Paraboloidal Space–times and Relativistic Models of Strange Stars

Jotania, Kanti; Tikekar, Ramesh

doi:10.1142/s021827180600884x

Cited by 45 publications

(30 citation statements)

References 16 publications

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“…Following Sharma et al [12] we have chosen central density ρ 0 = 4.68×10 15 g cm −3 . The behaviour of ρ and P for models obtained for different chosen values of the compactification factor are described graphically in figures 1, 2 and 3 after appropriately scaling the dynamical variables as ρ , P as in [18] using the relations ρ(z) = ρ (z) × 10 14 g cm −3 and P (z) = 7 × 10 33 · P (z) dyn cm −2 .…”

Section: Discussionmentioning

confidence: 99%

“…Finch and Skea have shown that this two-parameter family of solution is not only regular and physically viable for a range of its parameters, but also to a good approximation suitable to describe the interiors of neutron stars in equilibrium by comparing numerical models with neutron star models based on the relativistic mean field theory of Walecka [17]. We shall see in the next section that this family of solutions is also suitable to describe the interiors of other compact stars such as strange stars, hybrid neutron stars etc [18].…”

Section: General Two-parameter Family Of Solutionsmentioning

confidence: 99%

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On relativistic models of strange stars

Tikekar

Jotania

2007

Pramana - J Phys

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The superdense stars with mass-to-size ratio exceeding 0.3 are expected to be made of strange matter. Assuming that the 3-space of the interior space-time of a strange star is that of a three-paraboloid immersed in a four-dimensional Euclidean space, we obtain a two-parameter family of their physically viable relativistic models. This ansatz determines density distribution of the interior self-gravitating matter up to one unknown parameter. The Einstein's field equations determine the fluid pressure and the remaining geometrical variables. The information about mass-to-size ratio together with the conventional boundary conditions lead to the determination of total mass, radius and other parameters of the stellar configuration.

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Section: Discussionmentioning

confidence: 99%

Section: General Two-parameter Family Of Solutionsmentioning

confidence: 99%

On relativistic models of strange stars

Tikekar

Jotania

2007

Pramana - J Phys

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“…Due to cumbersome expressions of (25), (27) and (30), the trend of pressure-density ratio and adiabatic sound speed will be studied numerically after applying the boundary conditions.…”

Section: Properties Of the New Solutionmentioning

confidence: 99%

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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“…This approach leads to physically viable and easily tractable models of superdense stars in equilibrium. Tikekar and Jotania [87,88], Jotania and Tikekar [89] showed that the ansatz suggested by Tikekar and Thomas [90] has these features and the general three-parameter solution based on it also leads to physically plausible relativistic models of strange stars. Several aspects of physical relevance and the maximum mass of class of compact star models, based on Vaidya-Tikekar ansatz, for the both isotropic and anisotropic pressures have been investigated in [53,[91][92][93].…”

Section: Introductionmentioning

confidence: 98%

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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Paraboloidal Space–times and Relativistic Models of Strange Stars

Cited by 45 publications

References 16 publications

On relativistic models of strange stars

On relativistic models of strange stars

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

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

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