Physics of the interior of a spherical, charged black hole with a scalar field

Hansen, Jakob; Khokhlov, A. M.; Новиков, И. Д.

doi:10.1103/physrevd.71.064013

Cited by 49 publications

(107 citation statements)

References 30 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Analytic and numerical work on spherically symmetric collapse has commonly modeled the fluid accreted by the black hole as a massless scalar field, usually taken to be uncharged [7,9,11,12,13,14,15,24,27,32,33,38,50,56], but sometimes charged [26,46,48,49,61,71]. A key property of a massless scalar field is that it allows waves to counter-stream relativistically through each other, which allows the phenomenon of mass inflation on the Cauchy horizon to occur.…”

Section: Introductionmentioning

confidence: 99%

Inside charged black holes. I. Baryons

Hamilton

Pollack²

2005

Phys. Rev. D

View full text Add to dashboard Cite

An extensive investigation is made of the interior structure of self-similar accreting charged black holes. In this, the first of two papers, the black hole is assumed to accrete a charged, electrically conducting, relativistic baryonic fluid. The mass and charge of the black hole are generated selfconsistently by the accreted material. The accreted baryonic fluid undergoes one of two possible fates: either it plunges directly to the spacelike singularity at zero radius, or else it drops through the Cauchy horizon. The baryons fall directly to the singularity if the conductivity either exceeds a certain continuum threshold κ∞, or else equals one of an infinite spectrum κn of discrete values. Between the discrete values κn, the solution is characterized by the number of times that the baryonic fluid cycles between ingoing and outgoing. If the conductivity is at the continuum threshold κ∞, then the solution cycles repeatedly between ingoing and outgoing, displaying a discrete self-similarity reminiscent of that observed in critical collapse. Below the continuum threshold κ∞, and except at the discrete values κn, the baryonic fluid drops through the Cauchy horizon, and in this case undergoes a shock, downstream of which the solution terminates at an irregular sonic point where the proper acceleration diverges, and there is no consistent self-similar continuation to zero radius. As far as the solution can be followed inside the Cauchy horizon, the radial direction is timelike. If the radial direction remains timelike to zero radius (which cannot be confirmed because the selfsimilar solutions terminate), then there is presumably a spacelike singularity at zero radius inside the Cauchy horizon, which is distinctly different from the vacuum (Reissner-Nordström) solution for a charged black hole.

show abstract

Section: Introductionmentioning

confidence: 99%

Inside charged black holes. I. Baryons

Hamilton

Pollack²

2005

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…In this paper we shall always take M = 1 and q = 0.95 for the unperturbed black hole. If Λ = 0 one cannot, in general, provide an analytical solution for (12). Qualitatively, if Λ < 0, the spacetime is asymptotically Anti-de-Sitter and there are no further Killing horizons; if Λ > 0, the spacetime is asymptotically de-Sitter and there may be further Killing horizons of cosmological nature.…”

Section: D Dimensional Reissner-nordström-(a)dsmentioning

confidence: 99%

“…It is well established that the inner horizon of the Reissner-Nordström (RN) black hole is unstable and evolves into a curvature singularity when perturbed [1][2][3][4][5][6][7][8][9][10][11][12][13][14]. The formation of this singularity is a consequence of a large relativistic counter-streaming produced by the perturbation in the vicinity of the inner horizon.…”

Section: Introductionmentioning

confidence: 99%

Mass inflation in aD-dimensional Reissner-Nordström black hole: A hierarchy of particle accelerators?

et al. 2011

View full text Add to dashboard Cite

We study the geometry inside the event horizon of perturbed D dimensional Reissner-Nordström-(A)dS type black holes showing that, similarly to the four dimensional case, mass inflation also occurs for D > 4. First, using the homogeneous approximation, we show that an increase of the number of spatial dimensions contributes to a steeper variation of the metric coefficients with the areal radius and that the phenomenon is insensitive to the cosmological constant in leading order. Then, using the code reported in [1] adapted to D dimensions, we perform fully non-linear numerical simulations. We perturb the black hole with a compact pulse adapting the pulse amplitude such that the relative variation of the black hole mass is the same in all dimensions, and determine how the black hole interior evolves under the perturbation. We qualitatively confirm that the phenomenon is similar to four dimensions as well as the behaviour observed in the homogeneous approximation. We speculate about the formation of black holes inside black holes triggered by mass inflation, and about possible consequences of this scenario.

show abstract

“…We will also consider the same case but with an additional radial magnetic field. It was shown (see [56,57,58]) that, in the considered model, in the close vicinity of a space-like singularity of a BH, all processes, as a rule, have high temporal gradient (much higher than the spatial gradients along the singularity) and that the processes depend on the properties of a very restricted space region. It follows from here that, for clarification of some physical processes, one can use a homogenous approximation and that all processes and geometry depend on the time coordinate only.…”

Section: The Modelmentioning

confidence: 99%

Homogeneous singularity generated by exotic matter, with applications to collapsed black holes and wormholes

Новиков

2010

Phys. Rev. D

View full text Add to dashboard Cite

We analyze analytically and numerically the origin of the singularity in the course of the collapse of a wormhole with the exotic scalar field Ψ with negative energy density, and with this field Ψ together with the ordered magnetic field H. We do this under the simplifying assumptions of the spherical symmetry and that in the vicinity of the singularity the solution of the Einstein equations depends only on one coordinate (the homogeneous approximation). In the framework of these assumptions we found the principal difference between the case of the collapse of the ordinary scalar field Φ with the positive energy density together with an ordered magnetic field H and the collapse of the exotic scalar field Ψ together with the magnetic field H.

show abstract

Physics of the interior of a spherical, charged black hole with a scalar field

Cited by 49 publications

References 30 publications

Inside charged black holes. I. Baryons

Inside charged black holes. I. Baryons

Mass inflation in aD-dimensional Reissner-Nordström black hole: A hierarchy of particle accelerators?

Homogeneous singularity generated by exotic matter, with applications to collapsed black holes and wormholes

Contact Info

Product

Resources

About