Quantum hoop conjecture: Black hole formation by particle collisions

Casadio, Roberto; Micu, Octavian; Scardigli, Fabio

doi:10.1016/j.physletb.2014.03.037

Cited by 51 publications

(76 citation statements)

References 23 publications

(17 reference statements)

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“…We start from reviewing the basics of the (global) HQM for static spherically symmetric sources [1][2][3][4][5][6][7][8], and then extend this formalism to rotating systems by means of the Kerr relation for the horizon radii in terms of the asymptotic mass and angular momentum of the space-time. In particular, we shall rely on the results for the "global" case of Ref.…”

Section: Horizon Quantum Mechanicsmentioning

confidence: 99%

“…If the index α is continuous (again, see Ref. [3] for some important remarks), the probability density that we detect a gravitational radius of size R H associated with the quantum state | ψ S is given by P H (R H ) = 4 π R 2 H |ψ H (R H )| 2 , and we can define the conditional probability density that the source lies inside its own gravitational radius R H as 14) where 5 Finally, the probability that the system in the state | ψ S is a black hole will be obtained by integrating (2.14) over all possible values of R H , namely…”

Section: Spherically Symmetric Systemsmentioning

confidence: 99%

“…The formalism dubbed horizon quantum mechanics (HQM) [1][2][3][4][5][6][7][8], was initially proposed with the purpose of describing the gravitational radius of spherically symmetric compact sources and determining the existence of a horizon in a quantum mechanical fashion. It therefore appears as a natural continuation in this research direction to extend the HQM to rotating sources.…”

Section: Introductionmentioning

confidence: 99%

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Horizon quantum mechanics of rotating black holes

et al. 2017

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The horizon quantum mechanics is an approach that was previously introduced in order to analyze the gravitational radius of spherically symmetric systems and compute the probability that a given quantum state is a black hole. In this work, we first extend the formalism to general spacetimes with asymptotic (ADM) mass and angular momentum. We then apply the extended horizon quantum mechanics to a harmonic model of rotating corpuscular black holes. We find that simple configurations of this model naturally suppress the appearance of the inner horizon and seem to disfavor extremal (macroscopic) geometries.

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Section: Horizon Quantum Mechanicsmentioning

confidence: 99%

Section: Spherically Symmetric Systemsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Horizon quantum mechanics of rotating black holes

et al. 2017

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“…It is therefore very likely that, although their existence can be inferred within perturbation theory, like we have recalled in the previous section, a full description of their quantum properties requires a non-perturbative approach, like the horizon wave-function (HWF) formalism (for the details, see Refs. [29][30][31][32][33]; for a similar picture of the black hole horizon, see Ref. [34]).…”

Section: Horizon Wave-functionmentioning

confidence: 99%

The horizon of the lightest black hole

Calmet

Casadio

2015

Eur. Phys. J. C

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We study the properties of the poles of the resummed graviton propagator obtained by resumming bubble matter diagrams which correct the classical graviton propagator. These poles have been previously interpreted as black holes precursors. Here, we show using the horizon wavefunction formalism that these poles indeed have properties which make them compatible with being black hole precursors. In particular, when modeled with a Breit-Wigner distribution, they have a well-defined gravitational radius. The probability that the resonance is inside its own gravitational radius, and thus that it is a black hole, is about one half. Our results confirm the interpretation of these poles as black hole precursors.

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“…This implies 17) where N denotes the expectation value of the number of quanta in the coherent state,…”

Section: Quantum Coherent Statesmentioning

confidence: 99%

Black holes as self-sustained quantum states and Hawking radiation

Casadio

Giugno

Micu³

et al. 2014

Phys. Rev. D

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We employ the recently proposed formalism of the "horizon wave-function" to investigate the emergence of a horizon in models of black holes as Bose-Einstein condensates of gravitons. We start from the Klein-Gordon equation for a massless scalar (toy graviton) field coupled to a static matter current. The (spherically symmetric) classical field reproduces the Newtonian potential generated by the matter source, and the corresponding quantum state is given by a coherent superposition of scalar modes with continuous occupation number. Assuming an attractive self-interaction that allows for bound states, one finds that (approximately) only one mode is allowed, and the system can be confined in a region of the size of the Schwarzschild radius. This radius is then shown to correspond to a proper horizon, by means of the horizon wave-function of the quantum system, with an uncertainty in size naturally related to the expected typical energy of Hawking modes. In particular, this uncertainty decreases for larger black hole mass (with larger number of light scalar quanta), in agreement with semiclassical expectations, a result which does not hold for a single very massive particle. We finally speculate that a phase transition should occur during the gravitational collapse of a star, ideally represented by a static matter current and Newtonian potential, that leads to a black hole, again ideally represented by the condensate of toy gravitons, and suggest an effective order parameter that could be used to investigate this transition. *

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Quantum hoop conjecture: Black hole formation by particle collisions

Cited by 51 publications

References 23 publications

Horizon quantum mechanics of rotating black holes

Horizon quantum mechanics of rotating black holes

The horizon of the lightest black hole

Black holes as self-sustained quantum states and Hawking radiation

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