Motion of charged particles around a magnetized/electrified black hole

Lim, Yen-Kheng

doi:10.1103/physrevd.91.024048

Cited by 24 publications

(11 citation statements)

References 37 publications

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“…For instance, the motion of charged particles on the equatorial plane of the SMBH spacetime was studied in Refs. [55][56][57][58], while the motion of timelike and null geodesics on the equatorial plane was analyzed in Refs. [59][60][61], and it was noticed that the SMBH spacetime can have no LR at all outside the event horizon.…”

Section: Introductionmentioning

confidence: 99%

Shadows and lensing of black holes immersed in strong magnetic fields

Lima

Cunha²,

Herdeiro³

et al. 2021

Phys. Rev. D

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We investigate the null geodesic flow and in particular the light rings (LRs), fundamental photon orbits (FPOs) and shadows of a black hole (BH) immersed in a strong, uniform magnetic field, described by the Schwarzschilld-Melvin electrovacuum solution. The empty Melvin magnetic Universe contains a tube of planar LRs. Including a BH, for weak magnetic fields, the shadow becomes oblate, whereas the intrinsic horizon geometry becomes prolate. For strong magnetic fields (overcritical solutions), there are no LRs outside the BH horizon, a result explained using topological arguments. This feature, together with the light confining structure of the Melvin universe yields panoramic shadows, seen (almost) all around the equator of the observer's sky. Despite the lack of LRs, there are FPOs, including polar planar ones, which define the shadow edge. We also observe and discuss chaotic lensing, including in the empty Melvin universe, and multiple disconnected shadows.

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Section: Introductionmentioning

confidence: 99%

Shadows and lensing of black holes immersed in strong magnetic fields

Lima

Cunha²,

Herdeiro³

et al. 2021

Phys. Rev. D

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show abstract

“…A review on some early work on this topic may be found in [59]. Later, different types of Black Holes and magnetic field configurations have been considered, for example Schwarzschild Black Holes (SBHs) in dipole [60] or asymptotically uniform magnetic field with [58,61,62] and without [63,64] the consideration of energy losses due to radiation by accelerated charged particles, or including further mechanisms such as the presence of quintessence matter [65,66], as well as Ernst [56] and Kerr [57,67,68] Black Holes.…”

Section: Introductionmentioning

confidence: 99%

Influence of the vacuum polarization effect on the motion of charged particles in the magnetic field around a Schwarzschild black hole

Pavlović¹,

Saveliev

Sossich

2019

Phys. Rev. D

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The consequences of the vacuum polarization effect in magnetic fields around a Schwarzschild Black Hole (SBH) on the motion of charged particles are investigated in this work. Using the weak electromagnetic field approximation, we discuss the non-minimal coupling between magnetic fields and gravity caused by the vacuum polarization and study the equations of motion for the case of a magnetic field configuration which asymptotically approaches a dipole magnetic field. It is shown that the presence of non-minimal coupling can significantly influence the motion of charged particles around Black Holes. In particular, the vacuum polarization effect, leading to strong amplification or suppression of the magnetic field strength around the event horizon (depending on the sign of the coupling parameter), can affect the scattering angle and minimal distance for the electrons moving in the gravitational field of the Black Hole as well as the dependence of these parameters on the asymptotic magnetic field strength, initial distance and the Black Hole mass. It is further demonstrated that the non-minimal coupling between gravity and astrophysical magnetic fields, caused by the vacuum polarization, can cause significant changes of the parameter space corresponding to bound trajectories around the Black Hole. In certain cases, the bounded or unbounded character of a trajectory is determined solely by the presence of non-minimal coupling and its strength. These effects could in principle be used as observational signatures of the vacuum polarization effect and also to constrain the value of the coupling parameter.

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“…𝑀 is the mass of the BH and 𝐵 determines the strength of the external magnetic field. The electromagnetic potential 1-form is given by [58] 𝐴 = 𝐵𝑟 2 sin 2 𝜃 2Λ 𝑑𝜙.…”

Section: The Spacetimementioning

confidence: 99%

Shadows and lensing of black holes immersed in strong magnetic fields

Junior,

Cunha,

Herdeiro

et al. 2021

Preprint

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We investigate the null geodesic flow and in particular the light rings (LRs), fundamental photon orbits (FPOs) and shadows of a black hole (BH) immersed in a strong, uniform magnetic field, described by the Schwarzschilld-Melvin electrovacuum solution. The empty Melvin magnetic Universe contains a tube of planar LRs. Including a BH, for weak magnetic fields, the shadow becomes oblate, whereas the intrinsic horizon geometry becomes prolate. For strong magnetic fields (over-critical solutions), there are no LRs outside the BH horizon, a result explained using topological arguments. This feature, together with the light confining structure of the Melvin Universe yields panoramic shadows, seen (almost) all around the equator of the observer's sky. Despite the lack of LRs, there are FPOs, including polar planar ones, which define the shadow edge. We also observe and discuss chaotic lensing, including in the empty Melvin Universe, and multiple disconnected shadows.

show abstract

Motion of charged particles around a magnetized/electrified black hole

Cited by 24 publications

References 37 publications

Shadows and lensing of black holes immersed in strong magnetic fields

Shadows and lensing of black holes immersed in strong magnetic fields

Influence of the vacuum polarization effect on the motion of charged particles in the magnetic field around a Schwarzschild black hole

Shadows and lensing of black holes immersed in strong magnetic fields

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