Astrophysical Bose-Einstein condensates and superradiance

Kühnel, Florian; Rampf, Cornelius

doi:10.1103/physrevd.90.103526

Cited by 19 publications

(22 citation statements)

References 61 publications

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“…[26,27]. Finally, we would like to remark that, although we found that M M 0 for very large compactness, and one could thus infer that matter become almost irrelevant inside a black hole [10], the above picture inherently requires the presence of matter, whose role in black hole physics we believe needs more investigations [22][23][24][25].…”

Section: Conclusion and (Quantum) Outlookmentioning

confidence: 84%

Bootstrapped Newtonian stars and black holes

2019

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We study equilibrium configurations of a homogenous ball of matter in a bootstrapped description of gravity which includes a gravitational self-interaction term beyond the Newtonian coupling. Both matter density and pressure are accounted for as sources of the gravitational potential for test particles. Unlike the general relativistic case, no Buchdahl limit is found and the pressure can in principle support a star of arbitrarily large compactness. By defining the horizon as the location where the escape velocity of test particles equals the speed of light, like in Newtonian gravity, we find a minimum value of the compactness for which this occurs. The solutions for the gravitational potential here found could effectively describe the interior of macroscopic black holes in the quantum theory, as well as predict consequent deviations from general relativity in the strong field regime of very compact objects.

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Section: Conclusion and (Quantum) Outlookmentioning

confidence: 84%

Bootstrapped Newtonian stars and black holes

2019

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“…where the normalisation N H = √ 3/ π 2 − 6 ζ(3) 1.06, we introduced the dimensionless variables 5) and the states |E i = m 1/2 |ω i , such that the identity in the continuum can be written as…”

Section: Bec With Thermal Quantum Hairmentioning

confidence: 99%

“…Since the source represented by such quantum states is by construction (mostly) localised within R H , this shows that r = r H is a horizon for the system. Given the spectral coefficients (3.20), the corresponding horizon wave-function reads 5) where the state |R H represents the discrete part of the spectrum and is defined so that 6) and the states…”

Section: Horizon Wave-function and Backreactionmentioning

confidence: 99%

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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“…The quantum fluctuations approximately follow a Gaussian distribution centered around zero. The depletion process is given by a Poisson distribution [18][19][20][21].…”

Section: Competing Fluctuationsmentioning

confidence: 99%

“…In fact, some phenomena, like Hawking radiation, the Bekenstein entropy, or, the information paradox, can only be fully understood in this quantum picture [9][10][11][12][13][14][15] (cf. also [16][17][18][19][20][21][22][23][24][25][26][27] for recent progress).…”

Section: Introductionmentioning

confidence: 99%

Corpuscular consideration of eternal inflation

Kühnel

Sandstad

2015

Eur. Phys. J. C

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We review the paradigm of eternal inflation in the light of the recently proposed corpuscular picture of spacetime. Comparing the strength of the average fluctuation of the field up its potential with that of quantum depletion, we show that the latter can be dominant. We then study the full respective distributions in order to show that the fraction of the space-time which has an increasing potential is always below the eternal-inflation threshold. We prove that for monomial potentials eternal inflaton is excluded. This is likely to hold for other models as well.

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Astrophysical Bose-Einstein condensates and superradiance

Cited by 19 publications

References 61 publications

Bootstrapped Newtonian stars and black holes

Bootstrapped Newtonian stars and black holes

Thermal corpuscular black holes

Corpuscular consideration of eternal inflation

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