Horizon instability of extremal Kerr black holes: Nonaxisymmetric modes and enhanced growth rate

Casals, Marc; Gralla, Samuel E.; Zimmerman, Peter

doi:10.1103/physrevd.94.064003

Cited by 50 publications

(129 citation statements)

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“…Based on numerical studies of quasinormal modes on extremal Kerr [2,12], the expectation is that φ with a fixed azimuthal number m = 0 arising from initial data supported away from H + will decay slower than axisymmetric φ (for which m = 0) both away from H + and along H + .…”

Section: Linear Waves In the Exterior Region Of Extremal Kerrmentioning

confidence: 99%

Linear Waves in the Interior of Extremal Black Holes II

Gajic

2017

Ann. Henri Poincaré

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Abstract.We consider solutions to the linear wave equation in the interior region of extremal Kerr black holes. We show that axisymmetric solutions can be extended continuously beyond the Cauchy horizon and, moreover, that if we assume suitably fast polynomial decay in time along the event horizon, their local energy is finite. We also extend these results to nonaxisymmetric solutions on slowly rotating extremal Kerr-Newman black holes. These results are the analogues of results obtained in Gajic (Commun Math Phys 353(2), 717-770, 2017) for extremal Reissner-Nordström and stand in stark contrast to previously established results for the subextremal case, where the local energy was shown to generically blow up at the Cauchy horizon.

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Section: Linear Waves In the Exterior Region Of Extremal Kerrmentioning

confidence: 99%

Linear Waves in the Interior of Extremal Black Holes II

Gajic

2017

Ann. Henri Poincaré

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“…Here Φ is the scalar field, v is ingoing time (equal to affine time on the future degenerate horizon H), r is the areal radius, C is some constant, and n ≥ 2 derivatives are taken. The original result (1.1) held only for initial data that was non-zero on the event horizon, but it soon became clear that the instability persists for data supported arbitrarily far away [8][9][10], although sometimes with different rates [11]. The result was also extended to near-extremal black holes, where the growth occurs transiently (for a time of order the inverse temperature) near the horizon [8,[12][13][14].…”

Section: Introductionmentioning

confidence: 99%

Semi-local quantum criticality and the instability of extremal planar horizons

Gralla

Ravishankar

Zimmerman

2018

J. High Energ. Phys.

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We show that the Aretakis instability of compact extremal horizons persists in the planar case of interest to holography and discuss its connection with the emergence of "semi-local quantum criticality" in the field theory dual. In particular, the spatially localized power-law decay of this critical phase corresponds to spatially localized power-law growth of stress-energy on the horizon. For near-extremal black holes these phenomena occur transiently over times of order the inverse temperature. The boundary critical phase is characterized by an emergent temporal conformal symmetry, and the bulk instability seems to be essential to preserving the symmetry in the presence of interactions. We work primarily in the solvable example of charged scalar perturbations of fivedimensional (near-)extremal planar Reissner-Nordström anti-de Sitter spacetime and argue that the conclusions hold more generally. a

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“…[43]) if the NE family is a charged version of the zero-damping modes discussed recently in the context of rotating Kerr BHs [45]. It is also unclear if there is any relation between such long lived modes and the instability of exactly extremal geometries [46,47].…”

Section: Physical Review Letters 120 031103 (2018)mentioning

confidence: 99%

A Possible Failure of Determinism in General Relativity

Reall

2018

Physics

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The fate of Cauchy horizons, such as those found inside charged black holes, is intrinsically connected to the decay of small perturbations exterior to the event horizon. As such, the validity of the strong cosmic censorship (SCC) conjecture is tied to how effectively the exterior damps fluctuations. Here, we study massless scalar fields in the exterior of Reissner-Nordström-de Sitter black holes. Their decay rates are governed by quasinormal modes of the black hole. We identify three families of modes in these spacetimes: one directly linked to the photon sphere, well described by standard WKB-type tools; another family whose existence and time scale is closely related to the de Sitter horizon; finally, a third family which dominates for near-extremally charged black holes and which is also present in asymptotically flat spacetimes. The last two families of modes seem to have gone unnoticed in the literature. We give a detailed description of linear scalar perturbations of such black holes, and conjecture that SCC is violated in the near extremal regime.

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Horizon instability of extremal Kerr black holes: Nonaxisymmetric modes and enhanced growth rate

Cited by 50 publications

References 41 publications

Linear Waves in the Interior of Extremal Black Holes II

Linear Waves in the Interior of Extremal Black Holes II

Semi-local quantum criticality and the instability of extremal planar horizons

A Possible Failure of Determinism in General Relativity

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