Electromagnetic and gravitational signatures of accretion into black holes

2015 ◽  
Vol 24 (09) ◽  
pp. 1542004
Author(s):  
Juan Carlos Degollado
Keyword(s):  
Black Hole ◽  
Maxwell Equations ◽  
Einstein Equations ◽  
System Of Differential Equations ◽  
Charged Fluids ◽  
Schwarzschild Black Hole ◽  
Initial Value ◽  
Stationary Black Hole ◽  
Electromagnetic Signals ◽  
Set Up

In this paper, the gravitational and electromagnetic signals due to accretion of charged fluids into a Schwarzschild black hole is revisited. We set up the perturbed Einstein equations and Maxwell equations coupled to the fluid equations on a stationary black hole as a system of differential equations that can be integrated as an initial value problem. We numerically investigate cases in which we varied the properties of the fluid. Our scenario may provide an electromagnetic counterpart to gravitational waves in many situations of interest, enabling easier extraction and verification of gravitational waveforms from gravitational wave detection. We find that the features of the resulting electromagnetic signals depend on the properties and dynamics of the flow.

DE SITTER-SCHWARZSCHILD BLACK HOLE: ITS PARTICLELIKE CORE AND THERMODYNAMICAL PROPERTIES

1996 ◽  
Vol 05 (05) ◽  
pp. 529-540 ◽  
Author(s):  
I.G. DYMNIKOVA
Keyword(s):  
Black Hole ◽  
Lower Limit ◽  
Mass Parameter ◽  
Hawking Temperature ◽  
Einstein Equations ◽  
Black Hole Mass ◽  
De Sitter ◽  
Schwarzschild Black Hole ◽  
Schwarzschild Solution ◽  
Second Order Phase Transition

We analyze the globally regular solution of the Einstein equations describing a black hole whose singularity is replaced by the de Sitter core. The de Sitter—Schwarzschild black hole (SSBH) has two horizons. Inside of it there exists a particlelike structure hidden under the external horizon. The critical value of mass parameter M cr1 exists corresponding to the degenerate horizon. It represents the lower limit for a black-hole mass. Below M cr1 there is no black hole, and the de Sitter-Schwarzschild solution describes a recovered particlelike structure. We calculate the Hawking temperature of SSBH and show that specific heat is broken and changes its sign at the value of mass M cr 2>M cr 1 which means that a second-order phase transition occurs at that point. We show that the Hawking temperature drops to zero when a mass approaches the lower limit M cr1 .

scholarly journals AN INTRODUCTION TO LOCAL BLACK HOLE HORIZONS IN THE 3+1 APPROACH TO GENERAL RELATIVITY

2012 ◽  
Vol 07 ◽  
pp. 31-66
Author(s):  
JOSÉ LUIS JARAMILLO
Keyword(s):  
Black Hole ◽  
First Principles ◽  
Strong Field ◽  
A Priori ◽  
Einstein Equations ◽  
A Posteriori ◽  
Initial Value ◽  
Black Hole Spacetimes ◽  
Local Horizon ◽  
Trapping Horizons

We present an introduction to dynamical trapping horizons as quasi-local models for black hole horizons, from the perspective of an Initial Value Problem approach to the construction of generic black hole spacetimes. We focus on the geometric and structural properties of these horizons aiming, as a main application, at the numerical evolution and analysis of black hole spacetimes in astrophysical scenarios. In this setting, we discuss their dual role as an a priori ingredient in certain formulations of Einstein equations and as an a posteriori tool for the diagnosis of dynamical black hole spacetimes. Complementary to the first-principles discussion of quasi-local horizon physics, we place an emphasis on the rigidity properties of these hypersurfaces and their role as privileged geometric probes into near-horizon strong-field spacetime dynamics.

scholarly journals The weak cosmic censorship conjecture may be violated

2020 ◽  
Author(s):  
Wen-Xiang Chen
Keyword(s):  
Black Hole ◽  
Wave Function ◽  
Boundary Conditions ◽  
Cosmic Censorship ◽  
Traditional Theory ◽  
Schwarzschild Black Hole ◽  
Entropy Reduction ◽  
Set Up ◽  
Coupled Wave ◽  
Cosmic Censorship Conjecture

According to traditional theory, the Schwarzschild black hole does not produce superradiation. If the boundary conditions are set up in advance, this possibility will be combined with the boson-coupled wave function in the Schwarzschild black hole, where the incident boson will have a mirrored mass, so even the Schwarzschild black hole can generate superradiation phenomena.Recently, an article of mine obtained interesting results about the Schwarzschild black hole can generate superradiation phenomena. The result contains some conclusions that violate the "no-hair theorem". We know that the phenomenon of black hole superradiation is a process of entropy reduction I found that the weak cosmic censorship conjecture may be violated.

scholarly journals AN INTRODUCTION TO LOCAL BLACK HOLE HORIZONS IN THE 3+1 APPROACH TO GENERAL RELATIVITY

2011 ◽  
Vol 20 (11) ◽  
pp. 2169-2204 ◽  
Author(s):  
JOSÉ LUIS JARAMILLO
Keyword(s):  
Black Hole ◽  
First Principles ◽  
Strong Field ◽  
A Priori ◽  
Einstein Equations ◽  
A Posteriori ◽  
Initial Value ◽  
Black Hole Spacetimes ◽  
Local Horizon ◽  
Trapping Horizons

We present an introduction to dynamical trapping horizons as quasi-local models for black hole horizons, from the perspective of an Initial Value Problem approach to the construction of generic black hole spacetimes. We focus on the geometric and structural properties of these horizons aiming, as a main application, at the numerical evolution and analysis of black hole spacetimes in astrophysical scenarios. In this setting, we discuss their dual role as an a priori ingredient in certain formulations of Einstein equations and as an a posteriori tool for the diagnosis of dynamical black hole spacetimes. Complementary to the first-principles discussion of quasi-local horizon physics, we place an emphasis on the rigidity properties of these hypersurfaces and their role as privileged geometric probes into near-horizon strong-field spacetime dynamics.

scholarly journals Effect of gravitational wave on shadow of a Schwarzschild black hole

2021 ◽  
Vol 81 (6) ◽  
Author(s):  
Mingzhi Wang ◽  
Songbai Chen ◽  
Jiliang Jing
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Legendre Polynomial ◽  
Vertical Direction ◽  
Einstein Equations ◽  
Schwarzschild Black Hole ◽  
Fractal Structures ◽  
Odd Order ◽  
Particular Solution ◽  
Self Similar

AbstractWe have studied the shadows of a Schwarzschild black hole under a special polar gravitational perturbation, which is a particular solution of Einstein equations expanded up to first order. It is shown that the black hole shadow changes periodically with time and the change of shadow depends on the Legendre polynomial order parameter l and the frequency $$\sigma $$ σ of gravitational wave. For the odd order of Legendre polynomial, the center of shadow oscillates along the direction which is vertical to equatorial plane. For even l, the center of shadow does not move, but the shadow alternately stretches and squeezes with time along the vertical direction. Moreover, the presence of the gravitational wave leads to the self-similar fractal structures appearing in the boundary of the black hole shadow. We also find that this special gravitational wave has a greater influence on the vertical direction of black hole shadow.

scholarly journals CLASSICAL ANALOG OF THE QUANTUM SCHWARZSCHILD BLACK HOLE: LOCAL VS GLOBAL, AND THE MYSTERY OF log 3

2011 ◽  
Vol 26 (01) ◽  
pp. 161-178
Author(s):  
VICTOR BEREZIN
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Event Horizon ◽  
Einstein Equations ◽  
Schwarzschild Black Hole ◽  
Quantum Black Hole ◽  
Classical Analog ◽  
Global Properties

A model is built in which the main global properties of classical and quasiclassical black holes become local. These are the event horizon, "no hair," temperature and entropy. The construction is based on the features of a quantum collapse, discovered when studying some quantum black hole models. But the model is purely classical, and this allows one to use self-consistently the Einstein equations and classical (local) thermodynamics and explain in this way the " log 3" puzzle.

scholarly journals Horizon shells: Classical structure at the horizon of a black hole

2016 ◽  
Vol 25 (12) ◽  
pp. 1644010 ◽  
Author(s):  
Matthias Blau ◽  
Martin O’Loughlin
Keyword(s):  
Black Hole ◽  
Event Horizon ◽  
Infinite Number ◽  
Mass Formula ◽  
Black Hole Physics ◽  
Einstein Equations ◽  
Schwarzschild Black Hole ◽  
Schwarzschild Solution ◽  
Classical Structure ◽  
Codimension One

We address the question of the uniqueness of the Schwarzschild black hole by considering the following question: How many meaningful solutions of the Einstein equations exist that agree with the Schwarzschild solution (with a fixed mass [Formula: see text]) everywhere except maybe on a codimension one hypersurface? The perhaps surprising answer is that the solution is unique (and uniquely the Schwarzschild solution everywhere in spacetime) unless the hypersurface is the event horizon of the Schwarzschild black hole, in which case there are actually an infinite number of distinct solutions. We explain this result and comment on some of the possible implications for black hole physics.

GRAVITATIONAL FIELD AND ELECTRIC FORCE LINES OF A NEW 2-SOLITON SOLUTION

2007 ◽  
Vol 16 (06) ◽  
pp. 1087-1108
Author(s):  
MARCO PIZZI
Keyword(s):  
Black Hole ◽  
Maxwell Equations ◽  
Naked Singularity ◽  
Physical Parameters ◽  
Schwarzschild Black Hole ◽  
Electrical Field ◽  
Conic Singularity ◽  
Mathematical Construction ◽  
Anomaly Region ◽  
Two Bodies

A new exact solution of the coupled Einstein–Maxwell equations is given and studied. It is found using the soliton method, adding one soliton to the Schwarzschild background. The solution is stationary and axial-symmetric, and has five physical parameters. The physical interpretation we give is that it describes a Kerr–Newman (KN) naked singularity linked by a "strut" to a charged black hole. Indeed, on the axis, between the two bodies an unavoidable anomaly region is present (gφφ < 0 and a conic singularity). The solution is stationary also in the case with zero total angular momentum. Finally, we give the force lines of the electrical field in a general case, and in the case in which the KN singularity has a much smaller mass than the nearby black hole; we also considered the behavior at different distances of the charge. In spite of the naive interpretation suggested by the mathematical construction of the solution, what we expected to be a "Schwarzschild" black hole appears to be charged and rotating; we interpret this fact as a parameter-mixing phenomenon.

The Schwarzschild black hole

2018 ◽  
Author(s):  
Nathalie Deruelle ◽  
Jean-Philippe Uzan
Keyword(s):  
Black Hole ◽  
Gravitational Field ◽  
Equilibrium Configuration ◽  
Original Form ◽  
Schwarzschild Black Hole ◽  
Schwarzschild Metric ◽  
Schwarzschild Geometry

This chapter discusses the Schwarzschild black hole. It demonstrates how, by a judicious change of coordinates, it is possible to eliminate the singularity of the Schwarzschild metric and reveal a spacetime that is much larger, like that of a black hole. At the end of its thermonuclear evolution, a star collapses and, if it is sufficiently massive, does not become stabilized in a new equilibrium configuration. The Schwarzschild geometry must therefore represent the gravitational field of such an object up to r = 0. This being said, the Schwarzschild metric in its original form is singular, not only at r = 0 where the curvature diverges, but also at r = 2m, a surface which is crossed by geodesics.

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