Effects of the external magnetic field on the Lense–Thirring precession

2021 ◽  
Author(s):  
Muhammad Rizwan ◽  
Tooba Feroze
Keyword(s):  
Magnetic Field ◽  
Black Hole ◽  
External Magnetic Field ◽  
Equatorial Plane ◽  
Polar Axis ◽  
Precession Frequency ◽  
Black Hole Spacetime ◽  
Newman Black Hole

In this paper, we study the effects of the external magnetic field on the Lense–Thirring (LT) precession of a test gyroscope attached to an observer in magnetized black hole spacetime. For this, we consider a Kerr–Newman black hole embedded in the external magnetic field. The LT precession of a test gyroscope diverges near the ergosurface and remains finite everywhere outside the ergosurface. It is seen that by increasing the external magnetic field, the LT precession frequency in the region of large [Formula: see text] decreases as [Formula: see text] increases, while the precession frequency in the region of small [Formula: see text] increases as [Formula: see text] increases, whereas it increases with increasing the charge of the black hole. The LT precession of a test gyroscope attached to observers moving along the directions close to the polar axis is greater than that of the observer moving in the equatorial plane.

MOTION OF CHARGED PARTICLES AROUND A FIVE-DIMENSIONAL ROTATING MAGNETIZED BLACK HOLE

2007 ◽  
Vol 16 (08) ◽  
pp. 1369-1379
Author(s):  
R. KAYA
Keyword(s):  
Magnetic Field ◽  
Black Hole ◽  
External Magnetic Field ◽  
Effective Potential ◽  
Equatorial Plane ◽  
Charged Particles ◽  
Circular Motion ◽  
Test Particles ◽  
Jacobi Formalism ◽  
The Stability

We study the effect of an external magnetic field on the stability of circular motion of charged particles in the equatorial plane of a five-dimensional rotating black hole. Using the Hamilton–Jacobi formalism, we derive the effective potential for the radial motion of test particles around a five-dimensional magnetized Myers–Perry black hole. We show that there exist stable circular orbits in equatorial planes in the background of this metric.

scholarly journals Tidal disruption event discs around supermassive black holes: disc warp and inclination evolution

2019 ◽  
Vol 487 (4) ◽  
pp. 4965-4984 ◽  
Author(s):  
J J Zanazzi ◽  
Dong Lai
Keyword(s):  
Black Hole ◽  
Equatorial Plane ◽  
Accretion Rate ◽  
Accretion Disc ◽  
Precession Frequency ◽  
Tidal Disruption ◽  
Eigenmode Analysis ◽  
Accretion Rates ◽  
Rigid Disc ◽  
Disruption Event

ABSTRACT After the tidal disruption event (TDE) of a star around a supermassive black hole (SMBH), the bound stellar debris rapidly forms an accretion disc. If the accretion disc is not aligned with the spinning SMBH’s equatorial plane, the disc will be driven into Lense–Thirring precession around the SMBH’s spin axis, possibly affecting the TDE’s light curve. We carry out an eigenmode analysis of such a disc to understand how the disc’s warp structure, precession, and inclination evolution are influenced by the disc’s and SMBH’s properties. We find an oscillatory warp may develop as a result of strong non-Keplarian motion near the SMBH. The global disc precession frequency matches the Lense–Thirring precession frequency of a rigid disc around a spinning black hole within a factor of a few when the disc’s accretion rate is high, but deviates significantly at low accretion rates. Viscosity aligns the disc with the SMBH’s equatorial plane over time-scales of days to years, depending on the disc’s accretion rate, viscosity, and SMBH’s mass. We also examine the effect of fallback material on the warp evolution of TDE discs, and find that the fallback torque aligns the TDE disc with the SMBH’s equatorial plane in a few to tens of days for the parameter space investigated. Our results place constraints on models of TDE emission which rely on the changing disc orientation with respect to the line of sight to explain observations.

Modified fermion tunneling radiation of Demianski–Newman black hole at higher energy scales

2019 ◽  
Vol 35 (10) ◽  
pp. 2050061
Author(s):  
Z. Luo ◽  
X. G. Lan
Keyword(s):  
Black Hole ◽  
Dispersion Relation ◽  
Jacobi Equation ◽  
Black Hole Entropy ◽  
Hawking Temperature ◽  
Tunneling Radiation ◽  
Black Hole Spacetime ◽  
Newman Black Hole ◽  
Hamilton Jacobi Equation

It is suggested that the dispersion relation might be corrected at higher energy scales and lead to the deformed Hamilton–Jacobi equation. In this paper, we use the correction to investigate the fermion tunneling radiation for Demianski–Newman black hole spacetime, and the result shows that the corresponding Hawking temperature and the black hole entropy are related to the angular parameters of the black hole coordinates.

Trajectories of material particles in Kerr–Newman–de Sitter space–time

1989 ◽  
Vol 67 (5) ◽  
pp. 501-504
Author(s):  
K. D. Krori ◽  
Ranjana Choudhury ◽  
J. C. Sarmah
Keyword(s):  
Black Hole ◽  
Equatorial Plane ◽  
De Sitter Space ◽  
Space Time ◽  
De Sitter ◽  
Newman Black Hole

In this paper we show that in the Kerr–Newman–de Sitter space–time material particles may move in stable orbits in the equatorial plane (θ = π/2) of the Kerr–Newman black hole.

scholarly journals Charged particle and epicyclic motions around 4D Einstein–Gauss–Bonnet black hole immersed in an external magnetic field

2020 ◽  
Vol 30 ◽  
pp. 100648 ◽  
Author(s):  
Sanjar Shaymatov ◽  
Jaroslav Vrba ◽  
Daniele Malafarina ◽  
Bobomurat Ahmedov ◽  
Zdeněk Stuchlík
Keyword(s):  
Magnetic Field ◽  
Black Hole ◽  
Charged Particle ◽  
External Magnetic Field

ON ERNST BLACK HOLES WITH A DILATON POTENTIAL

2005 ◽  
Vol 20 (14) ◽  
pp. 1077-1085 ◽  
Author(s):  
MARICEL AGOP ◽  
EUGEN RADU ◽  
REINOUD SLAGTER
Keyword(s):  
Magnetic Field ◽  
Black Holes ◽  
Black Hole ◽  
External Magnetic Field ◽  
Thermodynamic Properties ◽  
Action Principle ◽  
Schwarzschild Black Hole ◽  
Liouville Type ◽  
Background Magnetic Field ◽  
Type Potential

The dilatonic Ernst solution describing a Schwarzschild black hole immersed in a background magnetic field is generalized by including a Liouville-type potential in the action principle. We prove that the thermodynamic properties of this new black hole dilaton solution are unaffected by an external magnetic field passing through it.

scholarly journals Dirac Monopoles in the Ernst–Schwarzschild Spacetime

2003 ◽  
Vol 18 (12) ◽  
pp. 2153-2157 ◽  
Author(s):  
A. A. Bytsenko ◽  
Yu. P. Goncharov
Keyword(s):  
Magnetic Field ◽  
Black Hole ◽  
External Magnetic Field ◽  
Explicit Form ◽  
Hawking Radiation ◽  
Maxwell Equations ◽  
Schwarzschild Spacetime ◽  
Dirac Monopole ◽  
Schwarzschild Metric ◽  
The Given

It is discussed that the Ernst–Schwarzschild metric describing a nonrotating black hole in the external magnetic field admits the solutions of the Dirac monopole types for the corresponding Maxwell equations. The given solutions are obtained in explicit form and a possible influence of the conforming Dirac monopoles on Hawking radiation is also outlined.

scholarly journals A NOTE ON SCHWARZSCHILD BLACK HOLE THERMODYNAMICS IN A MAGNETIC UNIVERSE

2002 ◽  
Vol 17 (34) ◽  
pp. 2277-2281 ◽  
Author(s):  
EUGEN RADU
Keyword(s):  
Magnetic Field ◽  
Black Hole ◽  
External Magnetic Field ◽  
Thermodynamic Properties ◽  
Background Subtraction ◽  
Black Hole Thermodynamics ◽  
Schwarzschild Black Hole

We prove that the thermodynamic properties of a Schwarzschild black hole are unaffected by an external magnetic field passing through it. Apart from the background subtraction prescription, this result is also obtained by using a counterterm method.

WIGGLY STRING SOLUTIONS IN KERR–NEWMAN BLACK HOLE

2011 ◽  
Vol 26 (16) ◽  
pp. 1221-1230 ◽  
Author(s):  
HIROMI SUZUKI
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Equatorial Plane ◽  
Circular Orbit ◽  
Axially Symmetric ◽  
Rotating Black Hole ◽  
Open Strings ◽  
Newman Black Hole ◽  
Kerr Black Holes

Previously we investigated the cosmic wiggly strings in (3+1)-dimensional Schwarzschild, Reissner–Nordström and Kerr black holes. As an extension, the solutions in (3+1)-dimensional axially symmetric charged rotating black hole are investigated. The solution for the wiggly string exhibits open strings lying along the circular orbit in the equatorial plane outside horizon.

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