Freely falling observer and black hole radiation

Kim, Wontae; Son, E. J.

doi:10.1142/s0217732314500527

Cited by 13 publications

(13 citation statements)

References 55 publications

(62 reference statements)

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“…Again, for a large black hole, the contribution of these perturbative interactions to the total density matrix is initially strongly suppressed, but it grows as the black hole evaporates and N approaches K. At the end of evaporation, when N = K, all the emitted Hawking quanta are strongly entangled by interactions, and the resulting density matrix will be that of a pure state, as we can see from Eq. (20).…”

Section: A Simple Modelmentioning

confidence: 99%

Icezones instead of firewalls: extended entanglement beyond the event horizon and unitary evaporation of a black hole

Hutchinson¹,

Stojković²

2016

Class. Quantum Grav.

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We examine the basic assumptions in the original setup of the firewall paradox. The main claim is that a single mode of the lathe radiation is maximally entangled with the mode inside the horizon and simultaneously with the modes of early Hawking radiation. We argue that this situation never happens during the evolution of a black hole. Quantum mechanics tells us that while the black hole exists, unitary evolution maximally entangles a late mode located just outside the horizon with a combination of early radiation and black hole states, instead of either of them separately. One of the reasons for this is that the black hole radiation is not random and strongly depends on the geometry and charge of the black hole, as detailed numerical calculations of Hawking evaporation clearly show. As a consequence, one can't factor out the state of the black hole. However, this extended entanglement between the black hole and modes of early and late radiation indicates that, as the black hole ages, the local Rindler horizon is modified out to macroscopic distances from the black hole. Fundamentally non-local physics nor firewalls are not necessary to explain this result. We propose an infrared mechanism called icezone that is mediated by low energy interacting modes and acts near any event horizon to entangle states separated by long distances. These interactions at first provide small corrections to the thermal Hawking radiation. At the end of evaporation however the effect of interactions is as large as the Hawking radiation and information is recovered for an outside observer. We verify this in an explicit construction and calculation of the density matrix of a spin model.

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Section: A Simple Modelmentioning

confidence: 99%

Icezones instead of firewalls: extended entanglement beyond the event horizon and unitary evaporation of a black hole

Hutchinson¹,

Stojković²

2016

Class. Quantum Grav.

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“…1 It is to be noted that this is in contrast to working in the Kruskal extension of Schwarzschild metric where different vacua need to be defined according to the different boundary conditions (See for example [19][20][21]). We believe that the in-vacum is more natural to work with in the collapse geometry.…”

Section: Figmentioning

confidence: 99%

Black hole kinematics: The “in”-vacuum energy density and flux for different observers

Singh

Chakraborty

2014

Phys. Rev. D

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We have investigated the local invariant scalar observables -energy density and flux -which explicitly depend on the kinematics of the concerned observers in the thin null shell gravitational collapse geometry. The use of globally defined null coordinates allows for the definition of a unique in-vacuum for the scalar field propagating in this background. Computing the stress-energy tensor for this scalar field, we work out the energy density and flux for the static observers outside the horizon and then consider the radially in-falling observers who fall in from some specified initial radius all the way through the horizon and inside to the eventual singularity. Our results confirm the thermal Tolman-shifted energy density and fluxes for the static observers which diverge at the horizon. For the in-falling observer starting from far off, both the quantities -energy density and flux at the horizon crossing are regular and finite. For example, the flux at the horizon for the in-falling observer from infinity is approximately 24 times the flux for the observer at infinity. Compared with the static observers in the near-horizon region, this is quite small. Both the quantities grow as the in-fall progresses inside the horizon and diverge at the singularity.

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“…This fact is based on the classical argument of locality but it may not be true in quantum regime such that a freely falling observer can find quantum-mechanical radiation and temperature [19][20][21][22][23]. Recently, it has been claimed that the freely falling observer dropped at the horizon necessarily encounters the infinite negative energy density when the observer passes through the horizon [24]. On general grounds, one may regard this phenomenon as a very special feature such a simplified model [25] that…”

Section: Introductionmentioning

confidence: 99%

Something special at the event horizon

2014

Self Cite

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We revisit the free-fall energy density of scalar fields semi-classically by employing the trace anomaly on a two-dimensional Schwarzschild black hole with respect to various black hole states in order to clarify whether something special at the horizon happens or not. For the Boulware state, the energy density at the horizon is always negative divergent, which is independent of initial free-fall positions. However, in the Unruh state the initial free-fall position is responsible for the energy density at the horizon and there is a critical point to determine the sign of the energy density at the horizon. In particular, a huge negative energy density appears when the freely falling observer is dropped just near the horizon. For the Hartle-Hawking state, it may also be positive or negative depending on the initial free-fall position, but it is always finite. Finally, we discuss physical consequences of these calculations.

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Freely falling observer and black hole radiation

Cited by 13 publications

References 55 publications

Icezones instead of firewalls: extended entanglement beyond the event horizon and unitary evaporation of a black hole

Icezones instead of firewalls: extended entanglement beyond the event horizon and unitary evaporation of a black hole

Black hole kinematics: The “in”-vacuum energy density and flux for different observers

Something special at the event horizon

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