Binding in Charged Spherically Symmetric Objects

Corne, Matthew; Kheyfets, Arkady; Piasio, Jennifer; Voegele, Chad

doi:10.1007/s10773-011-0773-3

Cited by 3 publications

(2 citation statements)

References 17 publications

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“…As a final point, we note the very recent claim by Corne et al [75] that 'pure electromagnetic mass cannot exist'. This result seems very puzzling as it raises a question regarding the validity of several classic as well as the seminal work in [5][6][7][8][11][12][13][14][15][16][17][18][19]33,35,[76][77][78].…”

Section: Resultsmentioning

confidence: 64%

“…In this connection we would specially like to mention the study of Arnowitt et al [79] where by considering the same self-energy they conclusively constructed 'pure electromagnetic mass' in the form m = 2|e|, where e is the electric charge. Therefore, we strongly feel that the result of Corne et al [75] needs further investigation with a proper and rigorous methodology.…”

Section: Resultsmentioning

confidence: 95%

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Spherically symmetric charged compact stars

Maurya

Gupta

Ray³

et al. 2015

Eur. Phys. J. C

129

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In this article we consider the static spherically symmetric metric of embedding class 1. When solving the Einstein-Maxwell field equations we take into account the presence of ordinary baryonic matter together with the electric charge. Specific new charged stellar models are obtained where the solutions are entirely dependent on the electromagnetic field, such that the physical parameters, like density, pressure etc. do vanish for the vanishing charge. We systematically analyze altogether the three sets of Solutions I, II, and III of the stellar models for a suitable functional relation of ν(r ). However, it is observed that only the Solution I provides a physically valid and well-behaved situation, whereas the Solutions II and III are not well behaved and hence not included in the study. Thereafter it is exclusively shown that the Solution I can pass through several standard physical tests performed by us. To validate the solution set presented here a comparison has also been made with that of the compact stars, like R X J 1856 − 37, Her X − 1, P S R 1937 + 21, P S R J 1614 − 2230, and P S R J 0348 + 0432, and we have shown the feasibility of the models.

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Section: Resultsmentioning

confidence: 64%

Section: Resultsmentioning

confidence: 95%

Spherically symmetric charged compact stars

Maurya

Gupta

Ray³

et al. 2015

Eur. Phys. J. C

129

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Gravitational binding energy in charged cylindrical symmetry

Sharif

Bhatti

2012

Can. J. Phys.

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Spherically symmetric anisotropic charged neutron stars in f(Q, T) gravity

Das,

Debnath

2024

Eur. Phys. J. C

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In this work, we have investigated a new solution for charged anisotropic compact stellar system in the framework of an extended theory of symmetric teleparallel gravity known as f(Q, T) gravity with the non-metricity term Q and the trace T for energy–momentum tensor. We have constructed a complete set of the gravitational field equations for a non-linear function $$f(Q,T)=\alpha Q + \beta (1+Q^{2}) + \lambda T$$ f ( Q , T ) = α Q + β ( 1 + Q 2 ) + λ T with $$\alpha , \beta $$ α , β and $$\lambda $$ λ are dimensionless constant parameters in case of static spherically symmetric space-time. To evaluate the expression of relevant unknown constants interior space-time has been matched with exterior Reissner–Nordstr$$\ddot{\textrm{o}}$$ o ¨ m metric. We have performed a graphical discussion in detail to test the behavior of physical parameters in the interior region of a stellar system like energy density, radial and tangential pressure, anisotropies of matter portion, electric field intensity etc. Also, to check the physical validity of our solutions, we have performed various tests viz., energy conditions, stability, mass–radius relation, surface redshift etc. The hydrostatic equilibrium position of our stellar system has been analysed through the TOV equation. Finally, we have determined that our stellar structure solutions satisfy all required physical conditions for viability and acceptability in the context of some pulsar like neutron stars. So our model can be used to characterise the neutron stars in f(Q, T) modified gravity.

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Binding in Charged Spherically Symmetric Objects

Cited by 3 publications

References 17 publications

Spherically symmetric charged compact stars

Spherically symmetric charged compact stars

Gravitational binding energy in charged cylindrical symmetry

Spherically symmetric anisotropic charged neutron stars in f(Q, T) gravity

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