Self-force as a cosmic censor

Zimmerman, Peter; Vega, Ian; Poisson, Eric; Haas, Roland

doi:10.1103/physrevd.87.041501

Cited by 95 publications

(96 citation statements)

References 42 publications

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“…They further argued that the same conclusion must then apply to any radially falling charge. In a later work, Zimmerman, Vega and Poisson [7] presented an explicit (numerical) calculation of the charged particle's trajectory including the full effect of the electromagnetic self-force. Analyzing a large sample of orbits within the domain identified by Hubeny, they found no example of successful overcharging: All particles with charge and energy suitable for overcharging the black hole were found to be repelled before reaching the horizon.…”

Section: Introductionmentioning

confidence: 99%

“…However, both above analyses [6,7] have neglected the coupling to gravity (both the back-reaction from the gravitational perturbation sourced by the perturbed electromagnetic stress-energy, and the perturbation in the electromagnetic field due to the particle's mass), which cannot be easily justified for the problem at hand. A complete analysis would require a calculation of both electromagnetic and gravitational self-forces in the coupled problem, which remains a difficult challenge despite recent progress [8][9][10].…”

Section: Introductionmentioning

confidence: 99%

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Self-force as a cosmic censor in the Kerr overspinning problem

et al. 2015

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It is known that a near-extremal Kerr black hole can be spun up beyond its extremal limit by capturing a test particle. Here we show that overspinning is always averted once back-reaction from the particle's own gravity is properly taken into account. We focus on nonspinning, uncharged, massive particles thrown in along the equatorial plane, and work in the first-order self-force approximation (i.e., we include all relevant corrections to the particle's acceleration through linear order in the ratio, assumed small, between the particle's energy and the black hole's mass). Our calculation is a numerical implementation of a recent analysis by two of us [Phys. Rev. D 91, 104024 (2015)], in which a necessary and sufficient "censorship" condition was formulated for the capture scenario, involving certain self-force quantities calculated on the one-parameter family of unstable circular geodesics in the extremal limit. The self-force information accounts both for radiative losses and for the finite-mass correction to the critical value of the impact parameter. Here we obtain the required self-force data, and present strong evidence to suggest that captured particles never drive the black hole beyond its extremal limit. We show, however, that, within our first-order self-force approximation, it is possible to reach the extremal limit with a suitable choice of initial orbital parameters. To rule out such a possibility would require (currently unavailable) information about higher-order self-force corrections.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Self-force as a cosmic censor in the Kerr overspinning problem

et al. 2015

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“…In all these calculations it was assumed that the test particle follows a geodesic motion and effects of the conservative and dissipative backreaction were ignored. There are investigations which suggest that the radiation reaction and self-force would act as a cosmic censor [5][6][7]. It was also shown that it would be possible to destroy a regular black hole with the test particles even when the backreaction effects are taken into account [8].…”

Section: Introductionmentioning

confidence: 99%

Destroying a near-extremal Kerr black hole with a charged particle: Can a test magnetic field serve as a cosmic censor?

et al. 2015

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We investigate effect of a test magnetic field on the process of destroying near-extremal Kerr black hole with a charged test particle. It has been shown that it would be possible to throw a charged test particle into the near extremal rotating black hole and make it go past the extremality i.e. turn Kerr black hole into the Kerr-Newmann naked singularity. Typically in an astrophysical scenario black holes are believed to be surrounded by a magnetic field. Magnetic field although small, affects motion of charged particles drastically due to the large Lorentz force, as the electromagnetic force is much stronger that the gravity. Thus a test magnetic field can affect the process of destroying black holes and restore the cosmic censorship in the astrophysical context. We show that a test magnetic field would act as a cosmic censor beyond a certain threshold value. We try to gauge the magnitude of the magnetic field by comparing its energy density with that of the change in the curvature induced by the test particle. We find that the magnetic field required in only as strong as or slightly stronger as compared to the value for which its effect of the background geometry is comparable to the tiny backreaction as that of the test particle. In such a case however one has to take take into account effect of the magnetic field on the background geometry, which is difficult to implement in the absence of any exact near-extremal rotating magnetized black hole solutions. We argue that magnetic field would still act as a cosmic censor.

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“…We first introduce dimensionless variables r := r/R, χ := M/R, and w := ω R 3 /M . When = 0 we introduce new dimensionless variables e j such that 26) and express the differential equations in the form 0 = E j :=r 27) where summation over the repeated index k is understood. The nonvanishing components of the matrix A k j are given by …”

Section: Modified N = 1 Polytropementioning

confidence: 99%

“…Other applications, however, may well involve the presence of matter. An example of such a situation is the recent effort [26] to take into account self-force effects in attempts to overcharge a near-extremal black hole [27] (this is the charged version of the overspinning scenario described previously). In this situation the black hole is charged, the spacetime is filled with an electrostatic field, and the coupling between gravitational and electromagnetic perturbations creates complications in the formulation of the self-force.…”

Section: Introductionmentioning

confidence: 99%

Self-force and fluid resonances

Isoyama

Mendes

Poisson

2016

Class. Quantum Grav.

Self Cite

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The gravitational self-force acting on a particle orbiting a massive central body has thus far been computed for vacuum spacetimes involving a black hole. In this work we continue an ongoing effort to study the self-force in nonvacuum situations. We replace the black hole by a material body consisting of a perfect fluid, and determine the impact of the fluid's dynamics on the selfforce and resulting orbital evolution. We show that as the particle inspirals toward the fluid body, its gravitational perturbations trigger a number of quasinormal modes of the fluid-gravity system, which produce resonant features in the conservative and dissipative components of the self-force. As a proof-of-principle, we demonstrate this phenomenon in a simplified framework in which gravity is mediated by a scalar potential satisfying a wave equation in Minkowski spacetime.

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Self-force as a cosmic censor

Cited by 95 publications

References 42 publications

Self-force as a cosmic censor in the Kerr overspinning problem

Self-force as a cosmic censor in the Kerr overspinning problem

Destroying a near-extremal Kerr black hole with a charged particle: Can a test magnetic field serve as a cosmic censor?

Self-force and fluid resonances

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