On the Energy of a Non-Singular Black Hole Solution Satisfying the Weak Energy Condition

Radinschi, Irina; Grammenos, Th.; Rahaman, Farook; Cazacu, Marius Mihai; Spanou, A.; Chakraborty, Joydeep

doi:10.3390/universe6100169

Cited by 6 publications

(4 citation statements)

References 54 publications

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“…The appearance of these discontinuities, that hinders the limit calculation for arbitrary mass M and charge q , is of purely mathematical origin and can be possibly attributed to the complicated functional form of the metric coefficient stemming from the coupling of gravity with non‐linear electrodynamics. A similar behavior of the Møller energy‐momentum complex was found in our previous work (Radinschi et al 2016, 2017, 2020a, 2020b) where again there was a coupling with non‐linear electrodynamics.…”

Section: Results and Conclusionsupporting

confidence: 88%

Einstein and Møller energies of a particular asymptotically Reissner–Nordström non‐singular black hole solution

et al. 2021

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The localization of energy-momentum for a four-dimensional charged, static, and spherically symmetric, non-singular black hole solution that asymptotically behaves as a Reissner-Nordström solution, is studied. The space-time geometry is distinguished by a particular distribution function entering the mass function m(r). The non-singular character of the metric is warranted by the coupling of general relativity with a non-linear electrodynamics, whereby the resulting electric field is everywhere non-singular and asymptotically tends to the Maxwell field. The energy and momentum distributions are computed by applying the Einstein and Møller energy-momentum complexes. It is found that all the momenta vanish, while the energies depend on the electric charge, the mass, and the radial coordinate. Finally, the behavior of the energies near the origin, near infinity, as well as in the case of a vanishing electric charge is examined.

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Section: Results and Conclusionsupporting

confidence: 88%

Einstein and Møller energies of a particular asymptotically Reissner–Nordström non‐singular black hole solution

et al. 2021

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“…Thus, their application requires the use of Cartesian or quasi-Cartesian coordinates, while particularly for the Møller prescription any coordinate system can be utilized for a given gravitational background. Despite the cavil raised by the aforementioned coordinate dependence (see, e.g., [8,9]), the last three decades have known a reinstatement of the energy-momentum complexes justified by a number of physically reasonable and compelling results for various (d + 1)-dimensional space-time geometries, where d = 1, 2, 3 [10][11][12][13][14][15][16][17][18][19][20][21][22][23][24], obtained by different localization prescriptions. In fact, it should be pointed out that different complexes have given the same energy-momentum distribution for any metric belonging to the Kerr-Schild class and for more general metrics [25][26][27].…”

Section: Introductionmentioning

confidence: 99%

Einstein and Møller Energy-Momentum Distributions for the Static Regular Simpson–Visser Space-Time

et al. 2021

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Energy-momentum localization for the four-dimensional static and spherically symmetric, regular Simpson–Visser black hole solution is studied by use of the Einstein and Møller energy-momentum complexes. According to the particular values of the parameter of the metric, the static Simpson–Visser solution can possibly describe the Schwarzschild black hole solution, a regular black hole solution with a one-way spacelike throat, a one-way wormhole solution with an extremal null throat, or a traversable wormhole solution of the Morris–Thorne type. In both prescriptions it is found that all the momenta vanish, and the energy distribution depends on the mass m, the radial coordinate r, and the parameter a of the Simpson–Visser metric. Several limiting cases of the results obtained are discussed, while the possibility of astrophysically relevant applications to gravitational lensing issues is pointed out.

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“…Besides that, the biggest lack was there is no precise definition of a pseudo tensor in the general relativity. Some interesting results have been found recently by using different energy-momentum complexes in the general theory of relativity (see for example, [25] [26] [27] [28] [29]).…”

Section: Introductionmentioning

confidence: 99%

Energy-Momentum Density of Non-Diagonal Bianchi Type Space-Time in General Relativity and Teleparallel Gravity

Gad¹,

Alharbi²

2021

JAMP

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We calculated the energy-momentum density of non-diagonal Bianchi type space-time in two different theories of gravity, General relativity (GR) and the theory of Teleparallel gravity (TG). Firstly, by applying Einstein, Landau-Lifshitz, Bergmann-Thomson and Møller prescriptions, using double index complexes in GR. Secondly, in the frame work of TG, we used the energy momentum complexes of Einstein, Bergmann-Thomson and Landau-Lifshitz. We also study the spacial cases of non-diagonal Bianchi type space-time BII, BVIII and BIX. We obtained the same energy-momentum density components for Einstein and Bergmann-Thomson prescriptions for the above four mentioned space-times that we considered in our work. Also, we found that the energy density component in Møller prescription is zero for all Bianchi types space-times in GR. Furthermore, we show that if the metric components are functions of time t alone, then the total gravitational energy is identically zero.

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On the Energy of a Non-Singular Black Hole Solution Satisfying the Weak Energy Condition

Cited by 6 publications

References 54 publications

Einstein and Møller energies of a particular asymptotically Reissner–Nordström non‐singular black hole solution

Einstein and Møller energies of a particular asymptotically Reissner–Nordström non‐singular black hole solution

Einstein and Møller Energy-Momentum Distributions for the Static Regular Simpson–Visser Space-Time

Energy-Momentum Density of Non-Diagonal Bianchi Type Space-Time in General Relativity and Teleparallel Gravity

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