Self-similar evaporation and collapse in the quantum portrait of black holes

Foit, Valentino F.; Wintergerst, Nico

doi:10.1103/physrevd.92.064043

Cited by 12 publications

(16 citation statements)

References 46 publications

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“…Our analysis however does not make use of any specific determination of the coefficients γ 1 and γ in terms of the details of the scatterings that give rise to the Hawking radiation (and we therefore assumed no dependence of these parameters from the number N ). A very interesting attempt at understanding the Hawking radiation directly from the two-and three-body decays inside a BEC recently appeared [9], where however no general relativistic effect is included. The estimate for the flux we provide in section 5 could therefore be viewed as complementary to that in Ref.…”

Section: Discussionmentioning

confidence: 99%

“…This in turn would mean that in principle γ 1 should also depend on N , for example if the maximal packing condition (2.4) remains satisfied along the evaporation (see Ref. [9] for a more detailed study of the scatterings inside the BEC). We however prefer to keep it as a free variable in this work, so that one could relate it a posteriori to known features of the Hawking radiation, at least in the large N limit.…”

Section: Bec With Thermal Quantum Hairmentioning

confidence: 99%

“…The result in Refs. [1,3] have thus triggered a number of developments [4,5,6,7,8,9] and possible cosmological implications were also investigated in Refs. [10,11,12,13].…”

Section: Introductionmentioning

confidence: 99%

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Thermal corpuscular black holes

2015

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We study the corpuscular model of an evaporating black hole consisting of a specific quantum state for a large number N of self-confined bosons. The single-particle spectrum contains a discrete ground state of energy m (corresponding to toy gravitons forming the black hole), and a gapless continuous spectrum (to accommodate for the Hawking radiation with energy ω > m). Each constituent is in a superposition of the ground state and a Planckian distribution at the expected Hawking temperature in the continuum. We first find that, assuming the Hawking radiation is the leading effect of the internal scatterings, the corresponding 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 a Planckian distribution for E > M at the same Hawking temperature. From this collective state, we compute the partition function and obtain an entropy which reproduces the usual area law with a logarithmic correction precisely related with the Hawking component. By means of the horizon wave-function for the system, we finally show the backreaction of modes with ω > m reduces the Hawking flux. Both corrections, to the entropy and to the Hawking flux, suggest the evaporation properly stops for vanishing mass, if the black hole is in this particular quantum state.

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Section: Discussionmentioning

confidence: 99%

Section: Bec With Thermal Quantum Hairmentioning

confidence: 99%

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Thermal corpuscular black holes

2015

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“…The simple and intuitive corpuscular model recently introduced by Dvali and Gomez in [16][17][18][19][20][21][22] and widely developed in [36][37][38][39][40][41][42][43][44], puts gravitation under a new light. The model is based on the assumption that the classical geometry should be viewed as an effective description of a quantum state with a large graviton occupation number, where gravitons play the role of space-time quanta, very much like photons are light quanta in a laser beam.…”

Section: Corpuscular Modelmentioning

confidence: 99%

“…From the expression of the Schwarzschild radius r H = 2 p E/m p , one easily finds r H R H , with R H given in Equation (39), and:…”

Section: Black Hole With Gaussian Excited Spectrummentioning

confidence: 99%

Thermal BEC Black Holes

Casadio

Giugno

Micu

et al. 2015

Entropy

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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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Universality of black hole quantum computing

Dvali

Gómez

Lüst

et al. 2016

Fortschritte der Physik

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By analyzing the key properties of black holes from the point of view of quantum information, we derive a model-independent picture of black hole quantum computing. It has been noticed that this picture exhibits striking similarities with quantum critical condensates, allowing the use of a common language to describe quantum computing in both systems. We analyze such quantum computing by allowing coupling to external modes, under the condition that the external influence must be soft-enough in order not to offset the basic properties of the system. We derive modelindependent bounds on some crucial time-scales, such as the times of gate operation, decoherence, maximal entanglement and total scrambling. We show that for black hole type quantum computers all these time-scales are of the order of the black hole half-life time. Furthermore, we construct explicitly a set of Hamiltonians that generates a universal set of quantum gates for the black hole type computer. We find that the gates work at maximal energy efficiency. Furthermore, we establish a fundamental bound on the complexity of quantum circuits encoded on these systems, and characterize the unitary operations that are implementable. It becomes apparent that the computational power is very limited due to the fact that the black hole life-time is of the same order of the gate operation time. As a consequence, it is impossible to retrieve its information, within the life-time of a black hole, by externally coupling to the black hole qubits. However, we show that, in principle, coupling to some of the internal degrees of freedom allows acquiring knowledge about the micro-state. Still, due to the trivial complexity of operations that can be performed, there is no time advantage over the collection of Hawking radiation and subsequent decoding.

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Self-similar evaporation and collapse in the quantum portrait of black holes

Cited by 12 publications

References 46 publications

Thermal corpuscular black holes

Thermal corpuscular black holes

Thermal BEC Black Holes

Universality of black hole quantum computing

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