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

Hussain, Saqib; Hussain, Ibrar; Jamil, Mubasher

doi:10.1140/epjc/s10052-014-3210-y

Cited by 82 publications

(67 citation statements)

References 37 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Kerr BHs studies have been constantly seen in the literature (see, for instance, [72][73][74][75]). Since BHs are characterized by strong gravitational fields in quantum length scales, it is expected that their physics will bring about some new insights as regards quantum theories of gravity [76,77].…”

Section: Another Further Work May Rise From An Alternative Form For Fmentioning

confidence: 99%

A complete cosmological scenario from $$f(R,T^{\phi })$$ f ( R , T ϕ )

Moraes¹,

Santos²

2016

Eur. Phys. J. C

View full text Add to dashboard Cite

Recent elaborated by Harko et al., the f (R, T ) theories of gravity allow one to contemplate an optimistic alternative to dark energy, for which R and T stand for the Ricci scalar and the trace of the energy-momentum tensor, respectively. Although the literature has shown that the T dependence on the gravitational part of the action -which is due to the consideration of quantum effects -may induce some novel features in the scope of late-time cosmological dynamics, in the radiation-dominated universe, when T = 0, no contributions seem to arise from such theories. Apparently, f (R, T ) contributions to a radiation-dominated universe may arise only from the f (R, T φ ) approach, which is nothing but the f (R, T ) gravity in the case of a selfinteracting scalar field whose trace of the energy-momentum tensor is T φ . We intend, in this article, to show how f (R, T φ ) theories of gravity can contribute to the study of the primordial stages of the universe. Our results predict a graceful exit from an inflationary stage to a radiation-dominated era. They also predict a late-time cosmic acceleration after a matter-dominated phase, enabling the f (R, T φ ) theories to describe, in a self-consistent way, all the different stages of the dynamics of the universe.

show abstract

Section: Another Further Work May Rise From An Alternative Form For Fmentioning

confidence: 99%

A complete cosmological scenario from $$f(R,T^{\phi })$$ f ( R , T ϕ )

Moraes¹,

Santos²

2016

Eur. Phys. J. C

View full text Add to dashboard Cite

show abstract

“…Figs. (18,20) display the path followed by the particle after being kicked from the ISCO, that ultimately escapes to infinity.…”

Section: Escape Trajectories and Escape Velocitymentioning

confidence: 99%

“…Chaotic particle motion in the Majumdar-Papapertou metric is discussed in [15,16]. Furthermore, collision between particles and their escape energies after collision around Kiselev black hole [17] and a slowly rotating Kerr black hole [18] have been studied.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of a charged particle around a weakly magnetized naked singularity

Babar

Jamil

Lim

2016

Int. J. Mod. Phys. D

Self Cite

View full text Add to dashboard Cite

We examine the motion of a charged particle in the vicinity of a weakly magnetized naked singularity. The escape velocity and energy of the particle moving around the naked singularity after being kicked by another particle or photon are investigated. Also at innermost stable circular orbit (ISCO) escape velocity and energy are examined. Effective potential and angular momentum of the particle are also discussed. We discuss the center of mass energy after collision between two particles having same mass and opposite charges moving along the same circular orbit in the opposite direction. It is investigated that under what conditions maximum energy can be produced as a result of collision.

show abstract

“…However the process itself is important to describe the ejection of particles from the vicinity of black holes. Later on Hussain et al [24] investigated a similar scenario for a slowly rotating Kerr black hole and discussed the conditions of escape for the particle. Jamil et al [25] investigated a similar scenario for a Schwarzschild black hole surrounded by quintessence.…”

Section: Neutral Particle Dynamics Around Mog Black Holementioning

confidence: 99%

“…Firstly, we will calculate the magnetic field in the vicinity of black hole by following the procedure as given by [23,24] The Killing vector equation is [42] …”

Section: B Magnetic Field Calculationmentioning

confidence: 99%

Timelike geodesics of a modified gravity black hole immersed in an axially symmetric magnetic field

Hussain

Jamil

2015

Phys. Rev. D

Self Cite

View full text Add to dashboard Cite

Abstract:We investigate the dynamics of a neutral and a charged particle around a black hole in modified gravity immersed in magnetic field. Our focus is on the scalar-tensor-vector theory as modified gravity. We are interested to explore the conditions on the energy of the particle under which it can escape to infinity after collision with another neutral particle in the vicinity of the black hole. We calculate escape velocity of particle orbiting in the innermost stable circular orbit (ISCO) after the collision. We study the effects of modified gravity on the dynamics of particles. Further we discuss how the presence of magnetic field in the vicinity of black hole, effects the motion of the orbiting particle. We show that the stability of ISCO increases due to presence of magnetic field. It is observed that a particle can go arbitrary close to the black hole due to presence of magnetic field. Furthermore ISCO for black hole is more stable as compared with Schwarzschild black hole. We also discuss the Lyapunov exponent and the effective force acting on the particle in the presence of magnetic field. * Electronic address: s

show abstract

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

Cited by 82 publications

References 37 publications

A complete cosmological scenario from $$f(R,T^{\phi })$$ f ( R , T ϕ )

A complete cosmological scenario from $$f(R,T^{\phi })$$ f ( R , T ϕ )

Dynamics of a charged particle around a weakly magnetized naked singularity

Timelike geodesics of a modified gravity black hole immersed in an axially symmetric magnetic field

Contact Info

Product

Resources

About