Dynamics of Magnetized and Magnetically Charged Particles around Regular Nonminimal Magnetic Black Holes

Galaxies ◽  
2021 ◽  
Vol 9 (4) ◽  
pp. 71
Author(s):  
Javlon Rayimbaev ◽  
Bakhtiyor Narzilloev ◽  
Ahmadjon Abdujabbarov ◽  
Bobomurat Ahmedov
Keyword(s):  
Black Hole ◽  
Magnetic Charge ◽  
Coupling Parameter ◽  
Charged Particles ◽  
Kerr Black Hole ◽  
Harmonic Oscillations ◽  
Yang Mills ◽  
Keplerian Orbits ◽  
Maximum Value ◽  
Mills Field

The present paper is devoted to the study of the event horizon properties of spacetime around a regular nonminimal magnetic black hole (BH), together with dynamics of magnetized and magnetically charged particles in the vicinity of the BH. It is shown that the minimum value of the outer horizon of the extreme charged BH increases with the increase in coupling parameter. It reaches its maximum value of 1.5M when q→∞, while the maximal value of the BH charge decreases and tends toward zero. We also present a detailed analysis of magnetized particles’ motion around a regular nonminimal magnetic black hole. The particle’s innermost circular stable orbits (ISCOs) radius decreases as the magnetic charge and the parameter β increase and the coupling parameter of Yang–Mills field causes a decrease at the values of the magnetic charge near to its maximum. We show that the magnetic charge can mimic the spin of a rotating Kerr black hole up to the value of a=0.7893M, providing the same value for an ISCO of a magnetized particle with the parameter β=10.2 when the coupling parameter is q=0. Moreover, Lyapunov exponents, Keplerian orbits and harmonic oscillations of magnetized particles motion are also discussed.

scholarly journals Dynamics of charged particles and magnetic dipoles around magnetized quasi-Schwarzschild black holes

2021 ◽  
Vol 81 (3) ◽  
Author(s):  
Bakhtiyor Narzilloev ◽  
Javlon Rayimbaev ◽  
Ahmadjon Abdujabbarov ◽  
Bobomurat Ahmedov ◽  
Cosimo Bambi
Keyword(s):  
Magnetic Field ◽  
Black Holes ◽  
Black Hole ◽  
External Magnetic Field ◽  
Coupling Parameter ◽  
Charged Particles ◽  
Kerr Black Hole ◽  
Rotation Parameter ◽  
Magnetic Dipoles ◽  
Deviation Parameter

AbstractIn the present paper, we have investigated the motion of charged particles together with magnetic dipoles to determine how well the spacetime deviation parameter $$\epsilon $$ ϵ 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 $$\epsilon $$ ϵ in the absence of an external magnetic fields can mimic the rotation parameter of the Kerr spacetime up to $$a/M \approx 0.5$$ a / M ≈ 0.5 . The combination of an external magnetic field and deviation parameter can do even a better job mimicking the rotation parameter up to $$a/M\simeq 0.93$$ a / M ≃ 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 $$\epsilon _{cr}>\epsilon \ge 0.35$$ ϵ cr > ϵ ≥ 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 $$\epsilon \in (-1,\ 1)$$ ϵ ∈ ( - 1 , 1 ) , it can mimic the spin of a rotating Kerr black hole in the range $$a/M \in (0.0537, \ 0.3952)$$ a / M ∈ ( 0.0537 , 0.3952 ) for magnetic dipoles with values of the magnetic coupling parameter $$\beta \in [-0.25,\ 0.25]$$ β ∈ [ - 0.25 , 0.25 ] in corotating orbits.

4D AdS Einstein–Gauss–Bonnet black hole with Yang–Mills field and its thermodynamics

2021 ◽  
Vol 434 ◽  
pp. 168642
Author(s):  
Dharm Veer Singh ◽  
Benoy Kumar Singh ◽  
Sudhaker Upadhyay
Keyword(s):  
Black Hole ◽  
Yang Mills ◽  
Mills Field

scholarly journals TOPOLOGICAL BLACK HOLES OF GAUSS–BONNET–YANG–MILLS GRAVITY

2010 ◽  
Vol 19 (07) ◽  
pp. 1107-1117 ◽  
Author(s):  
M. H. DEHGHANI ◽  
N. BOSTANI ◽  
R. POURHASAN
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Causal Structure ◽  
Naked Singularity ◽  
Higher Dimensions ◽  
Negative Mass ◽  
Five Dimensions ◽  
Yang Mills ◽  
Extreme Black Hole ◽  
Mills Field

We present the asymptotically AdS solutions of Gauss–Bonnet gravity with hyperbolic horizon in the presence of a non-Abelian Yang–Mills field with the gauge semisimple group So(n(n-1)/2-1, 1). We investigate the properties of these solutions and find that the non-negative mass solutions in six and higher dimensions are real everywhere with spacelike singularities. They present black holes with one horizon and have the same causal structure as the Schwarzschild space–time. The solutions in five dimensions or the solutions in higher dimensions with negative mass are not real everywhere. In these cases, one needs a transformation to make the solutions real. These solutions may present a naked singularity, an extreme black hole, a black hole with two horizons, or a black hole with one horizon.

scholarly journals The Carter constant for inclined orbits about a massive Kerr black hole: near-circular, near-polar orbits

Open Physics ◽  
2012 ◽  
Vol 10 (4) ◽  
Author(s):  
Peter Komorowski ◽  
Sree Valluri ◽  
Martin Houde
Keyword(s):  
Black Hole ◽  
Evolution Equations ◽  
Kerr Black Hole ◽  
Reaction Model ◽  
Back Reaction ◽  
Kerr Spacetime ◽  
System A ◽  
Binary Black Hole ◽  
Maximum Value ◽  
Published Result

AbstractIn an extreme mass-ratio binary black hole system, a non-equatorial orbit will list (i.e. increase its angle of inclination, i) as it evolves in Kerr spacetime. The abutment, a set of evolving, near-polar, retrograde orbits, for which the instantaneous Carter constant (Q) is at its maximum value (Q X) for given values of latus rectum (l̃) and eccentricity (e), has been introduced as a laboratory in which the consistency of dQ/dt with corresponding evolution equations for d l̃/dt and de/dt might be tested independently of a specific radiation back-reaction model. To demonstrate the use of the abutment as such a laboratory, a derivation of dQ/dt, based only on published formulae for d l̃/dt and de/dt, was performed for elliptical orbits on the abutment. The resulting expression for dQ/dt matched the published result to the second order in e. We believe the abutment is a potentially useful tool for improving the accuracy of evolution equations to higher orders of e and l̃−.

scholarly journals Applying explicit symplectic integrator to study chaos of charged particles around magnetized Kerr black hole

2021 ◽  
Vol 81 (9) ◽  
Author(s):  
Wei Sun ◽  
Ying Wang ◽  
Fuyao Liu ◽  
Xin Wu
Keyword(s):  
Black Hole ◽  
Charged Particles ◽  
Kerr Black Hole ◽  
Space Structure ◽  
Point Of View ◽  
Symplectic Integrator ◽  
Spacetime Geometry ◽  
Kerr Spacetime ◽  
Phase Space Structure ◽  
Local Point

AbstractIn a recent work of Wu, Wang, Sun and Liu, a second-order explicit symplectic integrator was proposed for the integrable Kerr spacetime geometry. It is still suited for simulating the nonintegrable dynamics of charged particles moving around the Kerr black hole embedded in an external magnetic field. Its successful construction is due to the contribution of a time transformation. The algorithm exhibits a good long-term numerical performance in stable Hamiltonian errors and computational efficiency. As its application, the dynamics of order and chaos of charged particles is surveyed. In some circumstances, an increase of the dragging effects of the spacetime seems to weaken the extent of chaos from the global phase-space structure on Poincaré sections. However, an increase of the magnetic parameter strengthens the chaotic properties. On the other hand, fast Lyapunov indicators show that there is no universal rule for the dependence of the transition between different dynamical regimes on the black hole spin. The dragging effects of the spacetime do not always weaken the extent of chaos from a local point of view.

Shadow cast and quasinormal modes in f(R) gravity model inspired by Yang–Mills field

2021 ◽  
pp. 2150143
Author(s):  
Younes Younesizadeh ◽  
Jennifer Liang
Keyword(s):  
Magnetic Charge ◽  
Null Geodesic ◽  
Quasinormal Modes ◽  
Third Order ◽  
Yang Mills ◽  
Shadow Cast ◽  
Schrödinger Form ◽  
Mills Field ◽  
Hamilton Jacobi Equation ◽  
Charge Formula

In this paper, the null geodesic equations are computed in [Formula: see text] space–time dimensions [Y. Younesizadeh, A. A. Ahmad, A. H. Ahmed, F. Younesizadeh, Ann. Phys. 420, 168246 (2020)] by using the concept of symmetries and Hamilton–Jacobi equation and Carter separable method. With these null geodesics in hand, we evaluate the celestial coordinates (x, y) and the radius [Formula: see text] of the BH shadow and represent it graphically. In addition, we have shown that the peak of this energy slowly shifts to lower frequencies and its height decreases with the increase in the YM magnetic charge ([Formula: see text]) values and decrease in the [Formula: see text] parameter ([Formula: see text]) values. In addition, we have analyzed the concept of effective potential barrier by transforming the radial equation of motion into standard Schrodinger form. The most important result derived from this study is that the height of this potential increases with increase in the YM magnetic charge ([Formula: see text]) values. Then, we study the quasinormal modes (QNMs) of these 4D black holes. For this purpose, we use the WKB approximation method upto third-order corrections. We have shown the perturbation’s decay in corresponding diagrams when the YM magnetic charge ([Formula: see text]) values and the [Formula: see text] parameter ([Formula: see text]) values change.

scholarly journals On the limiting energy of the collision of elementary particles close to horizon of the rotating black hole

2020 ◽  
Vol 35 (31) ◽  
pp. 2050262
Author(s):  
A. A. Grib ◽  
Yu. V. Pavlov
Keyword(s):  
Black Hole ◽  
Electromagnetic Radiation ◽  
Gravitational Radiation ◽  
Charged Particles ◽  
Kerr Black Hole ◽  
Elementary Particles ◽  
Rotating Black Hole ◽  
Energy Growth

Arguments are given for the conclusion that the energy of collision of two ultrarelativistic elementary particles due to gravitational radiation cannot exceed the Planck value. Comparison of the gravitational and electromagnetic radiation for charged particles close to the horizon of Kerr black hole is made. If for trans-Planckian energy the black hole can arise it is shown that the energy growth used in scattering for interaction of particles is still limited.

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