Resonance spectra of caged black holes

Hod, Shahar

doi:10.1140/epjc/s10052-014-3137-3

Cited by 20 publications

(35 citation statements)

References 51 publications

(112 reference statements)

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“…If the system has electric charge, we can also have static black hole bomb systems [2][3][4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19]. All we need is a complex scalar field with charge q scattering a Reissner-Nordström black hole with chemical potential µ that is placed inside a box that reflects the scalar waves.…”

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confidence: 99%

Evading no-hair theorems: Hairy black holes in a Minkowski box

Dias

Masachs

2018

Phys. Rev. D

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We find hairy black holes of Einstein-Maxwell theory with a complex scalar field that is confined inside a box in a Minkowski background. These regular hairy black holes are asymptotically flat and thus the presence of the box or mirror allows to evade well-known no-hair theorems. We also find the Israel surface stress tensor that the confining box must have to obey the energy conditions. In the zero horizon radius limit, these hairy black holes reduce to a regular asymptotically flat hairy soliton. We find our solutions using perturbation theory. At leading order, a hairy black hole can be seen as a Reissner-Nordstrom black hole placed on top of a hairy soliton with the same chemical potential (so that the system is in thermodynamic equilibrium). The hairy black holes merge with the Reissner-Nordstrom black hole family at the onset of the superradiant instability. When they co-exist, for a given energy and electric charge, hairy black holes have higher entropy than caged Reissner-Nordstrom black holes. Therefore, our hairy black holes are the natural candidates for the endpoint of charged superradiance in the Reissner-Nordstrom black hole mirror system. * Electronic address: ojcd1r13@soton.ac.uk † Electronic address: rmg1e15@soton.ac.uk

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confidence: 99%

Evading no-hair theorems: Hairy black holes in a Minkowski box

Dias

Masachs

2018

Phys. Rev. D

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“…of this relation. 7 Note that the black-hole surface area 8π M R H plays the role of an adiabatic invariant (see, Bekenstein [10] (8) for the evolution of the black-hole angular velocity during an adiabatic assimilation process of the orbiting ring by the central black hole.…”

Section: The Continuous (Smooth) Behavior Of the Black-hole Angular Vmentioning

confidence: 99%

“…Taking cognizance of Eqs. (1) and (11), and using the continuity argument (8) for the evolution of the black-hole angular velocity during the adiabatic assimilation process of the ring into the central black hole, one finds the characteristic angular-velocity/angular-momentum asymptotic relation …”

Section: The Continuous (Smooth) Behavior Of the Black-hole Angular Vmentioning

confidence: 99%

“…The general-relativistic problem of a slowly spinning black hole surrounded by a thin orbiting ring was studied perturbatively by Will [4,5] (see also [6][7][8]). It was shown in [4] that, due to the well-known phenomenon of dragging of inertial frames by the orbiting ring, the angular velocity BH-ring H 1 of the central black hole in the composed black- 1 We use the symbol BH-ring H to denote the angular velocity of the black-hole horizon in the composed black-hole-ring system.…”

Section: Introductionmentioning

confidence: 99%

“…of (8) refers to the angular velocity of the final Kerr (vacuum) black hole (that is, after it assimilated the ring).…”

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Dragging of inertial frames in the composed black-hole–ring system

Hod

2015

Eur. Phys. J. C

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A well-established phenomenon in general relativity is the dragging of inertial frames by a spinning object. In particular, due to the dragging of inertial frames by a ring orbiting a central black hole, the angular velocity BH-ring H of the black-hole horizon in the composed black-hole-ring system is no longer related to the black-hole angular momentum J H by the simple Kerr-like (vacuum) relation Kerr H (J H ) = J H /2M 2 R H (here M and R H are the mass and horizon-radius of the black hole, respectively). Will has performed a perturbative treatment of the composed black-hole-ring system in the regime of slowly rotating black holes and found the explicit relation BH-ring H(J H = 0, J R , R) = 2J R /R 3 for the angular velocity of a central black hole with zero angular momentum, where J R and R are respectively the angular momentum of the orbiting ring and its proper circumferential radius. Analyzing a sequence of black-hole-ring configurations with adiabatically varying (decreasing) circumferential radii, we show that the expression found by Will for BH-ring H (J H = 0, J R , R) implies a smooth transition of the central black-hole angular velocity from its asymptotic nearhorizon value H are the new parameters of the resulting Kerr (vacuum) black hole after it assimilated the orbiting ring]. We use this important observation in order to generalize the result of Will to the regime of black-hole-ring configurations in which the central black holes possess non-zero angular momenta. In particular, it is shown that the continuity argument (namely, the characteristic smooth evolution of the black-hole angular velocity during an adiabatic assimilation process of the a e-mail: shaharhod@gmail.com ring into the central black hole) yields a concrete prediction for the angular-velocity/angular-momentum asymptotic functional relationof generic (that is, with J H = 0) black-hole-ring configurations. Remarkably, we find the simple universal rela-3 for the asymptotic deviation of the black-hole angular velocity in the composed black-hole-ring system from the corresponding angular velocity of the unperturbed (vacuum) Kerr black hole with the same angular momentum.

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Spectroscopy of rotating linear dilaton black holes from boxed quasinormal modes

Сакалли

Tokgöz

2016

Annalen der Physik

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Numerical studies of the coupled Einstein-Klein-Gordon system have recently revealed that confined scalar fields generically collapse to form caged black holes. In the light of this finding, we analytically study the characteristic resonance spectra of the confined scalar fields in rotating linear dilaton black hole geometry. Confining mirrors (cage) are assumed to be placed in the near-horizon region of a caged rotating linear dilaton black hole rm−r 2 r 2 ≪ 1 (rm is the radius of the cage and r2 represents the event horizon). The radial part of the Klein-Gordon equation is written as a Schrödinger-like wave equation, which reduces to a Bessel differential equation around the event horizon. Using analytical tools and proper boundary conditions, we obtain the boxed-quasinormal mode frequencies of the caged rotating linear dilaton black hole. Finally, we employ Maggiore's method, which evaluates the transition frequency in the adiabatic invariant quantity from the highly damped quasinormal modes, in order to investigate the entropy/area spectra of the rotating linear dilaton black hole.

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Resonance spectra of caged black holes

Cited by 20 publications

References 51 publications

Evading no-hair theorems: Hairy black holes in a Minkowski box

Evading no-hair theorems: Hairy black holes in a Minkowski box

Dragging of inertial frames in the composed black-hole–ring system

Spectroscopy of rotating linear dilaton black holes from boxed quasinormal modes

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