Classical instability of Kerr-AdS black holes and the issue of final state

Cardoso, Vítor; Dias, Óscar J. C.; Yoshida, Shijun

doi:10.1103/physrevd.74.044008

Cited by 120 publications

(141 citation statements)

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“…Such possible end-states were discussed in Refs. [56,63,64,65]. Some examples of rotating solutions with scalar hair were explicitly constructed in Refs.…”

Section: Black Hole Bombs In Anti-de Sitter Spacementioning

confidence: 99%

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Black hole bombs and explosions: from astrophysics to particle physics

Cardoso

2013

Gen Relativ Gravit

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Black holes are the elementary particles of gravity, the final state of sufficiently massive stars and of energetic collisions. With a forty-year long history, black hole physics is a fully-blossomed field which promises to embrace several branches of theoretical physics. Here I review the main developments in highly dynamical black holes with an emphasis on high energy black hole collisions and probes of particle physics via superradiance. This write-up, rather than being a collection of well known results, is intended to highlight open issues and the most intriguing results.Keywords Black holes · Superradiance · Cosmic Censorship · Transplanckian collisions IntroductionThe Kerr-Newman family of black holes in stationary four-dimensional, asymptotically flat spacetimes exhausts all possible electro-vacuum solutions in General Relativity. Theoretical aspects of black hole physics were fully developed decades ago, when the Kerr-Newman family was discovered and characterized. Most of the tools to understand black hole physics have been in place since that period and most processes involving black holes were controlled at the order-of-magnitude level for at least two decades. Perhaps due to these reasons, "black hole physics" conjures up images of horizons and time-warps and old-fashioned, frozen-in-time topics to lay audiences. However, in the last years the activity in the field is bubbling up Vitor Cardoso CENTRA, Departamento de Física, Instituto Superior Técnico, Universidade Técnica de Lisboa -UTL, Av. Rovisco Pais 1, 1049 Lisboa, Portugal E-mail: vitor.cardoso@ist.utl.pt Present address: Perimeter Institute for Theoretical Physics, Waterloo, Ontario N2J 2W9, Canada 2 Vitor Cardoso and the interest in these issues has widened, driven by several unrelated events at the observational/instrumental, technical and conceptual levels such as (i) our capacity to observationally scrutinize the region close to the horizon within a few Schwarzschild radii, with radio and deep infrared interferometry, of which we have seen but the first steps [1,2,3,4];(ii) the ability to measure black hole spins more accurately than ever before using X-ray spectroscopy [5,6] or "continuum-fitting" methods [7]. Measurement of black hole mass and spin is one necessary step in testing General Relativity [8]; (iii) huge technological progress in gravitational-wave observatories, some of which had been gathering data at design sensitivities for several years and are now being upgraded to sensitivities one order of magnitude higher (black hole binaries are thought to be among the first objects to ever be detected in the gravitational-wave spectrum);(iv) our ability to numerically evolve black hole binaries at the full nonlinear level [9,10,11] and its immediate importance for gravitational-wave searches and high-energy physics [12]; (v) improvement of perturbative schemes, either by an understanding of regularization schemes to handle the self-force [13,14], or by faster and more powerful methods to deal with the full ladder of pe...

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“…Such possible end-states were discussed in Refs. [56,63,64,65]. Some examples of rotating solutions with scalar hair were explicitly constructed in Refs.…”

Section: Black Hole Bombs In Anti-de Sitter Spacementioning

confidence: 99%

“…[55] that small rotating anti-de Sitter black holes are unstable against a superradiant mechanism. This study was generalized to other geometries and perturbation sectors [56,57,58,59,60]. A full analysis of gravitational perturbations in four-dimensions is underway [61].…”

Section: Black Hole Bombs In Anti-de Sitter Spacementioning

confidence: 99%

Black hole bombs and explosions: from astrophysics to particle physics

Cardoso

2013

Gen Relativ Gravit

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“…4-5. However, because these modes are nonaxisymmetric, they are prone to superradiant effects when interacting with the BH [14][15][16][17]34]: for small enough rotating BHs in AdS, the resonant frequency is that of pure AdS, ω ∼ 1/ and can be superradiant, i.e., ω < mΩ ,…”

Section: Parametersmentioning

confidence: 99%

“…Thus, one expects the structure of the perturbation spectrum to change completely and to even find linear and nonlinear instabilities in these systems [14][15][16][17][18]. A further interesting aspect of the different boundary conditions is that, for small AdS BHs (i.e., for BHs whose areal radius at the horizon is much smaller than the AdS scale) one expects imprints of asymptotically flat spacetimes in the early signal [19,20].…”

Section: Introductionmentioning

confidence: 99%

Black holes in anti–de Sitter spacetime: Quasinormal modes, tails, and flat spacetime

Cardoso¹,

Khanna²

2015

Phys. Rev. D

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Black holes (BHs) in asymptotically anti-de Sitter (AdS) spacetimes have been the subject of intense scrutiny, including detailed frequency-domain analysis and full nonlinear evolutions. Remarkably, studies of linearized perturbations in the time-domain are scarce or non-existing. We close this gap by evolving linearized scalar wavepackets in the background of rotating BHs in AdS spacetimes. Our results show a number of interesting features. Small BHs in AdS behave as asymptotically flat BHs for early/intermediate times, displaying the same ringdown modes and power-law tails. As the field bounces back and forth between the horizon and the timelike boundary it "thermalizes" and the modes of AdS settle in. Finally, we have indications that wavepackets in the vicinity of fastly spinning BHs grow exponentially in time, signalling a superradiant instability of the geometry previously reported through a frequency-domain analysis.

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“…The second case is to study bosonic field perturbation in black hole background with Dirichlet boundary condition at the asymptotic infinity. These background spacetimes include the rotating black holes in AdS spacetime [23][24][25][26][27][28][29], in Gödel universe [30,31], and in the linear dilaton background [32,33]. In all these cases, superradiance will trigger the instabilities of rotating black holes plus bosonic field perturbation.…”

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Superradiant Instability of D-Dimensional Reissner—Nordström Black Hole Mirror System*

Kun²,

Zhang³

2015

Commun. Theor. Phys.

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We analytically study the superradiant instability of charged massless scalar field in the background of D-dimensional Reissner-Nordström (RN) black hole caused by mirror-like boundary condition. By using the asymptotic matching method to solve the Klein-Gordon equation that govern the dynamics of scalar field, we have derived the expressions of complex parts of boxed quasinormal frequencies, and shown they are positive in the regime of superradiance. This indicates the charged scalar field is unstable in D-dimensional Reissner-Nordström (RN) black hole surrounded by mirror. However, the numerical work to calculate the boxed quasinormal frequencies in this system is still required in the future. [2][3][4][5] in 70s last century. When an impinging bosonic wave with frequency satisfying superradiant condition is scattered by event horizon of rotating black hole, the scattered wave will be amplified. If one places a reflecting mirror outside of the black hole, the amplified wave will be reflected into the black hole once again. So it is obvious that the bosonic wave will be bounced back and forth between event horizon and mirror. Meanwhile, the energy of the wave can become sufficiently large in this black hole mirror system until the reflecting mirror is destroyed.Recent studies of black hole bomb mechanism was initiated by Cardoso et. al. in [6]. See also the Refs. [7][8][9][10][11][12] for the recent studies on this topic. Black hole bomb mechanism can also be realized in the following two cases. In the first case, the mass term of bosonic field plays the role of reflecting mirror, for example, the systems investigated in [13][14][15][16][17][18][19][20][21][22]. The second case is to study bosonic field perturbation in black hole background with Dirichlet boundary condition at the asymptotic infinity. These background spacetimes include the rotating black holes in AdS spacetime [23][24][25][26][27][28][29], in Gödel universe [30,31], and in the linear dilaton background [32,33]. In all these cases, superradiance will trigger the instabilities of rotating black holes plus bosonic field perturbation.For a charged scalar wave in the background of spherical symmetric charged black hole, the wave scattered by event horizon will also undergo superradiant process if the frequency of this impinging wave satisfying superradiant condition [34]. However, it was proved by Hod in [35,36] that, for four dimensional RN black holes, the existence of a trapping potential well outside black hole and superradiant amplification of trapped modes cannot be satisfied simultaneously. This means that the four dimensional RN black holes are stable under the perturbations * Corresponding author. Electronic mail: 021149@htu.cn of massive charged scalar fields. Soon after, Degollado et. al. [37,38] found that the same system can be made unstable by adding a mirror-like boundary condition like the case of the Kerr black hole. In [39], we also shown that the mass term of scalar field in charged stringy black hole is never able to generate a...

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Classical instability of Kerr-AdS black holes and the issue of final state

Cited by 120 publications

References 37 publications

Black hole bombs and explosions: from astrophysics to particle physics

Black hole bombs and explosions: from astrophysics to particle physics

Black holes in anti–de Sitter spacetime: Quasinormal modes, tails, and flat spacetime

Superradiant Instability of D-Dimensional Reissner—Nordström Black Hole Mirror System*

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