cites.
D. N. Page, “Average entropy of a subsystem,” Phys. Rev. Lett. 71
1993
Earlier work this paper cites.
L. Susskind, L. Thorlacius and J. Uglum, “The Stretched horizon and black hole complementarity,” Phys. Rev. D 48
1993
Earlier work this paper cites.
S. B. Giddings, “Comments on information loss and remnants,” Phys. Rev. D 49
1994
Earlier work this paper cites.
C. R. Stephens, G. ’t Hooft and B. F. Whiting, “Black hole evaporation without information loss,” Class. Quant. Grav. 11
1994
Earlier work this paper cites.
S. D. Mathur and D. Turton, “Comments on black holes I: The possibility of complementarity,” arXiv:1208.2005 [hep-th]
Original
2005
Earlier work this paper cites.
P. Hayden and J. Preskill, “Black holes as mirrors: Quantum information in random subsystems,” JHEP 0709
Original
2007
Earlier work this paper cites.

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S. D. Mathur, “What Exactly is the Information Paradox?,” Lect. Notes Phys. 769
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A. Giveon and N. Itzhaki, “String Theory Versus Black Hole Complementarity,” JHEP 1212
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2013

Horizons of semiclassical black holes are cold

Brustein, Ram, Medved, A. J. M.

Understand

We calculate, using our recently proposed semiclassical framework, the quantum state of the Hawking pairs that are produced during the evaporation of a black hole (BH).

Our framework adheres to the standard rules of quantum mechanics and incorporates the quantum fluctuations of the collapsing shell spacetime in Hawking's original calculation, while accounting for back-reaction effects.
We argue that the negative-energy Hawking modes need to be regularly integrated out; and so these are effectively subsumed by the BH and, as a result, the number of coherent negative-energy modes $N_{coh}$ at any given time is parametrically smaller than the total number of the Hawking particles $N_{total}$ emitted during the lifetime of the BH.
We find that $N_{coh}$ is determined by the width of the BH wavefunction and scales as the square root of the BH entropy.

Built on

S. W. Hawking, “Black hole explosions”, Nature 248
1975
Earlier work this paper cites.
S. W. Hawking, “Breakdown of Predictability in Gravitational Collapse,” Phys. Rev. D 14
1976
Earlier work this paper cites.
D. N. Page, “Average entropy of a subsystem,” Phys. Rev. Lett. 71
1993
Earlier work this paper cites.
L. Susskind, L. Thorlacius and J. Uglum, “The Stretched horizon and black hole complementarity,” Phys. Rev. D 48
1993
Earlier work this paper cites.
S. B. Giddings, “Comments on information loss and remnants,” Phys. Rev. D 49
1994
Earlier work this paper cites.
C. R. Stephens, G. ’t Hooft and B. F. Whiting, “Black hole evaporation without information loss,” Class. Quant. Grav. 11
1994
Earlier work this paper cites.
S. D. Mathur and D. Turton, “Comments on black holes I: The possibility of complementarity,” arXiv:1208.2005 [hep-th]
Original
2005
Earlier work this paper cites.
P. Hayden and J. Preskill, “Black holes as mirrors: Quantum information in random subsystems,” JHEP 0709
Original
2007
Earlier work this paper cites.