Abstract
In the present paper, we have investigated the motion of charged particles together with magnetic dipoles to determine how well the spacetime deviation parameter epsilon and external uniform magnetic field can mimic the spin of a rotating Kerr black hole. Investigation of charged particle motion has shown that the deviation parameter epsilon in the absence of an external magnetic fields can mimic the rotation parameter of the Kerr spacetime up to a/M approx 0.5. The combination of an external magnetic field and deviation parameter can do even a better job mimicking the rotation parameter up to a/Msimeq 0.93, which corresponds to the rapidly rotating case. Study of the dynamics of the magnetic dipoles around quasi-Schwarzschild black holes in the external magnetic field has shown that there are degeneracy values of the ISCO radius of test particles at epsilon _{cr}>epsilon ge 0.35 which may lead to two different values of the innermost stable circular orbit (ISCO) radius. When the deviation parameter is in the range of epsilon in (-1, 1), it can mimic the spin of a rotating Kerr black hole in the range a/M in (0.0537, 0.3952) for magnetic dipoles with values of the magnetic coupling parameter beta in [-0.25, 0.25] in corotating orbits.
Highlights
The first exact analytical solution of the vacuum field equations of Einstein’s general relativity has been obtained just after its discovery in 1916 by Schwarzschild [1] and describes the exterior spacetime of the non-rotating spherically symmetric black hole
In the present paper, we have investigated the motion of charged particles together with magnetic dipoles to determine how well the spacetime deviation parameter and external uniform magnetic field can mimic the spin of a rotating Kerr black hole
In this work the motion of charged particles together with magnetic dipoles has been investigated to determine how well the spacetime deviation parameter and external uniform magnetic field can mimic the rotation parameter of a Kerr black hole, which is the main point of this study
Summary
The first exact analytical solution of the vacuum field equations of Einstein’s general relativity has been obtained just after its discovery in 1916 by Schwarzschild [1] and describes the exterior spacetime of the non-rotating spherically symmetric black hole. We have studied the charged particle motion around a quasi-Kerr compact object in the presence of a magnetic field [42]. The stable circular and chaotic motions of neutral particles [50], the dynamics and quasiharmonic oscillations of charged particles around static and rotating black holes immersed in external asypmtotically uniform magnetic fields [51,52,53,54,55] and plasma magnetosphere surrounding black holes in different gravity models have been analyzed in detail by the authors of Refs. The detailed specifications of these changes and test particle motion around compact object in the presence of a magnetic field have been studied in Refs. 2 is devoted to a study of the dynamics of charged particles around a quasi-Schwarzschild black hole and comparison with one in Kerr spacetime.
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