Interior of a charged distorted black hole

Abdolrahimi, Shohreh; Frolov, Valeri P.; Shoom, Andrey A.

doi:10.1103/physrevd.80.024011

Cited by 20 publications

(50 citation statements)

References 50 publications

(82 reference statements)

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“…For the parameters one can choose, e.g., the mass M, the angular momentum J, and the electric charge Q of the black hole. 1 For a solitary black hole, which is characterized by the existence of an event horizon, the relation…”

Section: A Universal Inequality For Sub-extremal Black Holesmentioning

confidence: 99%

Universal properties of distorted Kerr–Newman black holes

2010

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We discuss universal properties of axisymmetric and stationary configurations consisting of a central black hole and surrounding matter in Einstein-Maxwell theory. In particular, we find that certain physical equations and inequalities (involving angular momentum, electric charge and horizon area) are not restricted to the Kerr-Newman solution but can be generalized to the situation where the black hole is distorted by an arbitrary axisymmetric and stationary surrounding matter distribution.

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Section: A Universal Inequality For Sub-extremal Black Holesmentioning

confidence: 99%

Universal properties of distorted Kerr–Newman black holes

2010

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“…where K is the Gaussian curvature of the horizon twodimensional spacelike surface (for details see, e.g., [60,65]). For the metric (11) with the quadrupole distortion fields (13)- (14), this expression reads…”

Section: B Quadrupole Distortionmentioning

confidence: 99%

Metamorphoses of a photon sphere

Shoom

2017

Phys. Rev. D

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There are circular planar null geodesics at r = 3M around a Schwarzschild black hole of mass M . These geodesics form a photon sphere. Null geodesics of the Schwarzschild space-time which do not form the photon sphere are either escape to null infinity or get captured by the black hole. Thus, from the dynamical point of view, the photon sphere represents a smooth basin boundary that separates the basins of escape and capture of the dynamical system governing the null geodesics. Here we consider a Schwarzschild black hole distorted by an external, static, and axisymmetric quadrupolar gravitational field defined by a quadrupole moment q. We study null geodesics around such a black hole and show that the photon sphere does not survive the distortion. For q −0.017001 it transforms into a fractal basin boundary that indicates chaotic behavior of the null geodesics. We calculate the box-counting fractal dimension of the basin boundary and the related uncertainty exponent, which depend on the value of the quadrupole moment.

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“…Instead the distortions are induced by a divergent asymptotic infinity. As such if we are interested in potential astrophysical effects we must restrict our attention to timelike and null geodesics in the vicinity of the black hole horizon and consider these solutions as local static distorted black holes (see, e.g., [32,33,[35][36][37]). Our goal is to see how distortion affects the geodesics.…”

Section: Introductionmentioning

confidence: 99%

Geodesic motion around a distorted static black hole

2016

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In this paper we study geodesic motion around a distorted Schwarzschild black hole. We consider both timelike and null geodesics which are confined to the black hole's equatorial plane. Such geodesics generically exist if the distortion field has only even interior multipole moments and so the field is symmetric with respect to the equatorial plane. We specialize to the case of distortions defined by a quadrupole Weyl moment. An analysis of the effective potential for equatorial timelike geodesics shows that finite stable orbits outside the black hole are possible only for q ∈ (qmin, qmax], where qmin ≈ −0.0210 and qmax ≈ 2.7086 × 10 −4 , while for null equatorial geodesics a finite stable orbit outside the black hole is possible only for q ∈ [qmin, 0). Moreover, the innermost stable circular orbits (ISCOs) are closer to the distorted black hole horizon than those of an undistorted Schwarzschild black hole for q ∈ (qmin, 0) and a null ISCO exists for q = qmin. These results shows that an external distortion of a negative and sufficiently small quadrupole moment tends to stabilize motion of massive particles and light.

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Interior of a charged distorted black hole

Cited by 20 publications

References 50 publications

Universal properties of distorted Kerr–Newman black holes

Universal properties of distorted Kerr–Newman black holes

Metamorphoses of a photon sphere

Geodesic motion around a distorted static black hole

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