Charged fluid sphere in general relativity

Pant, D. N.; Sah, Archana N.

doi:10.1063/1.524059

Cited by 38 publications

(30 citation statements)

References 2 publications

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“…To this end questions came up regarding the stability of the charged sphere and also about the amount of charge of the star. A good amount of work has been done by several authors on the stability issue [64][65][66][67][68][69]. On the other hand, in some recent studies [47,70,71] we find an estimate of the electric charge in compact stars, which amounts to a huge charge of the order of 10 19 -10 20 Coulomb.…”

Section: Resultsmentioning

confidence: 91%

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: 91%

Spherically symmetric charged compact stars

Maurya

Gupta

Ray³

et al. 2015

Eur. Phys. J. C

129

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“…For strange quark stars, the energy density does not vanish at the surface. Known applicable analytic solutions include [4,5,22]: In contrast, as far the literature is concerned known to the present authors, the charged analogs of Tolman's models (V-VI) obtained in [95][96][97][98][99][100][101] are not physically viable in the description of compact astrophysical objects as regards the infinite values of the central density and pressure. Though the Schwarzschild constant density solution is physically unrealistic, the charged analogs, obtained in [56,[102][103][104], and the charged analog of the Matese and Whitman solution, obtained in [105], may be relevant in the description of self-bound electrically charged strange quark stars.…”

Section: Introductionmentioning

confidence: 97%

Some new Wyman–Leibovitz–Adler type static relativistic charged anisotropic fluid spheres compatible to self-bound stellar modeling

Murad

Fatema

2015

Eur. Phys. J. C

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In this work some families of relativistic anisotropic charged fluid spheres have been obtained by solving the Einstein-Maxwell field equations with a preferred form of one of the metric potentials, and suitable forms of electric charge distribution and pressure anisotropy functions. The resulting equation of state (EOS) of the matter distribution has been obtained. Physical analysis shows that the relativistic stellar structure for the matter distribution considered in this work may reasonably model an electrically charged compact star whose energy density associated with the electric fields is on the same order of magnitude as the energy density of fluid matter itself (e.g., electrically charged bare strange stars). Furthermore these models permit a simple method of systematically fixing bounds on the maximum possible mass of cold compact electrically charged self-bound stars. It has been demonstrated, numerically, that the maximum compactness and mass increase in the presence of an electric field and anisotropic pressures. Based on the analytic models developed in this present work, the values of some relevant physical quantities have been calculated by assuming the estimated masses and radii of some well-known potential strange star candidates like PSR J1614-2230, PSR J1903+327, Vela X-1, and 4U 1820-30.

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“…Objects of this kind have been investigated previously [1,2,3]. The principal domains of application are the search for charged astrophysical objects [4,5] and the general relativistic generalization of the Lorentz theory of the extended electron model [6,7,8], the second of which was based originally on a belief that, in general relativity, gravitational binding might stabilize a pure electromagnetic object. A very simple, model independent analysis below shows that it is impossible in principle.…”

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confidence: 99%

Non-localizability of electric coupling and gravitational binding of charged objects

Corne¹,

Kheyfets²,

Miller³

2007

Class. Quantum Grav.

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Abstract. The energy-momentum tensor in general relativity contains only localized contributions to the total energy-momentum. Here, we consider a static, spherically symmetric object consisting of a charged perfect fluid.For this object, the total gravitational mass contains a non-localizable contribution of electric coupling (ordinarily associated with electromagnetic mass). We derive an explicit expression for the total mass which implies that the non-localizable contribution of electric coupling is not bound together by gravity, thus ruling out existence of the objects with pure Lorentz electromagnetic mass in general relativity.PACS numbers: 04.60.+n, 04.20.Cv, 04.20.Fy In general relativity, the energy-momentum tensor is determined as the variational derivative of the matter lagrangian with respect to the spacetime metric. For systems that include charged matter (either charged particles or charged fluid), the matter lagrangian is composed of the lagrangian of particles, lagrangian of the electromagnetic field, and the interaction lagrangian (interaction between the particles or fluid and the electromagnetic field). An interesting feature of the variational procedure that yields the energy-momentum tensor is that the interaction term does not contribute to the energymomentum. The total energy-momentum tensor is the sum of the energy-momentum of the particles (or fluid) and the energy-momentum of the electromagnetic field. This does not mean that the electromagnetic coupling between particles (or inside the fluid) does not contribute to the total energy of the system. The correct interpretation of the situation is that the contribution of the electromagnetic coupling is not localizable; it cannot be described by the energy-momentum tensor, which represents the distribution density (hence localization) of energy-momentum-stress. Rather, it should result from integration of some quantity over the object.This feature is by no means unique for electromagnetic coupling. For instance, it takes place in gravitational coupling. The gravity field itself does not contribute to the energy-momentum tensor but, in the theory of neutral spherical stars, does provide a

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Charged fluid sphere in general relativity

Cited by 38 publications

References 2 publications

Spherically symmetric charged compact stars

Spherically symmetric charged compact stars

Some new Wyman–Leibovitz–Adler type static relativistic charged anisotropic fluid spheres compatible to self-bound stellar modeling

Non-localizability of electric coupling and gravitational binding of charged objects

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