Sparsity of the Hawking flux

Visser, Matt; Gray, Finnian; Schuster, Sebastian; Van-Brunt, Alexander

doi:10.1142/9789813226609_0175

Cited by 6 publications

(5 citation statements)

References 33 publications

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“…Classical effective description of black hole radiation. Of course, one should first study carefully the semi-classical properties of this solution to interpret the outgoing flux as semi-classical [76,77]. However, it is interesting to consider this scenario as we may have a black-bounce to wormhole transition similar to that already considered in the previous subsection.…”

Section: Model With Outgoing Radiation (Evaporation)mentioning

confidence: 94%

Vaidya spacetimes, black-bounces, and traversable wormholes

Simpson

Martín–Moruno

Visser

2019

Class. Quantum Grav.

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105

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We consider a non-static evolving version of the regular "black-bounce"/traversable wormhole geometry recently introduced in JCAP02(2019)042. We first re-write the static metric using Eddington-Finkelstein coordinates, and then allow the mass parameter m to depend on the null time coordinate (à la Vaidya). The spacetime metric isHere w = {u, v} denotes suitably defined {outgoing, ingoing} null time coordinates; representing {retarded, advanced} time, while, (at least for a = 0), we allow r ∈ (−∞, +∞). This spacetime is still simple enough to be tractable, and neatly interpolates between Vaidya spacetime, a black-bounce, and a traversable wormhole. We show how this metric can be used to describe several physical situations of particular interest, including a growing black-bounce, a wormhole to black-bounce transition, and the opposite black-bounce to wormhole transition.

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Section: Model With Outgoing Radiation (Evaporation)mentioning

confidence: 94%

Vaidya spacetimes, black-bounces, and traversable wormholes

Simpson

Martín–Moruno

Visser

2019

Class. Quantum Grav.

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105

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“…(Such emission also contributes to the random walk of black hole, as the result of backreaction from Hawking emission [26].) See [27][28][29] for detailed discussions.…”

Section: Sparsity Makes Lifetime Even Longermentioning

confidence: 99%

“…Eq. (2.2) does not take into account the effect of sparsity, instead mass loss is only treated as particle mass loss associated to a given temperature [27][28][29]. Once the wave effect of the radiation is taken into account, sparsity becomes a crucial feature that extends the black hole lifetime.…”

Section: Jhep10(2018)195mentioning

confidence: 99%

An effective black hole remnant via infinite evaporation time due to generalized uncertainty principle

Ong¹

2018

J. High Energ. Phys.

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We study a form of generalized uncertainty principle (GUP) that leads to vanishing quantum effect, i.e. ∆x∆p ∼ 0, at sufficiently high momenta. We find that such a GUP allows black holes to evaporate completely, however this process takes an infinite amount of time to achieve, resulting in a metastable remnant. We also discuss some connections between the proposed generalized uncertainty principle with other quantum gravity models.

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“…* One still needs to make some choices regarding how the coordinates are set up. * In view of the known sparsity of the Hawking flux [37][38][39], it should be noted that the Vaidya geometry is a good approximation only on average: a Vaidya-like model necessarily approximates the Hawking flux by a continuum limit. -There is neither no real need for, nor advantage in, using generalized Vaidya spacetimes [40].…”

Section: Introductionmentioning

confidence: 99%

Evading the trans-Planckian problem with Vaidya spacetimes

Booth

Creelman

Santiago

et al. 2019

J. Cosmol. Astropart. Phys.

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Hawking radiation, when treated in the ray optics limit, exhibits the unfortunate trans-Planckian problem -a Hawking photon near spatial infinity, if backtracked to the immediate vicinity of the horizon is hugely blue-shifted and found to have had trans-Planckian energy. (And if back-tracked all the way to the horizon, the photon is formally infinitely blue-shifted, and formally acquires infinite energy.) Unruh has forcefully argued that this implies that the Hawking flux represents a vacuum instability in the presence of a horizon, and that the Hawking photons are actually emitted from some region exterior to the horizon. We seek to make this idea more precise and somewhat explicit by building a purely kinematical model for Hawking evaporation based on two Vaidya spacetimes (outer and inner) joined across a thin time-like boundary layer. The kinematics of this model is already quite rich, and we shall defer consideration of the dynamics for subsequent work. In particular we shall present an explicit calculation of the the 4-acceleration of the shell (including the effects of gravity, motion, and the outgoing null flux) and relate this 4-acceleration to the Unruh temperature.

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Sparsity of the Hawking flux

Cited by 6 publications

References 33 publications

Vaidya spacetimes, black-bounces, and traversable wormholes

Vaidya spacetimes, black-bounces, and traversable wormholes

An effective black hole remnant via infinite evaporation time due to generalized uncertainty principle

Evading the trans-Planckian problem with Vaidya spacetimes

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