Circular orbits and related quasiharmonic oscillatory motion of charged particles around weakly magnetized rotating black holes

Tursunov, Arman; Stuchlík, Zdeněk; Kološ, Martin

doi:10.1103/physrevd.93.084012

Cited by 136 publications

(158 citation statements)

References 57 publications

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“…Let us consider the deviations of the particle from the stable circular orbit at r 0 and θ 0 = π/2 which corresponds to the minimum of the radial function R. The radii of the oscillatory motion are denoted as r = r 0 + δr and θ = θ 0 + δθ. Then, evolution of these deviations is described by the equations [65,66] δr + ω …”

Section: Harmonic Oscillations Of Neutral Test Particlementioning

confidence: 99%

Generic rotating regular black holes in general relativity coupled to nonlinear electrodynamics

2017

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We construct regular rotating black hole and no-horizon spacetimes based on the recently introduced spherically symmetric generic regular black hole spacetimes related to electric or magnetic charge under nonlinear electrodynamics coupled to general relativity that for special values of the spacetime parameters reduce to the Bardeen and Hayward spacetimes. We show that the weak and strong energy conditions are violated inside the Cauchy horizons of these generic rotating black holes. We give the boundary between the rotating black hole and no-horizon spacetimes and determine the black hole horizons and the boundary of the ergosphere. We introduce the separated Carter equations for the geodesic motion in these rotating spacetimes. For the most interesting new class of the regular spacetimes, corresponding for magnetic charges to the Maxwell field in the weak field limit of the nonlinear electrodynamics, we determine the structure of the circular geodesics and discuss their properties. We study the epicyclic motion of a neutral particle moving along the stable circular orbits around the "Maxwellian" rotating regular black holes. We show that epicyclic frequencies measured by the distant observers and related to the oscillatory motion of the neutral test particle along the stable circular orbits around the rotating singular and regular Maxwellian black holes are always smaller than ones in the Kerr spacetime.

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Section: Harmonic Oscillations Of Neutral Test Particlementioning

confidence: 99%

Generic rotating regular black holes in general relativity coupled to nonlinear electrodynamics

2017

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“…Oscillatory motion of charged particles and related circular orbits in magnetized Schwarzschild BH spacetime were studied by Frolov & Shoom () and Kološ et al (); in magnetized Kerr spacetime by Kološ et al (), Shiose et al (), and Tursunov et al (); and in magnetized “Ernst” metric by Lim (), as well as in other papers, e.g., Abdujabbarov & Ahmedov (), Abdujabbarov et al (), Abdujabbarov et al (), Al Zahrani et al (), Aliev & Gal'tsov (), Gal'tsov & Petukhov (), Rahimov et al (), Rayimbaev (2016), Shaymatov et al (), and Tursunov et al (). Resonant phenomena were extensively discussed in Stuchlík et al ().…”

Section: Radiative Widening Of Circular Orbitsmentioning

confidence: 90%

Orbital widening due to radiation reaction around a magnetized black hole

2018

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Radiation reaction acting on a charged particle moving at a stable circular orbit of a magnetized black hole (BH) can lead to the shift of the orbital radius outward from the BH. The effect causes an increase of the energy and angular momentum of the particle measured by an observer at rest at infinity. In this paper, we show that “widening” of such orbits is independent of the field configuration, but it appears only in the cases with the external Lorentz force acting outward from the BH. This condition corresponds to qLB > 0, where q and L are the charge and angular momentum of the particle, and B is intensity of the external magnetic field. As examples of the orbital widening, we consider two scenarios with an external homogeneous magnetic field and a magnetic dipole field generated by a current loop around a Schwarzschild BH. We show that the orbital widening is accompanied by quasi‐harmonic oscillations of the particle, which are considerably large in the magnetic dipole fields. We also estimate the timescales of orbital widening, from which it follows that the effect can be relevant in the vicinity of stellar‐mass BHs.

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“…Other applications will follow [29]. The generalization along with the corrections made to Wald's formulas are crucial for a consistent analysis of (un)charged-particle dynamics around black holes [4][5][6][35][36][37][38], to mention but a few. From this point of view, some particle-dynamics analyses made in the literature have relied on Wald's formulas in cases where they do not apply.…”

Section: Resultsmentioning

confidence: 99%

“…Now if we set f 1 = M in (38), we see that the terms proportional to M in both expressions (38) and (41) (28), this produces the non-negligible extra magnetic force on a charged particle,…”

Section: The Rotating Case: a =mentioning

confidence: 99%

Vacuum and nonvacuum black holes in a uniform magnetic field

Azreg‐Aïnou

2016

Eur. Phys. J. C

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We modify and generalize the known solution for the electromagnetic field when a vacuum, stationary, axisymmetric black hole is immersed in a uniform magnetic field to the case of nonvacuum black holes (of modified gravity) and determine all linear terms of the vector potential in powers of the magnetic field and the rotation parameter. The magnetic field problemA Killing vector ξ μ in vacuum (no stress-energy T μν ≡ 0) is endowed with the property of being parallel, that is, proportional, to some vector potential A μ that solves the sourceless (no currentsMaxwell field equations. So, ξ μ is itself a solution to the same source-less Maxwell field equations. In Ref.[1], this property was employed as an ansatz to determine the electromagnetic field of a vacuum, stationary, axisymmetric, asymptotically flat black hole placed in a uniform magnetic field that is asymptotically parallel to the axis of symmetry. The ansatz stipulates that the vector potential of the solution be in the plane spanned by the timelike Killing vector ξ μ t = (1, 0, 0, 0) and spacelike one ξ μ ϕ = (0, 0, 0, 1) of the stationary, axisymmetric black hole,Since ξ μ t and ξ μ ϕ are pure geometric objects, they do not encode information on the applied magnetic field B; such information is encoded in the coefficients (C t , C ϕ ). Here B is taken as a test field, so the metric of the stationary, axisymmetric black hole too does not encode any information on the applied magnetic field.In this work, a spacetime metric has signature (+, −, −, −) and andrespectively, 1 where B and Q are seen as perturbations, that is, if the metric of the background black hole is that of Kerr, then Qξ t μ /(2M) is, up to an additive constant, the one-form A μ dx μ = −Qr(dt − a sin 2 θ dϕ)/ρ 2 of the Kerr-Newman black hole (with ρ 2 = r 2 + a 2 cos 2 θ ). It is important to emphasize this point: the potential given by (1) and (3) is not an exact solution to the source-less Maxwell equations,if the background metric is that of the charged black hole itself. Rather, it is a solution to (4) if the background metric is that of the corresponding uncharged black hole. For instance, in the Kerr background metric, the potential given by (1) and (3) is a solution to (4), but in the KerrNewman background metric the nonvanishing electric charge density J t and the ϕ current density J ϕ expand in powers of Q aswhich are zero to first order only. Even if rotation is suppressed (a = 0), J t is still nonzero:and its integral charge is also nonzero. Where does this electric charge density come from (the only existing electric 1 The sign "+" in (3) in front of Q is due to our metric-signature choice.123

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Circular orbits and related quasiharmonic oscillatory motion of charged particles around weakly magnetized rotating black holes

Cited by 136 publications

References 57 publications

Generic rotating regular black holes in general relativity coupled to nonlinear electrodynamics

Generic rotating regular black holes in general relativity coupled to nonlinear electrodynamics

Orbital widening due to radiation reaction around a magnetized black hole

Vacuum and nonvacuum black holes in a uniform magnetic field

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