Oscillatory Null Singularity inside Realistic Spinning Black Holes

Ori, Amos

doi:10.1103/physrevlett.83.5423

Cited by 62 publications

(111 citation statements)

References 30 publications

(44 reference statements)

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“…It seems possible that the oscillatory character of the solutions with conductivities between κ 1 and κ ∞ might perhaps be related in some way to the oscillatory character of the curvature near the inner horizon of a rotating black hole reported by [63]. Figure 9 illustrates a model with conductivity κ = 0.8 below the first critical threshold κ 1 .…”

Section: Incompleteness Of Solutions Inside the Cauchy Horizonsmentioning

confidence: 99%

“…The 4-velocity of an object instantaneously at rest in the tetrad frame is u t = 1 and u r = 0, and in this case equation (63) simplifies to υ lnt = −r/η. Thus the tetrad frame is ingoing or outgoing according to the sign of η ≡ αr/t.…”

Section: Ingoing Vs Outgoingmentioning

confidence: 99%

“…In the similarity solutions, geodesics between the outer and inner horizons can be classified as ingoing or outgoing according to the sign of minus the homothetic momentum −υ lnt , equation (63). This definition of ingoing versus outgoing is gauge-invariant, independent of the choice of either coordinates or tetrad frame.…”

Section: Ingoing Vs Outgoingmentioning

confidence: 99%

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Inside charged black holes. I. Baryons

Hamilton

Pollack²

2005

Phys. Rev. D

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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.

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Section: Incompleteness Of Solutions Inside the Cauchy Horizonsmentioning

confidence: 99%

Section: Ingoing Vs Outgoingmentioning

confidence: 99%

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Inside charged black holes. I. Baryons

Hamilton

Pollack²

2005

Phys. Rev. D

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“…A spacelike singularity to the future of the Cauchy horizon singularity was found in spherically-symmetric, charged models. It has been argued that no corresponding spacelike singularity is likely to occur inside a rotating black hole [13]. Others have argued, that a spacelike singularity, possibly of the Belinskii-Khalatnikov-Lifshitz type, is a possible outcome.…”

mentioning

confidence: 99%

Survival of the black hole’s Cauchy horizon under noncompact perturbations

Burko

2002

Phys. Rev. D

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We study numerically the evolution of spactime, and in particular of a spacetime singularity, inside a black hole under a class of perturbations of non-compact support. We use a very simplified toy model of a spherical charged black hole which is perturbed nonlinearly by a self-gravitating, spherical scalar field. The latter grows logarithmically with advanced time along an outgoing characteristic hypersurface. We find that for that class of perturbations a portion of the Cauchy horizon survives as a non-central, null singularity.

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“…For systematic discussion of the problems of the internal structure of black holes see [1][2][3][4]. Discussion of the problems of astrophysics of black holes see in [5][6][7][8][9][10].…”

Section: Introductionmentioning

confidence: 99%

The Interior of Black Holes and their Astrophysics

Artemova¹,

Новиков

2003

The Early Universe and the Cosmic Microwave Background: Theory and Observations

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Abstract.Gravity warps space and time into a funnel and generates a black hole when a cosmic body undergoes a catastrophic collapse. What can one say about the interior of a black hole? The important point is that inside a black hole the space radial direction becomes time, and time becomes a space direction. The path into the gravitational abyss of the interior of a black hole is a progression in time. There is a peculiar region inside a black hole where some characteristics of the space-time curvature become singular. We call this region singularity. The colossal tidal gravitational forces near singularity modify physical laws. Space and time are not only strongly curved near the singularity, but they split into quanta. The fall into the singularity is unstoppable for a body inside a black hole. This paper also addresses the following questions:Can one see what happens inside a black hole? Can a falling observer cross the singularity without being crushed? Can new baby universes arise inside a black hole? An answer to all these questions is probably "yes". We give also a brief review of the modern black hole astrophysics.

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Oscillatory Null Singularity inside Realistic Spinning Black Holes

Cited by 62 publications

References 30 publications

Inside charged black holes. I. Baryons

Inside charged black holes. I. Baryons

Survival of the black hole’s Cauchy horizon under noncompact perturbations

The Interior of Black Holes and their Astrophysics

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