Inner horizon of the quantum Reissner-Nordström black holes

Casadio, Roberto; Micu, Octavian; Stojković, Dejan

doi:10.1007/jhep05(2015)096

Cited by 19 publications

(17 citation statements)

References 32 publications

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“…In this section, we shall introduce the reader to some general aspects of the horizon quantum mechanics (HQM), according to its most recent updates [16][17][18][19][20][21][22]. If one envisages the source of the gravitational field as a purely quantum object under this perspective, then one can faithfully picture both the ADM mass and the gravitational radius as quantum variables in return.…”

Section: Horizon Quantum Mechanicsmentioning

confidence: 99%

Horizon quantum fuzziness for non-singular black holes

2018

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We study the extent of quantum gravitational effects in the internal region of non-singular, Hayward-like solutions of Einstein's field equations according to the formalism known as horizon quantum mechanics. We grant a microscopic description to the horizon by considering a huge number of soft, off-shell gravitons, which superimpose in the same quantum state, as suggested by Dvali and Gomez. In addition to that, the constituents of such a configuration are understood as loosely confined in a binding harmonic potential. A simple analysis shows that the resolution of a central singularity through quantum physics does not tarnish the classical description, which is bestowed upon this extended self-gravitating system by General Relativity. Finally, we estimate the appearance of an internal horizon as being negligible, because of the suppression of the related probability caused by the large number of virtual gravitons.

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Section: Horizon Quantum Mechanicsmentioning

confidence: 99%

Horizon quantum fuzziness for non-singular black holes

2018

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“…To prove this statement, one can start with the normal-ordered quantum Hamiltonian density in momentum space,Ĥ = kâ † kâ k +H g (27) whereH g is the ground state energy density,…”

Section: Scalar Toy Gravitons Coupled To a Sourcementioning

confidence: 99%

“…In these regimes, it is uncertain whether a semiclassical approach is still valid, since the quantum fluctuations become relevant with respect to the surrounding space-time geometry. The HWF [23][24][25][26][27][28] was precisely proposed in order to define the gravitational radius of any quantum system and should therefore be very useful for investigating this issue.…”

Section: Black Holes As Self-sustained Quantum Statesmentioning

confidence: 99%

“…A fairly recent formalism that is very suitable for such a task is the HWF introduced in [23] and further developed in [24][25][26][27][28]. This tool applies to the quantum mechanical state ψ S of any system localized in space and at rest in the chosen reference frame.…”

Section: Horizon Wave Function Formalismmentioning

confidence: 99%

“…The aim of this review is to present some of the features of this model obtained from the "horizon wave-function formalism" (HWF). In this general approach, a wave-function for the gravitational radius can be associated with any localized quantum mechanical particle [23][24][25][26][27][28], which makes it easy to formulate in a quantitative way a condition for distinguishing black holes from regular particles. Among the added values, the formalism naturally leads to an effective generalized uncertainty principle (GUP) [29][30][31][32][33] for the particle's position (similar features are naturally encoded in non-commutative models of black holes; for a review, see [34]), and a decay rate for microscopic black holes.…”

Section: Introductionmentioning

confidence: 99%

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Thermal BEC Black Holes

Casadio

Giugno

Micu

et al. 2015

Entropy

Self Cite

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Abstract:We review some features of Bose-Einstein condensate (BEC) models of black holes obtained by means of the horizon wave function formalism. We consider the Klein-Gordon equation for a toy graviton field coupled to a static matter current in a spherically-symmetric setup. The classical field reproduces the Newtonian potential generated by the matter source, while the corresponding quantum state is given by a coherent superposition of scalar modes with a continuous occupation number. An attractive self-interaction is needed for bound states to form, the case in which one finds that (approximately) one mode is allowed, and the system of N bosons can be self-confined in a volume of the size of the Schwarzschild radius. The horizon wave function formalism is then used to show that the radius of such a system corresponds to a proper horizon. The uncertainty in the size of the horizon is related to the typical energy of Hawking modes: it decreases with the increasing of the black hole mass (larger number of gravitons), resulting in agreement with the semiclassical calculations and which does not hold for a single very massive particle. The spectrum of these systems has two components: a discrete ground state of energy m (the bosons forming the black hole) and a continuous spectrum with energy ω > m (representing the Hawking radiation and modeled with a Planckian distribution at the expected Hawking temperature). Assuming the main effect of the internal scatterings is the Hawking radiation, the N -particle state can be collectively described by a single-particle wave-function given by a superposition of a total ground state with energy M = N m and Entropy 2015, 17 6894 a Planckian distribution for E > M at the same Hawking temperature. This can be used to compute the partition function and to find the usual area law for the entropy, with a logarithmic correction related to the Hawking component. The backreaction of modes with ω > m is also shown to reduce the Hawking flux. The above corrections suggest that for black holes in this quantum state, the evaporation properly stops for a vanishing mass.

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Classicalizing Gravity

Casadio

Giusti

2021

Modified Gravity and Cosmology

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Inner horizon of the quantum Reissner-Nordström black holes

Cited by 19 publications

References 32 publications

Horizon quantum fuzziness for non-singular black holes

Horizon quantum fuzziness for non-singular black holes

Thermal BEC Black Holes

Classicalizing Gravity

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