Thermal corpuscular black holes

Casadio, Roberto; Giugno, Andrea; Orlandi, Alessio

doi:10.1103/physrevd.91.124069

Cited by 45 publications

(37 citation statements)

References 34 publications

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“…Consequently, the probability of this system of size R s to be a black hole would be larger according to the Horizon Quantum Mechanics [43]. Moreover, this is qualitatively similar to what was found in [44], namely that the horizon area would also be larger than in general relativity. However, one has to be careful interpreting the results obtained in Figure 1, since R H − R M doesn't exceed l p , which is precisely the region where our approach breaks down, as discussed in the previous section.…”

Section: Model For Quantum Black Holes?supporting

confidence: 68%

Quantum gravitational corrections to a star metric and the black hole limit

2019

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In this paper we consider the full set of quantum gravitational corrections to a star metric to second order in curvature. As we use an effective field theoretical approach, these corrections apply to any model of quantum gravity that is based on general coordinate invariance. We then discuss the black hole limit and identify an interesting phenomenon which could shed some light on the nature of astrophysical black holes: while star metrics receive corrections at second order in curvature, vacuum solutions such as black hole metrics do not. What happens to these corrections when a star collapses? 1 x.calmet@sussex.ac.uk

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Section: Model For Quantum Black Holes?supporting

confidence: 68%

Quantum gravitational corrections to a star metric and the black hole limit

2019

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“…Even when the gravitational regime is strong, the set-up is nicely understood as a Newtonian theory of N gravitons, which are loosely confined in a "potential well" of size their Compton wavelength λ and interact with an effective gravitational coupling α ∼ 1/N . As a result, it is possible to recover the correct post-Newtonian expansion of the gravitational field generated by a static, spherically symmetric source [10] or the renowned Bekenstein-Hawking area law [11] with logarithmic corrections [12] for the Hawking radiation. On the other hand, this framework represents a natural scenario for a cosmological model of inflation [8,13], whose characteristic quantities display quantum properties related to the corpuscular nature of gravity.…”

Section: Introductionmentioning

confidence: 99%

Corpuscular slow-roll inflation

2018

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We show that a corpuscular description of gravity can lead to an inflationary scenario similar to Starobinsky's model without requiring the introduction of the inflaton field. All relevant properties are determined by the number of gravitons in the cosmological condensate or, equivalently, by their Compton length. In particular, the relation between the Hubble parameter H and its time derivativė H required by CMB observations at the end of inflation, as well as the (minimum) initial value of the slow-roll parameter, are naturally obtained from the Compton size of the condensate.

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“…This perspective leads one to a third choice: uniformly distributed matter -a stance that has JHEP08(2015)082 been advocated, in particular, by Dvali and Gomez in a recent series of articles [13][14][15][16][17][18][19]. (See [20,21] for related work.) Those authors have reasoned that the BH interior is composed, for the most part, by N ∼ S BH weakly coupled, horizon-sized gravitons whose state is that of a "leaky" Bose-Einstein condensate.…”

Section: Introductionmentioning

confidence: 99%

Quantum state of the black hole interior

Brustein

Medved

2015

J. High Energ. Phys.

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If a black hole (BH) is initially in an approximately pure state and it evaporates by a unitary process, then the emitted radiation will be in a highly quantum state. As the purifier of this radiation, the state of the BH interior must also be in some highly quantum state. So that, within the interior region, the mean-field approximation cannot be valid and the state of the BH cannot be described by some semiclassical metric. On this basis, we model the state of the BH interior as a collection of a large number of excitations that are packed into closely spaced but single-occupancy energy levels; a sort-of "Fermi sea" of all light-enough particles. This highly quantum state is surrounded by a semiclassical region that lies close to the horizon and has a non-vanishing energy density. It is shown that such a state looks like a BH from the outside and decays via gravitational pair production in the near-horizon region at a rate that agrees with the Hawking rate. We also consider the fate of a classical object that has passed through to the BH interior and show that, once it has crossed over the near-horizon threshold, the object meets its demise extremely fast. This result cannot be attributed to a "firewall", as the trauma to the in-falling object only begins after it has passed through the near-horizon region and enters a region where semiclassical spacetime ends but the energy density is still parametrically smaller than Planckian.

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Thermal corpuscular black holes

Cited by 45 publications

References 34 publications

Quantum gravitational corrections to a star metric and the black hole limit

Quantum gravitational corrections to a star metric and the black hole limit

Corpuscular slow-roll inflation

Quantum state of the black hole interior

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