Motion of charged particles around a rotating black hole in a magnetic field

Aliev, Alikram N.; Özdemir, Nülifer

doi:10.1046/j.1365-8711.2002.05727.x

Cited by 143 publications

(125 citation statements)

References 22 publications

(27 reference statements)

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“…8 that with the increase in the strength of the magnetic field, the local minimum of the effective potential is shifting toward the horizon. This local minimum corresponds to ISCO, which is in agreement with the result of [23].…”

Section: Trajectories For Escape Energysupporting

confidence: 91%

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Dynamics of a charged particle around a slowly rotating Kerr black hole immersed in magnetic field

Hussain

Jamil

2014

Eur. Phys. J. C

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The dynamics of a charged particle moving around a slowly rotating Kerr black hole in the presence of an external magnetic field is investigated. We are interested in exploring the conditions under which the charged particle can escape from the gravitational field of the black hole after colliding with another particle. The escape velocity of the charged particle in the innermost stable circular orbit is calculated. The effective potential and escape velocity of the charged particle with angular momentum in the presence of the magnetic field is analyzed. This work serves as an extension of a preceding paper dealing with the Schwarzschild black hole (Zahrani et al., Phys Rev D 87:084043, 2013).

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Section: Trajectories For Escape Energysupporting

confidence: 91%

“…An almost similar problem was studied for weakly charged rotating black holes in [23]. The main conclusion is that, if the magnetic field is present, then the ISCO is located closer to the black hole horizon.…”

Section: Introductionmentioning

confidence: 95%

Dynamics of a charged particle around a slowly rotating Kerr black hole immersed in magnetic field

Hussain

Jamil

2014

Eur. Phys. J. C

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“…12 that as we increase the strength of magnetic field stability is more as compare to the case for which magnetic field is absent b = 0. It can also be seen that the local minima of the effective potential which corresponds to ISCO is shifting toward the horizon which is in agreement with [38,39]. We are comparing the effective potential for massive particle and photon in Fig.…”

Section: Trajectories For Effective Potential and Escape Velocitysupporting

confidence: 84%

Dynamics of particles around a Schwarzschild-like black hole in the presence of quintessence and magnetic field

2015

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We have investigated the dynamics of a neutral and a charged particle around a static and spherically symmetric black hole in the presence of quintessence matter and external magnetic field. We explore the conditions under which the particle moving around the black hole could escape to infinity after colliding with another particle. The innermost stable circular orbit (ISCO) for the particles are studied in detail. Mainly the dependence of ISCO on dark energy and on the presence of external magnetic field in the vicinity of black hole is discussed. By using the Lyapunov exponent, we compare the stabilities of the orbits of the particles in the presence and absence of dark energy and magnetic field. The expressions for the center of mass energies of the colliding particles near the horizon of the black hole are derived. The effective force on the particle due to dark energy and magnetic field in the vicinity of black hole is also discussed.

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“…If the coefficients were taken as functions of the coordinates, it would be possible to determine them upon solving (4). This would allow one to generalize Wald's formulas (2,3) and this is the purpose of this work. These generalizations are useful for a consistent analysis of (un)charged-particle dynamics around black holes.…”

Section: Generalizing the Ansatzmentioning

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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Motion of charged particles around a rotating black hole in a magnetic field

Cited by 143 publications

References 22 publications

Dynamics of a charged particle around a slowly rotating Kerr black hole immersed in magnetic field

Dynamics of a charged particle around a slowly rotating Kerr black hole immersed in magnetic field

Dynamics of particles around a Schwarzschild-like black hole in the presence of quintessence and magnetic field

Vacuum and nonvacuum black holes in a uniform magnetic field

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