Nonlinear instability of Kerr-type Cauchy horizons

Brady, P. R.; Chambers, Chris M.

doi:10.1103/physrevd.51.4177

Cited by 54 publications

(69 citation statements)

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“…This analysis revealed that in the spinning case, too, there is a null, weak, curvature singularity at the IH. The main results of the perturbative analysis [12] were later confirmed by several non-perturbative local analyses [14][15][16][17].…”

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confidence: 58%

“…The actual formation of the null weak inner-horizon singularity in a generic gravitational collapse has been verified in an explicit manner by the perturbative analyses [12,13,18]. (The local consistency and genericity of this singularity have been verified also by several non-perturbative local analyses [14][15][16][17].) On the other hand, the analyses of the BKL singularity indicated the local consistency of this singularity, and probably also its inevitable occurrence in certain cosmological models, but so far not in asymptotically-flat situations.…”

Section: Comparing the Asymptotic Forms Of The Various Terms H (J)mentioning

confidence: 97%

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Oscillatory Null Singularity inside Realistic Spinning Black Holes

Ori

1999

Phys. Rev. Lett.

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We calculate the asymptotic behavior of the curvature scalar (Riemann) 2 near the null weak singularity at the inner horizon of a generic spinning black hole, and show that this scalar oscillates infinite number of times while diverging. The dominant parallelly-propagated Riemann components oscillate in a similar manner. This oscillatory behavior, which is in a remarkable contrast to the monotonic mass-inflation singularity in spherical charged black holes, is caused by the dragging of inertial frames due to the black-hole's spin.One of the major challenges in Classical general relativity during the last few decades has been to explore the nature of the spacetime singularities which form in gravitational collapse.The existence of singularities inside black holes has been verified by several mathematical theorems [1]. However, the singularity theorems do not tell us much about the location and features of these singularities.It is widely anticipated that the realistic astrophysical black holes are rapidly spinning is a null hypersurface located inside the BH. This hypersurface, also known as the Cauchy horizon [1], marks the boundary of predictability for physical fields whose initial data are specified outside the BH. In the pure Kerr geometry, the IH is a perfectly smooth surface.Penrose [5] pointed out, however, that ingoing electromagnetic or gravitational perturbations are infinitely blue-shifted at the IH. He therefore suggested that in a more realistic BH, which 1

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mentioning

confidence: 58%

Section: Comparing the Asymptotic Forms Of The Various Terms H (J)mentioning

confidence: 97%

Oscillatory Null Singularity inside Realistic Spinning Black Holes

Ori

1999

Phys. Rev. Lett.

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“…dynamical instability of the inner horizon of rotating and charged black holes is triggered by generic small perturbations, cutting off the region behind it and supporting the strong cosmic censorship conjecture [1,2]. Numerical and analytic studies of shells of matter in BTZ black holes suggest an instability at the inner horizon [13].…”

Section: Is a Penrose Diagrammentioning

confidence: 99%

“…In asymptotically flat space, numerical simulations and analytic studies have shown that a generic, small perturbation can cause such an inner horizon to itself collapse to a singularity [1,2] (for a more modern study in the context of classical gravity see [3]). This is a manifestation of strong cosmic censorship [4].…”

Section: Introductionmentioning

confidence: 99%

Beyond the veil: Inner horizon instability and holography

Balasubramanian

Levi

2004

Phys. Rev. D

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We show that scalar perturbations of the eternal, rotating BTZ black hole should lead to an instability of the inner (Cauchy) horizon, preserving strong cosmic censorship. Because of backscattering from the geometry, plane wave modes have a divergent stress tensor at the event horizon, but suitable wavepackets avoid this difficulty, and are dominated at late times by quasinormal behavior. The wavepackets have cuts in the complexified coordinate plane that are controlled by requirements of continuity, single-valuedness and positive energy. Due to a focusing effect, regular wavepackets nevertheless have a divergent stress-energy at the inner horizon, signaling an instability. This instability, which is localized behind the event horizon, is detected holographically as a breakdown in the semiclassical computation of dual CFT expectation values in which the analytic behavior of wavepackets in the complexified coordinate plane plays an integral role. In the dual field theory, this is interpreted as an encoding of physics behind the horizon in the entanglement between otherwise independent CFTs. * Electronic address: vijay@endive.hep.upenn.edu † Electronic address: tslevi@student.physics.upenn.edu 1 Contents

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“…We employ a double-null foliation developed by Hayward [2] (mainly for the characteristic initial value problem and the trapping horizon definition) and adapted by Brady and Chambers [6] to study a nonlinear stability of Kerr-type Cauchy horizons. The procedure is based on a local foliation by closed orientable 2-surfaces S with smooth embedding φ : S × [0,U) × [0,V) → M and induced spatial metric h ab on S with corresponding covariant derivative D a .…”

Section: Quasilocal Horizonsmentioning

confidence: 99%