A class of regular and well behaved relativistic super-dense star models

Gupta, Yashwant; Maurya, S. K.

doi:10.1007/s10509-010-0503-y

Cited by 61 publications

(38 citation statements)

References 18 publications

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“…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. Charged analogs of the Tolman IV and VII models [106][107][108]), as the neutral ones, exhibit the physical features required for the construction of a physically realizable relativistic compact stellar structure. The charged analogs of the Vaidya-Tikekar models have been derived in [109,110].…”

Section: Introductionmentioning

confidence: 99%

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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Section: Introductionmentioning

confidence: 99%

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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“…g 44 = B(1 + Cr 2 ) n for every integral value of n (neutral analogue of such solutions are already published by Gupta 2011a, 2011b). The charged fluid models for some integral value of n have already derived by Pant et al (2010Pant et al ( , 2011a for n = 3, Pant (2011) for n = 4, Gupta and Maurya (2011) for n = 5, Gupta (2011a, 2011b) for n = 6, and Pant et al (2011b) for n = 1, 2 and 7.…”

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confidence: 98%

Extremization of mass of charged superdense star models describe by Durgapal type space-time metric

Maurya

Gupta

2011

Astrophys Space Sci

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In the present article, we have obtained a class of charged superdense star models, starting with a static spherically symmetric metric in curvature coordinates by considering Durgapal (J. Phys. A 15:2637, 1982) type metric i.e. g 44 = B(1 + Cr 2 ) n , where n being any positive integer. It is observed that the maximum mass of the charged fluid models is monotonically increasing with the increasing values of n ≤ 4. For n ≥ 4, the maximum mass of the charged fluid models is throughout monotonically decreasing and over all maximum mass is attained at n = 4. The present metric tends to another metric which describes the charged analogue of Kuchowicz neutral solution as n → ∞. Consequently the lower limit of maximum mass of the charged fluid models could be determined and found to be 5.1165 solar mass with corresponding radius 18.0743 Km. While the upper limit of maximum mass of the model of this category is already known to be 5.7001 solar mass with corresponding radius 17.1003 Km for n = 4. The solutions so obtained are well behaved.

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“…It has been shown that presence of electromagnetic field influences the values of redshift, luminosities and maximum mass of CO [2,3]. Gupta and Maurya [4,5] found regular and well behaved charged models of super-dense star for particular choice of metric potential g 44 and electric field intensity. Pant et al [6] shown that a charged solution possess positively finite pressure and density at the center which fulfill the casuality condition, i.e., d P r dρ ≤ 1.…”

Section: Introductionmentioning

confidence: 99%

Anisotropic charged physical models with generalized polytropic equation of state

Nasim

Azam

2018

Eur. Phys. J. C

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In this paper, we found the exact solutions of Einstein-Maxwell equations with generalized polytropic equation of state (GPEoS). For this, we consider spherically symmetric object with charged anisotropic matter distribution. We rewrite the field equations into simple form through transformation introduced by Durgapal (Phys Rev D 27:328, 1983) and solve these equations analytically. For the physically acceptability of these solutions, we plot physical quantities like energy density, anisotropy, speed of sound, tangential and radial pressure. We found that all solutions fulfill the required physical conditions. It is concluded that all our results are reduced to the case of anisotropic charged matter distribution with linear, quadratic as well as polytropic equation of state.

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A class of regular and well behaved relativistic super-dense star models

Cited by 61 publications

References 18 publications

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

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

Extremization of mass of charged superdense star models describe by Durgapal type space-time metric

Anisotropic charged physical models with generalized polytropic equation of state

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