scholarly journals Circular orbits in the Taub–NUT and massless Taub–NUT spacetime

2017 ◽  
Vol 14 (07) ◽  
pp. 1750101
Author(s):  
Parthapratim Pradhan
Keyword(s):  
Black Hole ◽  
Circular Orbit ◽  
Center Of Mass ◽  
Null Geodesic ◽  
Spherically Symmetric ◽  
Potential Well ◽  
Killing Horizon ◽  
Stable Circular Orbit ◽  
Innermost Stable Circular Orbit

In this work, we study the equatorial causal geodesics of the Taub–NUT (TN) spacetime in comparison with massless TN spacetime. We emphasized both on the null circular geodesics and time-like circular geodesics. From the effective potential diagram of null and time-like geodesics, we differentiate the geodesics structure between TN spacetime and massless TN spacetime. It has been shown that there is a key role of the NUT parameter to changes the shape of pattern of the potential well in the NUT spacetime in comparison with massless NUT spacetime. We compared the innermost stable circular orbit (ISCO), marginally bound circular orbit (MBCO) and circular photon orbit (CPO) of the said spacetime with graphically in comparison with massless cases. Moreover, we compute the radius of ISCO, MBCO and CPO for extreme TN black hole (BH). Interestingly, we show that these three radii coincides with the Killing horizon, i.e. the null geodesic generators of the horizon. Finally in Appendix A, we compute the center-of-mass (CM) energy for TN BH and massless TN BH. We show that in both cases, the CM energy is finite. For extreme NUT BH, we found that the diverging nature of CM energy. First, we have observed that a non-asymptotic flat, spherically symmetric and stationary extreme BH showing such feature.

scholarly journals Circular geodesics in tidal-charged black hole

2017 ◽  
Vol 15 (01) ◽  
pp. 1850011
Author(s):  
Parthapratim Pradhan
Keyword(s):  
Black Hole ◽  
Circular Orbit ◽  
Center Of Mass ◽  
Normal Modes ◽  
Charged Black Hole ◽  
Particle Accelerators ◽  
Spherically Symmetric ◽  
Stable Circular Orbit ◽  
Existence And Stability ◽  
Limiting Case

We study the existence and stability criteria for circular geodesics of spherically symmetric tidal-charged black hole (BH). We investigate in details the equatorial causal geodesics of the tidal-charged BH in comparison with spherically symmetric Reissner–Nordström BH spacetime. We particularly focused on both the null circular geodesics and time-like circular geodesics. Using the effective potential diagram, we have compared the geodesic structure between two spacetimes. We have derived the ISCO (innermost stable circular orbit), MBCO (marginally bound circular orbit) and CPO (circular photon orbit) for both the spacetimes. Moreover, we have derived the quasi-normal modes[Formula: see text]QNMs[Formula: see text] frequency in the eikonal limit for both the spacetimes via Lyapunov exponent. In the appendix section, we have shown that a spherically symmetric tidal-charged BH can act as particle accelerators with ultra-high center-of-mass (CM) energy in the limiting case of maximal BH tidal-charge[Formula: see text] and it is possible when two neutral particles are colliding near the horizon.

scholarly journals Lyapunov exponent, ISCO and Kolmogorov–Senai entropy for Kerr–Kiselev black hole

2021 ◽  
Vol 81 (1) ◽  
Author(s):  
Monimala Mondal ◽  
Farook Rahaman ◽  
Ksh. Newton Singh
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Lyapunov Exponent ◽  
Circular Orbit ◽  
Real Root ◽  
Angular Frequency ◽  
Geodesic Motion ◽  
Radial Equation ◽  
Stable Circular Orbit ◽  
Innermost Stable Circular Orbit

AbstractGeodesic motion has significant characteristics of space-time. We calculate the principle Lyapunov exponent (LE), which is the inverse of the instability timescale associated with this geodesics and Kolmogorov–Senai (KS) entropy for our rotating Kerr–Kiselev (KK) black hole. We have investigate the existence of stable/unstable equatorial circular orbits via LE and KS entropy for time-like and null circular geodesics. We have shown that both LE and KS entropy can be written in terms of the radial equation of innermost stable circular orbit (ISCO) for time-like circular orbit. Also, we computed the equation marginally bound circular orbit, which gives the radius (smallest real root) of marginally bound circular orbit (MBCO). We found that the null circular geodesics has larger angular frequency than time-like circular geodesics ($$Q_o > Q_{\sigma }$$ Q o > Q σ ). Thus, null-circular geodesics provides the fastest way to circulate KK black holes. Further, it is also to be noted that null circular geodesics has shortest orbital period $$(T_{photon}< T_{ISCO})$$ ( T photon < T ISCO ) among the all possible circular geodesics. Even null circular geodesics traverses fastest than any stable time-like circular geodesics other than the ISCO.

scholarly journals Geodesic motion near self-gravitating scalar field configurations

2019 ◽  
Vol 27 (3) ◽  
pp. 231-241
Author(s):  
Ivan M. Potashov ◽  
Julia V. Tchemarina ◽  
Alexander N. Tsirulev
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Circular Orbit ◽  
Naked Singularity ◽  
Schwarzschild Black Hole ◽  
Null Geodesics ◽  
Naked Singularities ◽  
Test Particles ◽  
Stable Circular Orbit ◽  
Innermost Stable Circular Orbit

We study the geodesics motion of neutral test particles in the static spherically symmetric spacetimes of black holes and naked singularities supported by a selfgravitating real scalar field. The scalar field is supposed to model dark matter surrounding some strongly gravitating object such as the centre of our Galaxy. The behaviour of timelike and null geodesics very close to the centre of such a configuration crucially depends on the type of spacetime. It turns out that a scalar field black hole, analogously to a Schwarzschild black hole, has the innermost stable circular orbit and the (unstable) photon sphere, but their radii are always less than the corresponding ones for the Schwarzschild black hole of the same mass; moreover, these radii can be arbitrarily small. In contrast, a scalar field naked singularity has neither the innermost stable circular orbit nor the photon sphere. Instead, such a configuration has a spherical shell of test particles surrounding its origin and remaining in quasistatic equilibrium all the time. We also show that the characteristic properties of null geodesics near the centres of a scalar field naked singularity and a scalar field black hole of the same mass are qualitatively different.

Effects of electromagnetic field on the motion of particles in dyonic Reissner–Nordström black hole

2017 ◽  
Vol 26 (09) ◽  
pp. 1750091 ◽  
Author(s):  
M. Sharif ◽  
Sehrish Iftikhar
Keyword(s):  
Black Hole ◽  
Electromagnetic Field ◽  
Lyapunov Exponent ◽  
Circular Orbit ◽  
Center Of Mass ◽  
Mass Energy ◽  
Center Of Mass Energy ◽  
Stable Circular Orbit ◽  
The Stability ◽  
Dynamics Of Particles

This paper explores dynamics of particles in the combined gravitational and electromagnetic fields of the dyonic Reissner–Nordström background. We discuss possibilities for the particle escape to infinity at inner most stable circular orbit. We study the stability of orbit through Lyapunov exponent and the effective force on particle. The collision of particles is investigated through the center of mass energy near the horizon of black hole. Finally, we compare our results with the motion of particles around Schwarzschild and Reissner–Nordström black hole. We conclude that charge of the black hole has a strong effect on the motion of particles.

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