Distorted stationary rotating black holes

Shoom, Andrey A.

doi:10.1103/physrevd.91.064030

Cited by 10 publications

(15 citation statements)

References 62 publications

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“…"Apparently, the rich structure of the Weyl-type solutions is far from completely explored." is the last sentence of paper [1] and we beg to borrow it as the first one. 1 The quoted paper deals with stationary situation, but the statement even holds for a static case which will be considered here.…”

Section: Introductionmentioning

confidence: 99%

“…is the last sentence of paper [1] and we beg to borrow it as the first one. 1 The quoted paper deals with stationary situation, but the statement even holds for a static case which will be considered here. More specifically, we will focus on static, axially symmetric and asymptotically flat gravitational fields generated by thin circular rings.…”

Section: Introductionmentioning

confidence: 99%

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Static axisymmetric rings in general relativity: How diverse they are

Semerák

2016

Phys. Rev. D

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Three static and axially symmetric (Weyl-type) ring singularities -the Majumdar-Papapetroutype (extremally charged) ring, the Bach-Weyl ring and the Appell ring -are studied in general relativity in order to show how remarkably the geometries in their vicinity differ from each other. This is demonstrated on basic measures of the rings and on invariant characteristics given by the metric and by its first and second derivatives (lapse, gravitational acceleration and curvature), and also on geodesic motion. The results are also compared against the Kerr space-time which possesses a ring singularity too. The Kerr solution is only stationary, not static, but in spite of the consequent complication by dragging, its ring appears to be simpler than the static rings. We show that this mainly applies to the Bach-Weyl ring, although this straightforward counter-part of the Newtonian homogeneous circular ring is by default being taken as the simplest ring solution, and although the other two static ring sources may seem more "artificial". The weird, directional deformation around the Bach-Weyl ring probably indicates that a more adequate coordinate representation and interpretation of this source should exists.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Static axisymmetric rings in general relativity: How diverse they are

Semerák

2016

Phys. Rev. D

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“…In this paper, we carry out a detailed analysis of the horizon structure of rotating Einstein-Born-Infeld black hole and we explicitly make manifest the effect β has. Recently, the horizon structure has been studied for various space-time geometries, see, e.g., [19][20][21][22]. We also investigate the apparent shape of the non-rotating Einstein-Born-Infeld black hole to visualize the shape of the shadow and compare the results with the images for the corresponding Reissner-Nordstrom black hole.…”

Section: Introductionmentioning

confidence: 99%

Horizon structure of rotating Einstein–Born–Infeld black holes and shadow

2016

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We investigate the horizon structure of the rotating Einstein-Born-Infeld solution which goes over to the Einstein-Maxwell's Kerr-Newman solution as the BornInfeld parameter goes to infinity (β → ∞). We find that for a given β, mass M, and charge Q, there exist a critical spinning parameter a E and r E H , which corresponds to an extremal Einstein-Born-Infeld black hole with degenerate horizons, and a E decreases and r E H increases with increase of the Born-Infeld parameter β, while a < a E describes a non-extremal Einstein-Born-Infeld black hole with outer and inner horizons. Similarly, the effect of β on the infinite redshift surface and in turn on the ergo-region is also included. It is well known that a black hole can cast a shadow as an optical appearance due to its strong gravitational field. We also investigate the shadow cast by the both static and rotating Einstein-Born-Infeld black hole and demonstrate that the null geodesic equations can be integrated, which allows us to investigate the shadow cast by a black hole which is found to be a dark zone covered by a circle. Interestingly, the shadow of an Einstein-Born-Infeld black hole is slightly smaller than for the Reissner-Nordstrom black hole, which consists of concentric circles, for different values of the Born-Infeld parameter β, whose radius decreases with increase of the value of the parameter β. Finally, we have studied observable distortion parameter for shadow of the rotating Einstein-Born-Infeld black hole. a e-mails: farruh@astrin.uz;

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“…The distortions in these spacetimes are induced by distortions of the asymptotic structure and by similar methods one can also distort both Reissner-Nordström [7,8] and KN [9,10] solutions. Most generally, stationary axisymmetric electrovac spacetimes may be written as Ernst solutions [11] and there are many solution generating techniques that take existing solutions and generate new ones [12].…”

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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Distorted stationary rotating black holes

Cited by 10 publications

References 62 publications

Static axisymmetric rings in general relativity: How diverse they are

Static axisymmetric rings in general relativity: How diverse they are

Horizon structure of rotating Einstein–Born–Infeld black holes and shadow

Insights from Melvin–Kerr–Newman spacetimes

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