Isotropic Cases of Static Charged Fluid Spheres in General Relativity

Das, Basanti; Ray, Pulak; Radinschi, Irina; Rahaman, Farook; Ray, Saibal

doi:10.1142/s0218271811019724

Cited by 37 publications

(26 citation statements)

References 23 publications

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“…Our class of solution comprises a particular well behaved solution previously derived by one of us [44]. In continuation of our previous work [45] we present here a new class of solutions of Einstein-Maxwell field equations with well behaved neutral counterpart in isotropic coordinates by motivation of Das et al [46], Ivanov [47], and Murad and Pant [48]. Such solutions are expected to provide simplified but easy to mathematically analyzed compact stellar models of bare strange quark star, a star with nonzero ultra-high surface density.…”

Section: Introductionmentioning

confidence: 82%

A Class of Super Dense Stars Models Using Charged Analogues of Hajj-Boutros Type Relativistic Fluid Solutions

2014

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We present a spherically symmetric solution of the general relativistic field equations in isotropic coordinates for perfect charged fluid, compatible with a super dense star modeling. The solution is well behaved for all the values of Schwarzschild parameter u lying in the range 0 < u < 0.1727 for the maximum value of charge parameter K = 0.08163. The maximum mass of the fluid distribution is calculated by using stellar surface density as ρ b = 4.6888 × 10 14 g cm −3 . Corresponding to K = 0.08 and u max = 0.1732, the resulting well behaved solution has a maximum mass M = 0.9324M and radius R = 8.00 and by assuming ρ b = 2 × 10 14 g cm −3 the solution results a stellar configuration with maximum mass M = 1.43M and radius R b = 12.25 km. The maximum mass is found increasing with increasing K up to 0.08. The well behaved class of relativistic stellar models obtained in this work might has astrophysical significance in the study of internal structure of compact star such as neutron star or self-bound strange quark star like Her X-1.

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Section: Introductionmentioning

confidence: 82%

A Class of Super Dense Stars Models Using Charged Analogues of Hajj-Boutros Type Relativistic Fluid Solutions

2014

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“…For further studies on different aspects of electromagnetic mass models, see Refs. [32][33][34][35][36][37][38].…”

Section: Introductionmentioning

confidence: 99%

Spherically symmetric charged compact stars

Maurya

Gupta

Ray³

et al. 2015

Eur. Phys. J. C

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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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“…Numerous investigations have been performed in GR as well as modified theories to analyze the role of charge on different physical properties of celestial objects. The Einstein field equations coupled with the charge are known as Einstein-Maxwell equations whose solution has been found by Das et al [28] through matching the static interior spacetime with exterior Reissner-Nordström. Sunzu et al [29] examined the quark stars influenced from charge by utilizing the mass-radius relation.…”

Section: Introductionmentioning

confidence: 99%

Influence of Charge on Extended Decoupled Anisotropic Solutions in $f(\mathcal{R},\mathcal{T},\mathcal{R}_{λξ}\mathcal{T}^{λξ})$ Gravity

Sharif,

Naseer

2022

Preprint

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In this paper, we consider static self-gravitating spherical spacetime and determine various anisotropic solutions through the extended gravitational decoupling technique in f (R, T , R λξ T λξ ) gravity to analyze the influence of electromagnetic field on them. We construct two different sets of modified field equations by employing the transformations on both radial as well as temporal metric potentials. The first set symbolizes the isotropic fluid distribution, thus we take Krori-Barua solution to deal with it. The indefinite second sector comprises the influence of anisotropy. In this regard, we apply some constraints to determine unknowns. Further, we observe the impact of charge as well as decoupling parameter ζ on the developed physical variables (such as energy density, radial and tangential pressures) and anisotropy. We also analyze other physical features of the compact geometry like mass, compactness and redshift along with the energy conditions. Eventually, we find that our both solutions show less stable behavior for higher values of charge near the boundary in this gravity.

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Isotropic Cases of Static Charged Fluid Spheres in General Relativity

Cited by 37 publications

References 23 publications

A Class of Super Dense Stars Models Using Charged Analogues of Hajj-Boutros Type Relativistic Fluid Solutions

A Class of Super Dense Stars Models Using Charged Analogues of Hajj-Boutros Type Relativistic Fluid Solutions

Spherically symmetric charged compact stars

Influence of Charge on Extended Decoupled Anisotropic Solutions in $f(\mathcal{R},\mathcal{T},\mathcal{R}_{λξ}\mathcal{T}^{λξ})$ Gravity

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