Black hole area–angular-momentum inequality in nonvacuum spacetimes

Jaramillo, José Luis; Reiris, Martin; Dain, Sergio

doi:10.1103/physrevd.84.121503

Cited by 56 publications

(138 citation statements)

References 32 publications

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“…The BHs that violated the ζ = 1 bound were not able to sustain super-extremality and simultaneously retain axisymmetry. Our results are also consistent with work by Jaramillo, Reiris and Dain [16] that appeared soon after the submission of our manuscript. The work in Ref.…”

Section: Discussionsupporting

confidence: 83%

“…The work in Ref. [16] proved that ζ ≤ 1 holds for outermost stably marginally trapped surfaces that are axisymmetric in the presence of surrounding matter satisfying the dominant energy condition. The proof did not require axisymmetry of the exterior matter, only for the trapped surface.…”

Section: Discussionmentioning

confidence: 99%

“…It has been then suggested [5,6] that a quantity more suitable to investigate extremality is ζ ≡ |J|/(2M 2 H ), or equivalently ζ ≡ 8π|J|/A [16]. In terms of ζ, the spin parameter χ and the surface gravity κ take the form…”

mentioning

confidence: 99%

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Superextremal spinning black holes via accretion

2011

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A Kerr black hole with mass M and angular momentum J satisfies the extremality inequality |J| ≤ M 2 . In the presence of matter and/or gravitational radiation, this bound needs to be reformulated in terms of local measurements of the mass and the angular momentum directly associated with the black hole. The isolated and dynamical horizon framework provides such quasi-local characterization of black hole mass and angular momentum. With this framework, it is possible in axisymmetry to reformulate the extremality limit as |J| ≤ 2 M 2 H , with MH the irreducible mass of the black hole computed from its apparent horizon area and J obtained using a rotational Killing vector field on the apparent horizon. The |J| ≤ 2 M 2 H condition is also equivalent to requiring a non-negative black hole surface gravity. We present numerical experiments of an accreting black hole that temporarily violates this extremality inequality. The initial configuration consists of a single, rotating black hole surrounded by a thick, shell cloud of negative energy density. For these numerical experiments, we introduce a new matter-without-matter evolution method.

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Section: Discussionsupporting

confidence: 83%

Section: Discussionmentioning

confidence: 99%

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Superextremal spinning black holes via accretion

2011

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“…Recall [31,32,33] that there is also a universal bound on the Komar angular momentum (4). To confirm this for the MKN horizons we need to demonstrate that…”

Section: Komar Angular Momentum Is Bound By Areamentioning

confidence: 99%

“…Again assuming an axisymmetric and stable MOTS it has been demonstrated [31,32,33] that for any matter fields satisfying the dominant energy condition, the possible values of the Komar angular momentum are bound by the areal radius:…”

Section: Introductionmentioning

confidence: 99%

Insights from Melvin–Kerr–Newman spacetimes

Booth

Hunt

Palomo-Lozano

et al. 2015

Class. Quantum Grav.

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Abstract. We examine several aspects of black hole horizon physics using the Melvin-Kerr-Newman (MKN) family of spacetimes. Roughly speaking these are black holes immersed in a distorting background magnetic field and unlike the standard Kerr-Newman (KN) family they are not asymptotically flat. As exact solutions with horizons that can be highly distorted relative to KN, they provide a good testbed for ideas about and theorems constraining black hole horizons.We explicitly show that MKN horizons with fixed magnetic field parameter may be uniquely specified by their area, charge and angular momentum and that the charge and angular momentum are bound by horizon area in the same way as for KN. As expected, extremal MKN horizons are geometrically isomorphic to extremal KN horizons and the geometric distortion of near-extremal horizons is constrained by their proximity to extremality. At the other extreme, Melvin-Schwarzschild (MS) solutions may be infinitely distorted, however for intermediate cases any non-zero charge or angular momentum restricts distortions to be finite. These properties are in agreement with known theorems but are seen to be satisfied in interesting and non-trivial ways.

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