Localization of energy for a regular black hole solution in an asymptotically de Sitter spacetime geometry

Open Physics ◽  
2011 ◽  
Vol 9 (5) ◽  
Author(s):  
Irina Radinschi ◽  
Theophanes Grammenos ◽  
Andromahi Spanou
Keyword(s):  
Black Hole ◽  
Black Hole Solution ◽  
Mass Parameter ◽  
De Sitter Spacetime ◽  
De Sitter ◽  
Regular Black Hole ◽  
Spacetime Geometry ◽  
Sitter Spacetime ◽  
Momentum Distributions ◽  
Energy And Momentum

AbstractThe energy and momentum distributions of a regular black hole in a four-dimensional, asymptotically de Sitter spacetime geometry are computed, whereby the Einstein, Landau-Lifshitz, Weinberg and Møller energy-momentum complexes are utilized. It is found, for all prescriptions applied, that the momentum distribution vanishes, while the energy distribution depends on the mass parameter M, the electric charge Q, and the cosmological constant Λ. In addition, various limiting cases are discussed.

BACK REACTION IN SCHWARZSCHILD–de SITTER SPACETIME WITH A MASSLESS QUANTUM FIELD

2006 ◽  
Vol 21 (02) ◽  
pp. 169-179
Author(s):  
P. I. KURIAKOSE ◽  
V. C. KURIAKOSE
Keyword(s):  
Black Hole ◽  
Effective Potential ◽  
Thermal Equilibrium ◽  
Back Reaction ◽  
De Sitter Spacetime ◽  
Quantum Field ◽  
De Sitter ◽  
Spacetime Geometry ◽  
Sitter Spacetime ◽  
Massless Quantum

Back reaction in the Schwarzschild–de Sitter black hole in thermal equilibrium with conformal massless quantum field is discussed using the method of York. The presence of quantum field and back reaction ensures the entropy of dressed black hole. In the perturbed spacetime geometry, the nature of the effective potential and the orbits of massless and massive particles are also investigated.

scholarly journals Localization of Energy and Momentum in an Asymptotically Reissner-Nordström Non-Singular Black Hole Space-Time Geometry

Universe ◽  
2020 ◽  
Vol 6 (5) ◽  
pp. 69
Author(s):  
Irina Radinschi ◽  
Pradyumn Kumar Sahoo ◽  
Theophanes Grammenos ◽  
Surajit Chattopadhyay ◽  
Marius-Mihai Cazacu
Keyword(s):  
Black Hole ◽  
Gravitational Lensing ◽  
Black Hole Solution ◽  
Space Time ◽  
Radial Coordinate ◽  
De Sitter ◽  
Momentum Distributions ◽  
Energy And Momentum ◽  
Two Parameters ◽  
De Sitter Metric

The space-time geometry exterior to a new four-dimensional, spherically symmetric and charged black hole solution that, through a coupling of general relativity with a non-linear electrodynamics, is non-singular everywhere, for small r it behaves as a de Sitter metric, and asymptotically it behaves as the Reissner-Nordström metric, is considered in order to study energy-momentum localization. For the calculation of the energy and momentum distributions, the Einstein, Landau-Lifshitz, Weinberg and Møller energy-momentum complexes were applied. The results obtained show that in all prescriptions the energy depends on the mass M of the black hole, the charge q, two parameters a ∈ Z + and γ ∈ R + , and on the radial coordinate r. The calculations performed in each prescription show that all the momenta vanish. Additionally, some limiting and particular cases for r and q are studied, and a possible connection with strong gravitational lensing and microlensing is attempted.

scholarly journals Einstein and Møller Energy-Momentum Complexes for a New Regular Black Hole Solution with a Nonlinear Electrodynamics Source

2016 ◽  
Vol 2016 ◽  
pp. 1-9 ◽  
Author(s):  
Irina Radinschi ◽  
Farook Rahaman ◽  
Theophanes Grammenos ◽  
Sayeedul Islam
Keyword(s):  
Black Hole ◽  
Black Hole Solution ◽  
Relevant Literature ◽  
Nonlinear Electrodynamics ◽  
Radial Coordinate ◽  
Schwarzschild Black Hole ◽  
Regular Black Hole ◽  
Momentum Distributions ◽  
Energy And Momentum ◽  
Gravitational Background

A study about the energy and momentum distributions of a new charged regular black hole solution with a nonlinear electrodynamics source is presented. The energy and momentum are calculated using the Einstein and Møller energy-momentum complexes. The results show that in both pseudotensorial prescriptions the expressions for the energy of the gravitational background depend on the massMand the chargeqof the black hole, an additional factorβcoming from the spacetime metric considered, and the radial coordinater, while in both prescriptions all the momenta vanish. Further, it is pointed out that in some limiting and particular cases the two complexes yield the same expression for the energy distribution as that obtained in the relevant literature for the Schwarzschild black hole solution.

scholarly journals An exact black hole spacetime with scalar field and its shadow together with quasinormal modes

2020 ◽  
Vol 35 (31) ◽  
pp. 2050256 ◽  
Author(s):  
Shuang Yu ◽  
Changjun Gao
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Black Hole Solution ◽  
Quasinormal Modes ◽  
The Other ◽  
De Sitter Spacetime ◽  
De Sitter ◽  
First Law Of Thermodynamics ◽  
Sitter Spacetime ◽  
Black Hole Spacetime

We find an exact black hole solution with a minimally coupled scalar field. The corresponding spacetime has two horizons and one of them is the black hole event horizon and the other is the cosmic horizon. In this sense, the solution is analogous to the Schwarzschild-de Sitter (or anti-de Sitter) spacetime. We investigate the thermodynamics and construct the first law of thermodynamics. At the same time, we make a study on the shadow and quasinormal modes of this black hole solution.

Teleparallel energy–momentum distribution of various black hole and wormhole metrics

2018 ◽  
Vol 33 (30) ◽  
pp. 1850184 ◽  
Author(s):  
S. Aygün ◽  
H. Baysal ◽  
C. Aktaş ◽  
İ. Yılmaz ◽  
P. K. Sahoo ◽  
...  
Keyword(s):  
Black Hole ◽  
Energy Density ◽  
Teleparallel Gravity ◽  
De Sitter ◽  
Zero Energy ◽  
Energy Distributions ◽  
Regular Black Hole ◽  
Asymptotically Flat ◽  
Momentum Distributions ◽  
Energy And Momentum

Using the Einstein, Bergmann–Thomson (BT) and Landau–Lifshitz (LL) energy and momentum formulations in teleparallel gravity (TG), we obtain the total energy and momentum distributions for phantom black hole metric. We get different energy distributions similar to the earlier study and the momentum distributions vanish for phantom black hole metric in TG. These momentum solutions agree with the study of Sahoo et al. in general relativity. However, using Einstein, Bergmann–Thomson and Landau–Lifshitz energy and momentum complexes, we investigate regular black hole, asymptotically flat wormhole, anti-de Sitter wormhole and Ellis wormhole solutions in TG. We obtain (i) same BT and LL energy density solutions for regular black hole metric, (ii) same and zero energy distribution for asymptotically flat wormhole, (iii) proportion with Einstein and BT energy density solutions for anti-de Sitter wormhole, (iv) same and negative Einstein and BT energy density solutions for Ellis wormhole in TG.

scholarly journals NONSTATIC CHARGED BTZ-LIKE BLACK HOLES IN N+1 DIMENSIONS

2012 ◽  
Vol 21 (03) ◽  
pp. 1250022 ◽  
Author(s):  
SUSHANT G. GHOSH
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Collapse ◽  
Naked Singularity ◽  
De Sitter Spacetime ◽  
De Sitter ◽  
Btz Black Hole ◽  
Sitter Spacetime ◽  
Apparent Horizons ◽  
Sitter Background

We find an exact nonstatic charged BTZ-like solutions, in (N+1)-dimensional Einstein gravity in the presence of negative cosmological constant and a nonlinear Maxwell field defined by a power s of the Maxwell invariant, which describes the gravitational collapse of charged null fluid in an anti-de Sitter background. Considering the situation that a charged null fluid injects into the initially an anti-de Sitter spacetime, we show that a black hole form rather than a naked singularity, irrespective of spacetime dimensions, from gravitational collapse in accordance with cosmic censorship conjecture. The structure and locations of the apparent horizons of the black holes are also determined. It is interesting to see that, in the static limit and when N = 2, one can retrieve 2+1 BTZ black hole solutions.

scholarly journals SPECTRA OF BLACK HOLE IN DE SITTER SPACETIME WITH HIGHLY DAMPED QUASINORMAL MODES: HIGH OVERTONE CASE

2012 ◽  
Vol 27 (23) ◽  
pp. 1250123 ◽  
Author(s):  
MOLIN LIU ◽  
XUEHUI HU ◽  
JUNWANG LU ◽  
JIANBO LU
Keyword(s):  
Black Hole ◽  
Quasinormal Modes ◽  
De Sitter Spacetime ◽  
De Sitter ◽  
Flat Spacetime ◽  
Sitter Spacetime ◽  
Spacetime Structure ◽  
Electrically Charged ◽  
High Overtone ◽  
Charged Case

Motivated by recent physical interpretation on quasinormal modes presented by Maggiore [Phys. Rev. Lett. 100, 141301 (2008)], the adiabatic quantity method given by Kunstatter [Phys. Rev. Lett. 90, 161301 (2003)] is used to calculate the spectrums of a non-extremal Schwarzschild de Sitter black hole in this paper, as well as electrically charged case. According to highly damped Konoplya and Zhidenko's numerical observational results for high overtone modes [JHEP 06, 037 (2004)], we found that the asymptotic non-flat spacetime structure leads to two interesting facts: (i) near inner event horizon, the area and entropy spectrums, which are given by Aen= 8 n1πℏ, Sen= 2πn1ℏ, are equally spaced accurately. (ii) However, near outer cosmological horizon the spectrums, which are in the form of [Formula: see text], are not markedly equidistant. Finally, we also discuss the electrically charged case and find that the black holes in de Sitter spacetime have similar quantization behavior no matter with or without charge.

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