Motion of the charged test particles in Kerr-Newman-Taub-NUT spacetime and analytical solutions

Cebeci, Hakan; Özdemir, Nülifer; Şentorun, Seçil

doi:10.1103/physrevd.93.104031

Cited by 39 publications

(28 citation statements)

References 38 publications

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“…where we used r + = M + √ M 2 − a 2 + ℓ 2 = M(1 + ǫ) and ℓ 2 = M 2 β 2 = M 2 (α 2 + ǫ 2 − 1). If the frequency of the incoming scalar field satisfies both (11) and (13), i.e. ω sl < ω < ω max , the horizon can be destroyed at the end of the interaction.…”

Section: Can Test Fields Destroy the Event Horizon?mentioning

confidence: 99%

Can test fields destroy the event horizon in the Kerr–Taub–NUT spacetime?

Düztaş¹

2018

Class. Quantum Grav.

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Abstract. In this work we investigate if the interaction of the Kerr-Taub-NUT spacetime with test scalar and neutrino fields can lead to the destruction of the event horizon. It turns out that both extremal and nearly extremal black holes can be destroyed by scalar and neutrino fields if the initial angular momentum of the spacetime is sufficiently large relative to its mass and NUT charge. This is the first example in which a classical field satisfying the null energy condition can actually destroy an extremal black hole. For scalar fields, the modes that can lead to the destruction of the horizon are restricted to a narrow range due to superradiance. Since superradiance does not occur for neutrino fields, the destruction of the horizon by neutrino fields is generic, and it cannot be fixed by backreaction effects. We also show that the extremal black holes that can be destroyed by scalar fields correspond to naked singularities in the Kerr limit, in accord with the previous results which imply that extremal Kerr black holes cannot be destroyed by scalar test fields.

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Section: Can Test Fields Destroy the Event Horizon?mentioning

confidence: 99%

Can test fields destroy the event horizon in the Kerr–Taub–NUT spacetime?

Düztaş¹

2018

Class. Quantum Grav.

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“…which correspond to circular orbits. The equation W (r) = 0 is generically of fourth order [12]. However it can be reduced to a second-order equation if W (r) is even in r, i.e.…”

Section: Circular Orbits: Case Of the Massless Magnetic Brill Spacetimementioning

confidence: 99%

“…The purpose of the present paper is to study the motion of charged particles, with the question of CWLs in mind, in a class of Brill spacetimes more general than that considered in [10]. This motion was recently analyzed in [12] in the case of the electric Kerr-Newman-NUT spacetime, but the question of causality was not investigated there. Here, in order to have a simple tractable form for the effective potential, we restrict to the case of the massless magnetic Reissner-Nordström-NUT spacetime, considering the whole range of black hole, extreme black hole and wormhole solutions.…”

Section: Introductionmentioning

confidence: 99%

Motion of charged particles in a NUTty Einstein–Maxwell spacetime and causality violation

Clément

Guenouche

2018

Gen Relativ Gravit

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We investigate the motion of electrically charged test particles in spacetimes with closed timelike curves, a subset of the black hole or wormhole Reissner-Nordström-NUT spacetimes without periodic identification of time. We show that, while in the wormhole case there are closed worldlines inside a potential well, the wordlines of initially distant charged observers moving under the action of the Lorentz force can never close or self-intersect. This means that for these observers causality is preserved, which is an instance of our weak chronology protection criterion. *

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“…Thus a proper understanding of the geodesic motion in the presence of NUT parameter is essential. Following such implications in mind, there have been attempts to study circular timelike geodesics in presence of NUT parameter [14][15][16] 1 as well as motion of charged particles in this spacetime [17]. Various weak field tests, e.g., perihelion precession, Lense-Thirring effect has also been discussed [18][19][20] (for a taste of these weak field tests in theories beyond general relativity, see [21][22][23][24][25]).…”

Section: Introductionmentioning

confidence: 99%

On some novel features of the Kerr–Newman-NUT spacetime

2019

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In this work we have presented a special class of Kerr-Newman-NUT black hole, having its horizon located precisely at r = 2M , for Q 2 = l 2 − a 2 , where M , l, a and Q are respectively mass, NUT, rotation and electric charge parameters of the black hole. Clearly this choice radically alters the causal structure as there exists no Cauchy horizon indicating spacelike nature of the singularity when it exists. On the other hand, there is no curvature singularity for l 2 > a 2 , however it may have conical singularities. Furthermore there is no upper bound on specific rotation parameter a/M , which could exceed unity without risking destruction of the horizon. To bring out various discerning features of this special member of the Kerr-Newman-NUT family, we study timelike and null geodesics in the equatorial as well as off the equatorial plane, energy extraction through super-radiance and Penrose process, thermodynamical properties and also the quasi-periodic oscillations. It turns out that the black hole under study radiates less energy through the super-radiant modes and Penrose process than the other black holes in this family. * sm13ip029@iiserkol.ac.in

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Motion of the charged test particles in Kerr-Newman-Taub-NUT spacetime and analytical solutions

Cited by 39 publications

References 38 publications

Can test fields destroy the event horizon in the Kerr–Taub–NUT spacetime?

Can test fields destroy the event horizon in the Kerr–Taub–NUT spacetime?

Motion of charged particles in a NUTty Einstein–Maxwell spacetime and causality violation

On some novel features of the Kerr–Newman-NUT spacetime

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