scholarly journals Tidal forces in the charged Hayward black hole spacetime

2020 ◽  
Vol 29 (11) ◽  
pp. 2041014
Author(s):  
Haroldo C. D. Lima ◽  
Luís C. B. Crispino
Keyword(s):  
Black Hole ◽  
Initial Conditions ◽  
Radial Coordinate ◽  
Geodesic Deviation ◽  
Regular Black Hole ◽  
Tidal Forces ◽  
Deviation Equation ◽  
Spacetime Curvature ◽  
Black Hole Spacetime ◽  
Electrically Charged

Tidal forces produced by black holes are an important result of General Relativity related to the spacetime curvature tensor. Among the astrophysical implications of tidal forces, the tidal disruption events stand out. We analyze the tidal forces in the spacetime of an electrically charged Hayward regular black hole, obtaining the components of the tidal tensor and the geodesic deviation equation. We find that the radial and angular tidal forces may vanish and change sign unlike in the Schwarzschild spacetime. We note that tidal forces are finite at the origin of the radial coordinate in this regular black hole spacetime. We obtain the geodesic deviation vector for a body constituted of dust infalling towards the black hole with two different initial conditions.

scholarly journals Tidal effects in 4D Einstein–Gauss–Bonnet black hole spacetime

2021 ◽  
Vol 81 (7) ◽  
Author(s):  
Jing Li ◽  
Songbai Chen ◽  
Jiliang Jing
Keyword(s):  
Black Hole ◽  
Initial Conditions ◽  
Tidal Force ◽  
Coupling Constant ◽  
Tidal Effects ◽  
Schwarzschild Spacetime ◽  
Geodesic Deviation ◽  
Tidal Forces ◽  
Black Hole Spacetime ◽  
Deviation Vector

AbstractWe have investigated tidal forces and geodesic deviation motion in the 4D-Einstein–Gauss–Bonnet spacetime. Our results show that tidal force and geodesic deviation motion depend sharply on the sign of Gauss–Bonnet coupling constant. Comparing with Schwarzschild spacetime, the strength of tidal force becomes stronger for the negative Gauss–Bonnet coupling constant, but is weaker for the positive one. Moreover, tidal force behaves like those in the Schwarzschild spacetime as the coupling constant is negative, and like those in Reissner–Nordström black hole as the constant is positive. We also present the change of geodesic deviation vector with Gauss–Bonnet coupling constant under two kinds of initial conditions.

scholarly journals Tidal forces in Kottler spacetimes

2021 ◽  
Vol 81 (7) ◽  
Author(s):  
V. P. Vandeev ◽  
A. N. Semenova
Keyword(s):  
Black Hole ◽  
Cosmological Constant ◽  
Radial Component ◽  
Tidal Force ◽  
De Sitter ◽  
Geodesic Deviation ◽  
Tidal Forces ◽  
Sitter Spacetime ◽  
Deviation Equation ◽  
Deviation Vector

AbstractThe article considers tidal forces in the vicinity of the Kottler black hole. We find a solution of the geodesic deviation equation for radially falling bodies, which is determined by elliptic integrals. And also the asymptotic behavior of all spatial geodesic deviation vector components were found. We demonstrate that the radial component of the tidal force changes sign outside the single event horizon for any negative values of the cosmological constant, in contrast to the Schwarzschild black hole, where all the components of the tidal force are sign-constant. We also find the similarity between the Kottler black hole and the Reissner–Nordström black hole, because we indicate the value of the cosmological constant, which ensures the existence of two horizons of the black hole, between which the angular components of the tidal force change sign. It was possible to detect non-analytical behavior of geodesic deviation vector components in anti-de Sitter spacetime and to describe it locally.

scholarly journals Geodesic motion in a charged 2D stringy black hole spacetime

2014 ◽  
Vol 29 (29) ◽  
pp. 1450157 ◽  
Author(s):  
Rashmi Uniyal ◽  
Hemwati Nandan ◽  
K. D. Purohit
Keyword(s):  
Black Hole ◽  
Tidal Force ◽  
Two Dimensional ◽  
Geodesic Deviation ◽  
Deviation Equation ◽  
Test Particles ◽  
Exactly Solvable ◽  
Black Hole Spacetime ◽  
Geodesic Deviation Equation ◽  
Deviation Vector

We study the time-like geodesics and geodesic deviation for a two-dimensional (2D) stringy black hole (BH) spacetime in Schwarzschild gauge. We have analyzed the properties of effective potential along with the structure of the possible orbits for test particles with different settings of BH parameters. The exactly solvable geodesic deviation equation is used to obtain corresponding deviation vector. The nature of deviation and tidal force is also examined in view of the behavior of corresponding deviation vector. The results are also compared with an another 2D stringy BH spacetime.

scholarly journals Energy Distribution of a Regular Black Hole Solution in Einstein-Nonlinear Electrodynamics

2015 ◽  
Vol 2015 ◽  
pp. 1-12 ◽  
Author(s):  
I. Radinschi ◽  
F. Rahaman ◽  
Th. Grammenos ◽  
A. Spanou ◽  
Sayeedul Islam
Keyword(s):  
Black Hole ◽  
Positive Integer ◽  
Energy Distribution ◽  
Black Hole Solution ◽  
Mass Function ◽  
Nonlinear Electrodynamics ◽  
Radial Coordinate ◽  
Regular Black Hole ◽  
Limiting Behavior ◽  
Special Case

A study about the energy momentum of a new four-dimensional spherically symmetric, static and charged, regular black hole solution developed in the context of general relativity coupled to nonlinear electrodynamics is presented. Asymptotically, this new black hole solution behaves as the Reissner-Nordström solution only for the particular valueμ=4, whereμis a positive integer parameter appearing in the mass function of the solution. The calculations are performed by use of the Einstein, Landau-Lifshitz, Weinberg, and Møller energy momentum complexes. In all the aforementioned prescriptions, the expressions for the energy of the gravitating system considered depend on the massMof the black hole, its chargeq, a positive integerα, and the radial coordinater. In all these pseudotensorial prescriptions, the momenta are found to vanish, while the Landau-Lifshitz and Weinberg prescriptions give the same result for the energy distribution. In addition, the limiting behavior of the energy for the casesr→∞,r→0, andq=0is studied. The special caseμ=4andα=3is also examined. We conclude that the Einstein and Møller energy momentum complexes can be considered as the most reliable tools for the study of the energy momentum localization of a gravitating system.

scholarly journals MOTION OF CHARGED PARTICLES ON THE REISSNER–NORDSTRÖM (ANTI)-DE SITTER BLACK HOLE SPACETIME

2011 ◽  
Vol 26 (39) ◽  
pp. 2923-2950 ◽  
Author(s):  
MARCO OLIVARES ◽  
JOEL SAAVEDRA ◽  
CARLOS LEIVA ◽  
JOSÉ R. VILLANUEVA
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Charged Particles ◽  
De Sitter ◽  
Point Particles ◽  
Charged Black Holes ◽  
Black Hole Spacetime ◽  
Jacobi Functions ◽  
Electrically Charged ◽  
Charged Point

We study the motion of relativistic, electrically charged point particles in the background of charged black holes with nontrivial asymptotic behavior. We compute the exact trajectories of massive particles and express them in terms of elliptic Jacobi functions. As a result, we obtain a detailed description of particles orbits in the gravitational field of Reissner–Nordström (anti)-de Sitter black hole, depending of their charge, mass and energy.

scholarly journals Regular black hole interior spacetime supported by three-form field

2021 ◽  
Vol 81 (4) ◽  
Author(s):  
Mariam Bouhmadi-López ◽  
Che-Yu Chen ◽  
Xiao Yan Chew ◽  
Yen Chin Ong ◽  
Dong-han Yeom
Keyword(s):  
Black Hole ◽  
Energy Condition ◽  
Null Energy Condition ◽  
De Sitter ◽  
Regular Black Hole ◽  
Black Hole Spacetime ◽  
Form Field ◽  
Black Hole Interior ◽  
Metric Function ◽  
Geodesically Complete

AbstractIn this paper, we show that a minimally coupled 3-form endowed with a proper potential can support a regular black hole interior. By choosing an appropriate form for the metric function representing the radius of the 2-sphere, we solve for the 3-form field and its potential. Using the obtained solution, we construct an interior black hole spacetime which is everywhere regular. The singularity is replaced with a Nariai-type spacetime, whose topology is $$\text {dS}_2 \times \text {S}^2$$ dS 2 × S 2 , in which the radius of the 2-sphere is constant. So long as the interior continues to expand indefinitely, the geometry becomes essentially compactified. The 2-dimensional de Sitter geometry appears despite the negative potential of the 3-form field. Such a dynamical compactification could shed some light on the origin of de Sitter geometry of our Universe, exacerbated by the Swampland conjecture. In addition, we show that the spacetime is geodesically complete. The geometry is singularity-free due to the violation of the null energy condition.

scholarly journals Geodesic deviation, Raychaudhuri equation, Newtonian limit, and tidal forces in Weyl-type f(Q, T) gravity

2021 ◽  
Vol 81 (2) ◽  
Author(s):  
Jin-Zhao Yang ◽  
Shahab Shahidi ◽  
Tiberiu Harko ◽  
Shi-Dong Liang
Keyword(s):  
Field Approximation ◽  
The Body ◽  
Newtonian Limit ◽  
Raychaudhuri Equation ◽  
Geodesic Deviation ◽  
Weyl Geometry ◽  
Matter Coupling ◽  
Tidal Forces ◽  
Deviation Equation ◽  
Geodesic Deviation Equation

AbstractWe consider the geodesic deviation equation, describing the relative accelerations of nearby particles, and the Raychaudhuri equation, giving the evolution of the kinematical quantities associated with deformations (expansion, shear and rotation) in the Weyl-type f(Q, T) gravity, in which the non-metricity Q is represented in the standard Weyl form, fully determined by the Weyl vector, while T represents the trace of the matter energy–momentum tensor. The effects of the Weyl geometry and of the extra force induced by the non-metricity–matter coupling are explicitly taken into account. The Newtonian limit of the theory is investigated, and the generalized Poisson equation, containing correction terms coming from the Weyl geometry, and from the geometry matter coupling, is derived. As a physical application of the geodesic deviation equation the modifications of the tidal forces, due to the non-metricity–matter coupling, are obtained in the weak-field approximation. The tidal motion of test particles is directly influenced by the gradients of the extra force, and of the Weyl vector. As a concrete astrophysical example we obtain the expression of the Roche limit (the orbital distance at which a satellite begins to be tidally torn apart by the body it orbits) in the Weyl-type f(Q, T) gravity.

scholarly journals New regular black hole solutions and other electrically charged compact objects with a de Sitter core and a matter layer

2018 ◽  
Vol 27 (11) ◽  
pp. 1843015
Author(s):  
Angel D. D. Masa ◽  
Enesson S. de Oliveira ◽  
Vilson T. Zanchin
Keyword(s):  
Black Hole ◽  
Equation Of State ◽  
Energy Density ◽  
Thin Shell ◽  
Compact Objects ◽  
Interior Solution ◽  
De Sitter ◽  
Regular Black Hole ◽  
Electrically Charged ◽  
Black Hole Solutions

The main objective of this work is the construction of regular black hole solutions in the context of the Einstein–Maxwell theory. The strategy is to match an interior regular solution to an exterior electrovacuum solution. With this purpose, we first write explicitly the Einstein field equations for the interior regular region. We take an electrically charged nonisotropic fluid, which presents spherical symmetry and a de Sitter type equation of state, where the radial pressure [Formula: see text] is equal to the negative of energy density [Formula: see text], [Formula: see text]. Then, two solutions for the Einstein equations are built, a regular interior solution for the region with matter satisfying a de Sitter equation of state, and an external solution for the region outside the matter, that corresponds to the Reissner–Nordström metric. To complete the solution we apply the Darmois–Israel junction conditions with a timelike thin shell at the matching surface. It is assumed that the matching surface is composed by a thin shell of matter, i.e. a surface layer in the form of a perfect fluid obeying a barotropic equation of state, [Formula: see text] and [Formula: see text] being the intrinsic pressure and energy density of the shell, respectively, and [Formula: see text] a constant parameter. We show that there are electrically charged regular black hole solutions and other compact objects for specific choices of [Formula: see text] and of the other parameters of the model. Some properties the objects are investigated.

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