Advances in High Energy Physics

Volume 2015 (2015), Article ID 671259, 11 pages

http://dx.doi.org/10.1155/2015/671259

## Particle Dynamics around Weakly Magnetized Reissner-Nordström Black Hole

^{1}Department of Mathematics, School of Natural Sciences (SNS), National University of Sciences and Technology (NUST), H-12, Islamabad 44000, Pakistan^{2}Department of Physics, School of Natural Sciences (SNS), National University of Sciences and Technology (NUST), H-12, Islamabad 44000, Pakistan

Received 7 September 2015; Revised 24 November 2015; Accepted 25 November 2015

Academic Editor: Juan José Sanz-Cillero

Copyright © 2015 Bushra Majeed et al. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The publication of this article was funded by SCOAP^{3}.

#### Abstract

Considering the geometry of Reissner-Nordström (RN) black hole immersed in magnetic field, we have studied the dynamics of neutral and charged particles. A collision of particles in the inner stable circular orbit is considered and the conditions for the escape of colliding particles from the vicinity of black hole are given. The trajectories of the escaping particle are discussed. Also, the velocity required for this escape is calculated. It is observed that there is more than one stable region if magnetic field is present in the accretion disk of black hole, so the stability of ISCO increases in the presence of magnetic field. Effect of magnetic field on the angular motion of neutral and charged particles is observed graphically.

#### 1. Introduction

The geometrical structure of the spacetime around black hole (BH) could be understood better by studying the dynamics of particles in the vicinity of black holes [1, 2]. Circular geodesics give information about geometry of spacetime [3, 4]. The motion of test particles helps to study the gravitational fields of objects experimentally and to compare the observations with the predictions about observable effects (light like deflection, gravitational time delay, and perihelion shift). Presence of plasma is responsible for magnetic field [5], in the surroundings of the black hole [6, 7]. Near the event, horizon effect of magnetic field is strong but not enough to disturb the geometry of the black hole. Motion of a charged particle around black hole in the presence of magnetic field gets influenced [8, 9]. Black holes with such scenario are known as “weakly magnetized” [10]; that is, the magnetic field strength lies within Gauss. Magnetic field is responsible for transferring energy to the particles moving in the geometry around black hole, so that their escape to spatial infinity is possible [11]. Hence, the collision of charged particles near the black hole may produce much higher energy in the presence of magnetic field than in its absence. In [12–15], the effects of magnetic fields on the charged particles around black holes were investigated. Timelike geodesics in modified gravity black hole in the presence of axially symmetric magnetic field are studied in [16]. In [17], authors have studied the dynamics of a charged particle around a weakly magnetized naked singularity, in the Janis-Newman-Winicour (JNW) spacetime. Kaya [18] studied the motion of charged particles around a five-dimensional rotating black hole in a uniform magnetic field and found stable circular orbits around the black hole. In literature, many aspects of the particles motion in the vicinity of RN-black hole have been studied. In [19], authors have studied the high energy collisions phenomenon between the particles, currently termed as BSW mechanism. In [20], the spatial regions for circular motion of neutral and charged test particles around RN-BH and naked singularities have been studied. Critical escape velocity for a charged particle moving around a weakly magnetized Schwarzschild black hole has been studied in [21]. We consider Reissner-Nordström (RN) black hole is surrounded by an axially symmetric magnetic field which is homogeneous at infinity. Particles in the accretion disc move in circular orbits in the equatorial plane. Following the work done by Al Zahrani et al. [21], collision of a neutral and a charged particle with another neutral particle is studied in the vicinity of magnetized RN-BH. We focus on under what circumstances the particle can escape to infinity after collision. To evade the complication in modeling the particle’s motion around a black hole under the influence of both gravitational and magnetic forces, we first consider the motion of a neutral particle in the absence of magnetic field. The study of particle dynamics around RN spacetime is also relevant as this metric represents the extreme RN-BH and a naked singularity as special cases.

Outline of the paper is as follows. In Section 2, metric of RN-BH is discussed and escape velocity of a neutral particle is calculated. In Section 3, the equations of motion of a charged particle moving around weakly magnetized RN-BH are derived. Trajectories of the particles moving around the extremal RN-BH are plotted in Section 4. In Section 5, the dimensionless form of the equations is given. In Section 6, trajectories for escape energy and escape velocity of the particle are presented. Motion of the particle is initially considered in the equatorial plane for the sake of simplicity. The metric signature is and , .

#### 2. Escape Velocity for a Neutral Particle

We first work for the escape velocity of a neutral particle in the absence of magnetic field. The RN-BH metric is given bywhereHere, is the mass and is electric charge of the black hole. Horizon of the RN-BH is located atIf , there are two real positive roots; the larger root corresponds to the event horizon and the smaller root refers to the Cauchy horizon which is associated with the timelike singularity at . Black hole is known to be extremal black hole if and it has only one event horizon at . If , there is no real root of the equation and there is no event horizon. This case is known as naked singularity of RN spacetime. Symmetries of the black hole metric are along the time translation and rotation around symmetry axis. The corresponding constants of motion can be calculated using the Killing vectors: Here, and . The corresponding conserved quantities are the total energy of the moving particle and its azimuthal angular momentum :Over dot is the differentiation with respect to proper time and . From the normalization condition , we have We considered , that is, the planar motion of the particle. Solving , we get the value of corresponding to the extreme values of the effective potential (the convolution point) [22]:The ISCO is at for extreme RN-BH . For , it reduces to (Schwarzschild black hole) [21]. The corresponding energy and the azimuthal angular momentum of the particle (in ISCO) are, respectively,For extremal black hole case, that is, at , (8) becomesNow, consider the collision of a particle, moving in the ISCO, with another particle which is coming from infinity (initially at rest). This collision may result in three possibilities (depending on the progression of the collision): (i) a bounded motion, (ii) particle captured by black hole, and (iii) particle escape to infinity. Orbit of the particle alters slightly if the energy and angular momentum of the particle do not undergo a major change; otherwise, the particle can move away from the original path resulting in captured by black hole or an escape to infinity may occur. Collision of the particles changes the equatorial plane of the moving particle, but since the metric is spherical symmetric, all the equatorial planes are similar. We consider the collision occurring in such a way that (i) the azimuthal angular momentum remains invariant and (ii) initial radial velocity also remains the same. Hence, only the change in energy will be considered for determining the motion of particle after collision. These conditions are imposed for simplification only. Particle gains an escape velocity in orthogonal direction of the equatorial plane after collision [23] and its momentum and energy (in the new equatorial plan) become Here, and denotes the particles’ initial polar angular velocity. Energy of the particle iswith , given in (9). After collision, particle gains greater angular momentum and energy as compared to that before collision. From (11), it is clear that, in the asymptotic limit (), . So for unbounded motion (escape), particle requires . Hence, for escape to infinity, the necessary condition isWe have solved (11) taking and the quantities with subscript denote the extremal black hole case.

#### 3. Charged Particle around RN-BH Surrounded by Magnetic Field

The presence of magnetic field interrupts the motion of a charged particle around black hole. To know the aftermath of this perturbation, let us start with the Lagrangian of the moving particle asHere, is mass of the particle and is the charge of particle. The Killing vector equation resembles the Maxwell equation for in the Lorentz gauge [24, 25]; here, denotes the Killing vector and is the 4-potential defined as [24, 25]with as the magnetic field strength given as and using Levi Civita symbol, , one can write The Maxwell tensor, , is defined as For a local observer in RN geometry, . The only two components of will survive which are and .

Using the Euler-Lagrange equations for the Lagrangian defined in (13), one can get easilyHere, . The normalization condition givesEquation of motion of a charged particle moving in an external electromagnetic field satisfiesUsing (20) for the metric defined in (1), we get the dynamical equations for and given asHere, .

#### 4. Dynamical Equations in Dimensionless Form

For the sake of convenience, we can rewrite the dynamical equations of and in dimensionless form by introducing the following dimensionless quantities [23]:Here, . Using the quantities defined in (22), (18), and (21), take the following forms:For extremal black hole case, it becomesFor the particle moving in equatorial plane, (25) and (26) becomeUsing the built-in command NDSolve in Mathematica , (28) can be solved and the behavior of the obtained interpolating function can be better understood by plotting it against . Using (22) for (19), we obtainand for extreme black hole,The effective potential given in (19) becomesand for extreme black hole it becomesFor the particle moving around RN-BH in the equatorial plane, , at radius , (30)–(32) becomeFor extreme black hole,Again, considering the ideal scenario of collision which does not change the azimuthal angular momentum of the particle except its energy, that is, , defined asfor extremal black hole,where is the energy defined in (33). As already mentioned, when the energy . So for the unbound motion the energy of the particle should be . Solving (36) at , for escape velocity of the particle, we get the following expression:and for extremal RN-BHFor simplicity, we are considering the particle to be initially in ISCO; further, we discuss the behavior of the particle when it escapes to asymptotic infinity. The only parameters required for describing the motion of the particle are the parameters and defined in terms of and the energy of the particle. The expression for the parameters and in terms of could be obtained by dealing with (35). The first and second derivatives of the effective potential defined in (35) areThe values of and can be found by solving simultaneously and , as given in the following: In Section 7, the parameters and are plotted against .

#### 5. Effect of Magnetic Field on Motion of Particles

Consider the neutral particle moving around RN-BH. Writing the equations associated with the constants of motion, in dimensionless form, we have where positive sign is for the particle going away from the black hole and negative sign is for the path of an ingoing particle; alsoUsing (42) and (43) together, we have For extremal black hole, it becomesIt is observed graphically that a particle having less angular momentum approaches the black hole more closely as compared to the one having large angular momentum. This shows that when a particle does not move radially, its chances for approaching the black hole event horizon are very less (Figure 1). For a charged particle moving around RN-BH in the presence of magnetic field, we can writeUsing (46) and (47) together, we haveFor extremal black hole,Change in during the motion of particle, around RN-BH, starting its motion from some finite distance is shown in Figure 2. It is observed that behavior of angular motion of particle is linked with the strength of magnetic field.