Relativistic Superdense Star Models of Pseudo Spheroidal Space–time

Tikekar, Ramesh; Jotania, Kanti

doi:10.1142/s021827180500722x

Cited by 40 publications

(33 citation statements)

References 12 publications

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“…The effects of higher dimensions on the mass, size and density of the star is presented. The compact star solution obtained by Tikekar and Jotania [22] is recovered for D = 4. It may be pointed out here that for λ = 2 in the usual four-dimensional space-time (n = 2), the solution obtained by Tikekar and Thomas [13] is relevant.…”

Section: Discussionmentioning

confidence: 63%

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Relativistic star solutions in higher-dimensional pseudospheroidal space-time

Chattopadhyay¹,

Paul

2010

Pramana - J Phys

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We obtain relativistic solutions of a class of compact stars in hydrostatic equilibrium in higher dimensions by assuming a pseudospheroidal geometry for the spacetime. The space-time geometry is assumed to be (D − 1) pseudospheroid immersed in a D-dimensional Euclidean space. The spheroidicity parameter (λ) plays an important role in determining the equation of state of the matter content and the maximum radius of such stars. It is found that the core density of compact objects is approximately proportional to the square of the space-time dimensions (D), i.e., core of the star is denser in higher dimensions than that in conventional four dimensions. The central density of a compact star is also found to depend on the parameter λ. One obtains a physically interesting solution satisfying the acoustic condition when λ lies in the range λ > (D + 1)/(D − 3) for the space-time dimensions ranging from D = 4 to 8 and (D + 1)/(D − 3) < λ < (D 2 − 4D + 3)/(D 2 − 8D − 1) for space-time dimensions ≥9. The non-negativity of the energy density (ρ) constrains the parameter with a lower limit (λ > 1). We note that in the case of a superdense compact object the number of space-time dimensions cannot be taken infinitely large, which is a different result from the braneworld model.

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Section: Discussionmentioning

confidence: 63%

“…Recently, a class of relativistic solution of compact star assuming a pseudospheroidal geometry in four dimensions was obtained by Tikekar and Jotania [22]. The motivation of the paper is to look for the effects of embedding the compact star in a higher-dimensional space-time.…”

Section: Introductionmentioning

confidence: 99%

Relativistic star solutions in higher-dimensional pseudospheroidal space-time

Chattopadhyay¹,

Paul

2010

Pramana - J Phys

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“…X-1 and observed that the equation of state of the ReSS (realistic equation of state of strange star) approximated to linear form is derivable from models based on Vaidya-Tikekar ansatz. We have shown elsewhere [14] that the alternative ansatz suggested by Tikekar and Thomas [15] also has these features and the general threeparameter solution based on it also leads to physically plausible relativistic models of strange stars.…”

Section: Introductionmentioning

confidence: 70%

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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“…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: 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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Relativistic Superdense Star Models of Pseudo Spheroidal Space–time

Cited by 40 publications

References 12 publications

Relativistic star solutions in higher-dimensional pseudospheroidal space-time

Relativistic star solutions in higher-dimensional pseudospheroidal space-time

On relativistic models of strange stars

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

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