scholarly journals GEODESIC STRUCTURE OF TEST PARTICLE IN BARDEEN SPACETIME

2012 ◽  
Vol 21 (09) ◽  
pp. 1250077 ◽  
Author(s):  
SHENG ZHOU ◽  
JUHUA CHEN ◽  
YONGJIU WANG
Keyword(s):  
Black Hole ◽  
Energy Level ◽  
Test Particle ◽  
Effective Potential ◽  
Null Geodesic ◽  
Low Velocity ◽  
Effective Potentials ◽  
Black Hole Spacetime ◽  
Geodesic Structure ◽  
Bound Orbits

The Bardeen model describes a regular spacetime, i.e. a singularity-free black hole spacetime. In this paper, by analyzing the behavior of the effective potential for the particles and photons, we investigate the timelike and null geodesic structures in the Bardeen spacetime. At the same time, all kinds of orbits, which are allowed according to the energy level corresponding to the effective potentials, are numerically simulated in detail. We find many-world bound orbits, two-world escape orbits and escape orbits in this spacetime. We also find that bound orbits precession directions are opposite and their precession velocities are different, the inner bound orbits shift along counter-clockwise with high velocity while the exterior bound orbits shift along clockwise with low velocity.

Trajectories of photons in modified Hayward black hole spacetime

2019 ◽  
Vol 34 (23) ◽  
pp. 1950182 ◽  
Author(s):  
Jian-Ping Hu ◽  
Yu Zhang ◽  
Li-Li Shi ◽  
Guang-Hai Guo ◽  
Peng-Fei Duan
Keyword(s):  
Black Hole ◽  
Time Delay ◽  
Effective Potential ◽  
Circular Orbit ◽  
Null Geodesic ◽  
Quantum Corrections ◽  
Circular Orbits ◽  
Black Hole Spacetime ◽  
Bound Orbits ◽  
Lapse Function

We study the trajectories of photons in modified Hayward black hole spacetime. Three kinds of horizons are distinguished by analyzing the lapse function of modified Hayward black hole spacetime. Through plotting the effective potential with different values of parameters, it is found that the parameter [Formula: see text] has more conspicuous effects than parameters [Formula: see text] ([Formula: see text] is associated with the time-delay) and [Formula: see text] ([Formula: see text] is related to the 1-loop quantum corrections) for the effective potential. The change of the parameters ([Formula: see text], [Formula: see text] and [Formula: see text]) has an obvious influence on unstable circular orbits. The structure of null geodesic is simpler than that of time-like geodesic. The stable circular orbits and the bound orbits are not included for the photon trajectories. By analyzing the corresponding effective potential, all possible orbits of null geodesic are found. The radius of unstable circular orbit equals 2.8790 for fixed [Formula: see text], [Formula: see text], [Formula: see text], [Formula: see text] and [Formula: see text].

Bekenstein–Hawking entropy by energy quantization from Reissner–Nordström black hole

2016 ◽  
Vol 25 (03) ◽  
pp. 1650034 ◽  
Author(s):  
M. Jakir Hossain ◽  
M. Atiqur Rahman ◽  
M. Ilias Hossain
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Test Particle ◽  
Effective Potential ◽  
Circular Orbits ◽  
Energy Quantization ◽  
Quantum Numbers ◽  
Black Hole Spacetime ◽  
Complete Set ◽  
Large Quantum

We consider the motion of a test particle orbiting around Reissner–Nordström (RN) black hole spacetime. The complete set of equations for radial motion and effective potential is derived. We also derive the radius of the different stable circular orbits of this particle corresponding to different label indexes like the Bohr atomic model. We also quantized the energy of this particle from the quantization of angular momentum and calculated the Bekenstein–Hawking entropy of RN black hole. We also investigate the change of entropy between two nearby states approaches to zero for large quantum numbers.

Geodesic structure of the Clifton–Barrow black hole space–time

2019 ◽  
Vol 34 (22) ◽  
pp. 1950123
Author(s):  
Li-Li Shi ◽  
Jian-Ping Hu ◽  
Yu Zhang ◽  
Chen Ma ◽  
Peng-Fei Duan
Keyword(s):  
Black Hole ◽  
Circular Orbit ◽  
Orbital Motion ◽  
Null Geodesic ◽  
Space Time ◽  
Circular Orbits ◽  
Test Particles ◽  
Stable Circular Orbit ◽  
Geodesic Structure ◽  
Bound Orbits

In this paper, we investigate the geodesic structure of Clifton–Barrow black hole space–time. Through the numerical analysis of the effective potential and the motion equation, the orbital types of test particles and photons and the corresponding orbital motion diagrams of each orbital types under certain conditions are obtained. We find that angular momentum [Formula: see text] and [Formula: see text] determine the existence of bound orbits and circular orbits. And we also find that the radius of unstable circular orbit decreases with increases in [Formula: see text] while the radius of stable circular orbit increases. Furthermore, as [Formula: see text] increases, the radius of unstable circular orbit increases, while the radius of stable circular orbit decreases. For null geodesic, parameters [Formula: see text] and [Formula: see text] do not affect the types of null orbits. The radius of the unstable circular orbits increases with the increase of [Formula: see text]. However, the radius of the unstable circular orbits remains unchanged as [Formula: see text] increases. Also, we show that the precession direction of the bound orbits of the test particles is counterclockwise for [Formula: see text], but clockwise with [Formula: see text]. Moreover, different energy values have an effect on the curvature of escape and absorb orbits curve.

scholarly journals GEODESIC STRUCTURE OF THE SCHWARZSCHILD BLACK HOLE IN RAINBOW GRAVITY

2009 ◽  
Vol 24 (18) ◽  
pp. 1443-1451 ◽  
Author(s):  
CARLOS LEIVA ◽  
JOEL SAAVEDRA ◽  
JOSÉ VILLANUEVA
Keyword(s):  
Black Hole ◽  
Test Particle ◽  
Radial Motion ◽  
Schwarzschild Black Hole ◽  
Geodesic Structure

In this paper we study the geodesic structure of the Schwarzschild black hole in rainbow gravity analyzing the behavior of null and time-like geodesic. We find that the structure of the geodesics essentially does not change when the semiclassical effects are included. However, we can distinguish different scenarios if we take into account the effects of rainbow gravity. Depending on the type of rainbow functions under consideration, inertial and external observers see very different situations in radial and non-radial motion of a test particle.

scholarly journals Trajectory around a spherically symmetric non-rotating black hole

2011 ◽  
Vol 89 (6) ◽  
pp. 689-695 ◽  
Author(s):  
Sumanta Chakraborty ◽  
Subenoy Chakraborty
Keyword(s):  
Black Hole ◽  
Gravitational Field ◽  
Gravitational Potential ◽  
Test Particle ◽  
Effective Potential ◽  
Particle Motion ◽  
Spherically Symmetric ◽  
Rotating Black Hole

The trajectory of a test particle or a photon around a general spherical black hole is studied, and bending of the light trajectory is investigated. A pseudo-Newtonian gravitational potential describing the gravitational field of the black hole is determined and is compared with the related effective potential for test particle motion. As an example, results are presented for a Reissner–Nordström black hole.

Geodesic structure of magnetically charged regular black hole

2017 ◽  
Vol 14 (09) ◽  
pp. 1750120 ◽  
Author(s):  
Muhammad Azam ◽  
Ghulam Abbas ◽  
Syeda Sumera ◽  
Abdul Rauf Nizami
Keyword(s):  
Black Hole ◽  
Effective Potential ◽  
Proper Time ◽  
Massive Particle ◽  
Circular Motion ◽  
Geodesic Path ◽  
Timelike Geodesic ◽  
Null Geodesics ◽  
Regular Black Hole ◽  
Geodesic Structure

The purpose of this paper is to study the geodesic structure of magnetically charged regular black hole (MCRBH). The behavior of timelike and null geodesics of MCRBH is investigated. The graphs have been plotted to show the relation between distance versus time and proper time for photon-like and massive particle. For radial and circular motion, the effective potential has been plotted with different parameters of BH. We conclude that massive particles move around the BH in timelike geodesic path.

scholarly journals Timelike geodesics around a charged spherically symmetric dilaton black hole

2015 ◽  
pp. 41-48 ◽  
Author(s):  
C. Blaga
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Test Particle ◽  
Effective Potential ◽  
Equations Of Motion ◽  
Equation Of Motion ◽  
Qualitative Approach ◽  
Extremal Black Hole ◽  
Spherically Symmetric ◽  
Dilaton Black Hole

In this paper we study the timelike geodesics around a spherically symmetric charged dilaton black hole. The trajectories around the black hole are classified using the effective potential of a free test particle. This qualitative approach enables us to determine the type of orbit described by test particle without solving the equations of motion, if the parameters of the black hole and the particle are known. The connections between these parameters and the type of orbit described by the particle are obtained. To visualize the orbits we solve numerically the equation of motion for different values of parameters envolved in our analysis. The effective potential of a free test particle looks different for a non-extremal and an extremal black hole, therefore we have examined separately these two types of black holes.

scholarly journals Null geodesics and repulsive behavior of gravity in $(2+1)$D massive gravity

2019 ◽  
Vol 2019 (7) ◽  
Author(s):  
Keisuke Nakashi ◽  
Shinpei Kobayashi ◽  
Shu Ueda ◽  
Hiromi Saida
Keyword(s):  
Black Hole ◽  
Deflection Angle ◽  
Null Geodesic ◽  
Analytic Solutions ◽  
Massive Gravity ◽  
Geodesic Equation ◽  
Null Geodesics ◽  
Black Hole Background ◽  
Black Hole Spacetime ◽  
The Impact

Abstract We study the null geodesics in a static circularly symmetric (SCS) black hole spacetime, which is a solution in the $(2+1)$D massive gravity proposed by Bergshoeff, Hohm, and Townsend (BHT massive gravity). We obtain analytic solutions for the null geodesic equation in the SCS black hole background and find the explicit form of deflection angles. We see that, for various values of the impact parameter, the deflection angle can be positive, negative, or even zero in this black hole spacetime. The negative deflection angle indicates the repulsive behavior of the gravity that comes from the gravitational hair parameter that is the most characteristic quantity of the BHT massive gravity.

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