Black holes in a magnetic universe

Ernst, Frederick J.

doi:10.1063/1.522781

Cited by 260 publications

(219 citation statements)

References 7 publications

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“…The Melvin-Kerr-Newman (MKN) family of solutions [14,15] is described by a metric and electromagnetic potential respectively of the form…”

Section: Form Of the Solutionsmentioning

confidence: 99%

“…In this paper we focus on a class of solutions generated by Harrison transforms of KN spacetimes. These MelvinKerr-Newman (MKN) spacetimes describe a black hole immersed in a background magnetic field (see, for example, [13,14,15,16,17,18,19,20]). Though quite complicated algebraically they are conceptually relatively easy to work with as the degree of distortion is parameterized by a single parameter B which is associated with the distorting magnetic field.…”

Section: Introductionmentioning

confidence: 99%

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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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“…The Melvin-Kerr-Newman (MKN) family of solutions [14,15] is described by a metric and electromagnetic potential respectively of the form…”

Section: Form Of the Solutionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Insights from Melvin–Kerr–Newman spacetimes

Booth

Hunt

Palomo-Lozano

et al. 2015

Class. Quantum Grav.

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show abstract

“…They can nonetheless be physically interesting as descriptions of the near horizon geometry of isolated black holes which are distorted by the presence of far away matter [6,7]. There are also solutions which describe a black hole immersed in a magnetic field [8]. However, in all these cases, the distorted black holes themselves do not carry any charge.…”

Section: Introductionmentioning

confidence: 99%

Distorted Black Holes With Charge

Fairhurst

Krishnan

2001

Int. J. Mod. Phys. D

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We present new solutions to the Einstein-Maxwell equations representing a class of charged distorted black holes. These solutions are static-axisymmetric and are generalizations of the distorted black hole solutions studied by Geroch and Hartle. Physically, they represent a charged black hole distorted by external matter fields. We discuss the zeroth and first law for these black holes. The first law is proved in two different forms, one motivated by the isolated horizon framework and the other using normalizations at infinity.

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“…In that case, one can go ahead and find the angular momentum using equation (25). However, we are also interested in the more general case, when there is an axial symmetry, but the coordinates used in the simulation are not adapted to it.…”

Section: Finding the Killing Vectormentioning

confidence: 99%

“…We use a second order interpolation method for this purpose. This finally gives us the normalized symmetry vector ϕ a , which is used to calculate J ∆ from equation (25).…”

Section: Finding the Killing Vectormentioning

confidence: 99%

Introduction to isolated horizons in numerical relativity

et al. 2003

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We present a coordinate-independent method for extracting mass (M∆) and angular momentum (J∆) of a black hole in numerical simulations. This method, based on the isolated horizon framework, is applicable both at late times when the black hole has reached equilibrium, and at early times when the black holes are widely separated. Assuming that the spatial hypersurfaces used in a given numerical simulation are such that apparent horizons exist and have been located on these hypersurfaces, we show how J∆ and M∆ can be determined in terms of only those quantities which are intrinsic to the apparent horizon. We also present a numerical method for finding the rotational symmetry vector field (required to calculate J∆) on the horizon.

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Black holes in a magnetic universe

Cited by 260 publications

References 7 publications

Insights from Melvin–Kerr–Newman spacetimes

Insights from Melvin–Kerr–Newman spacetimes

Distorted Black Holes With Charge

Introduction to isolated horizons in numerical relativity

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