ON THE LINEARIZATION OF THE BELINSKI-ALEKSEEV EXACT SOLUTION FOR TWO CHARGED MASSES IN EQUILIBRIUM

2008 ◽  
Vol 23 (08) ◽  
pp. 1226-1230 ◽  
Author(s):  
D. BINI ◽  
A. GERALICO ◽  
R. RUFFINI
Keyword(s):  
Exact Solution ◽  
Black Hole ◽  
Massive Particle ◽  
Body System ◽  
Perturbative Solution ◽  
Charged Masses

A perturbative solution describing a two-body system consisting of a Reissner-Nordström black hole and a charged massive particle at rest is presented. The coincidence between such a solution and the linearized form of the recently obtained Belinski-Alekseev exact solution is explicitly shown.

scholarly journals Spectroscopy of z=0 Lifshitz Black Hole

2018 ◽  
Vol 2018 ◽  
pp. 1-7 ◽  
Author(s):  
Gulnihal Tokgoz ◽  
Izzet Sakalli
Keyword(s):  
Exact Solution ◽  
Black Hole ◽  
Normal Modes ◽  
Hawking Temperature ◽  
Massive Scalar ◽  
Local Mass ◽  
Entropy Formula ◽  
Adiabatic Invariant Quantity ◽  
Lifshitz Black Hole ◽  
Area Spectra

We studied the thermodynamics and spectroscopy of a 4-dimensional, z=0 Lifshitz black hole (Z0LBH). Using Wald’s entropy formula and the Hawking temperature, we derived the quasi-local mass of the Z0LBH. Based on the exact solution to the near-horizon Schrödinger-like equation (SLE) of the massive scalar waves, we computed the quasi-normal modes of the Z0LBH via employing the adiabatic invariant quantity for the Z0LBH. This study shows that the entropy and area spectra of the Z0LBH are equally spaced.

The relation between a black hole and a general black body system

2010 ◽  
Vol 19 (1) ◽  
pp. 010403-4 ◽  
Author(s):  
Zhou Shi-Wei ◽  
Liu Bo ◽  
Huang Ji-Li ◽  
Liu Wen-Biao
Keyword(s):  
Black Hole ◽  
Black Body ◽  
Body System

scholarly journals ELECTRIC FORCE LINES OF THE DOUBLE REISSNER–NORDSTROM EXACT SOLUTION

2008 ◽  
Vol 17 (08) ◽  
pp. 1159-1177 ◽  
Author(s):  
ARMANDO PAOLINO ◽  
MARCO PIZZI
Keyword(s):  
Exact Solution ◽  
Black Hole ◽  
Electric Fields ◽  
Maxwell Equation ◽  
Naked Singularity ◽  
Extreme Case ◽  
The Other ◽  
Electric Force ◽  
Coordinate Systems ◽  
Equal Sign

Recently Alekseev and Belinski have presented a new exact solution to the Einstein–Maxwell equation which describes two Reissner–Nordstrom (RN) sources in reciprocal equilibrium (no struts or strings); one source is a naked singularity, the other is a black hole: this is the only possible configuration for two separable objects, apart from the well-known extreme case (mi = ei). In the present paper, after a brief summary of this solution, we study in some detail the coordinate systems used and the main features of the gravitational and electric fields. In particular, we graph the plots of the electric force lines in three qualitatively different situations: equal-sign charges, opposite charges and the case of a naked singularity near a neutral black hole.

The motion of a charged black hole in an electromagnetic field

1980 ◽  
Vol 371 (1746) ◽  
pp. 429-438 ◽  
Keyword(s):  
Exact Solution ◽  
Black Hole ◽  
Electromagnetic Field ◽  
Approximate Solution ◽  
Electric Field ◽  
Hamiltonian Formalism ◽  
Charged Black Hole ◽  
Uniform Electric Field ◽  
Inertial Observer ◽  
Gravitational Perturbations

The motion of a charged black hole in a weak, asymptotically uniform electric field is analysed by using the Hamiltonian formalism for coupled electromagnetic and gravitational perturbations of the Reissner-Nordstrom space-time. The hole is shown to accelerate with respect to a distant inertial observer according to Newton’s law. The relation of the approximate solution obtained to the exact solution of Ernst, representing the charged C-metric without nodal singularity, is then clarified.

On the collision of impulsive gravitational waves when coupled with fluid motions

1985 ◽  
Vol 402 (1822) ◽  
pp. 37-65 ◽  
Keyword(s):  
Exact Solution ◽  
Gravitational Waves ◽  
Massive Particle ◽  
Natural Generalization ◽  
Space Time ◽  
Direct Result ◽  
Sound Waves ◽  
Time Singularity ◽  
Consistent Extension ◽  
Ultimate Result

An exact solution of Einstein’s equations, with a source derived from a perfect fluid in which the energy density, ε , is equal to the pressure, p , is obtained. The solution describes the space–time following the collision of plane impulsive gravitational waves and is the natural generalization of the Nutku─Halil solution of the vacuum equations, in the region of interaction under similar basic conditions. A consistent extension of the solution, prior to the instant of collision, requires that the fluid in the region of interaction is the direct result of a transformation of incident null-dust (i. e. of massless particles describing null trajectories). The ultimate result of the collision is the development of a space─time singularity, the nature of which is strongly dependent on the amplitude and the character of the sound waves that are present. The distribution of ε that follows the collision has many intriguing features. The solution obtained in this paper provides the first example of an induced transformation of a massless into a massive particle.

scholarly journals TACHYON EFFECTS ON THE TWO-DIMENSIONAL BLACK HOLE GEOMETRY

1995 ◽  
Vol 10 (18) ◽  
pp. 1277-1286 ◽  
Author(s):  
G.A. DIAMANDIS ◽  
B.C. GEORGALAS ◽  
E. PAPANTONOPOULOS
Keyword(s):  
Exact Solution ◽  
Black Hole ◽  
Black Hole Solution ◽  
Equations Of Motion ◽  
Tree Level ◽  
Two Dimensional ◽  
Full System ◽  
Dimensional Black Hole ◽  
Hole Geometry ◽  
Hole Structure

We study solutions of the tree level string effective action in the presence of the tachyon mode. In the case of static fields we find numerically that the full system has a black hole solution with the tachyon regular at the horizon. We also find a nonstatic exact solution of the equations of motion having a black hole structure with a past singularity.

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.

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