On relativistic models of strange stars

Tikekar, Ramesh; Jotania, Kanti

doi:10.1007/s12043-007-0043-3

Cited by 50 publications

(39 citation statements)

References 20 publications

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“…For that purpose, we have calculated model parameters (see Tables 1, 2 and 3) by choosing the radius of the compact stars R X J 1856-37,S AX J 1808.4-3658 (SS2) and S AX J 1808.4-3658 (SS1). The calculated mass in Table 1 of the different compact stars are matched well with the proposed values by Li et al [19], Tikekar and Jotania [20] and Thirukkanesh and Ragel [21]. In Fig.…”

Section: Mass-radius Relationsupporting

confidence: 87%

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Generalised model for anisotropic compact stars

Gupta²,

et al. 2016

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In the present investigation an exact generalised model for anisotropic compact stars of embedding class 1 is sought with a general relativistic background. The generic solutions are verified by exploring different physical aspects, viz. energy conditions, mass-radius relation, stability of the models, in connection to their validity. It is observed that the model presented here for compact stars is compatible with all these physical tests and thus physically acceptable as far as the compact star candidates R X J 1856-37, S AX J 1808.4-3658 (SS1) and S AX J 1808.4-3658 (SS2) are concerned.

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Section: Mass-radius Relationsupporting

confidence: 87%

“…In the present article using the observed parameters [19][20][21] of ultra-dense compact stars like RXJ 1856-37, SAX J 1808.4-3658 (SS1) and SAX J 1808.4-3658 (SS2), we have studied the consistency of the proposed model with these compact stars. One may notice that all these stars are nothing but pulsars.…”

Section: Introductionmentioning

confidence: 99%

Generalised model for anisotropic compact stars

Gupta²,

et al. 2016

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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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“…The solution is, in fact, a sub-class of the model developed by Pandya et al (2015). Tikekar and Jotania (2007) have shown that the Finch-Skea model can be used to describe ultra-compact stars like 'strange stars' composed of u, d and s quarks.…”

Section: Introductionmentioning

confidence: 99%

Anisotropic extension of Finch and Skea stellar model

Sharma¹,

Das²,

Thirukkanesh³

2017

Astrophys Space Sci

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In this paper, the spacetime geometry of Finch and Skea [Class. Quantum Grav. 6 (1989) 467] has been utilized to obtain closed-form solutions for a spherically symmetric anisotropic matter distribution. By examining its physical admissibility, we have shown that the class of solutions can be used as viable models for observed pulsars. In particular, a specific class of solutions can be used as an 'anisotropic switch' to examine the impact of anisotropy on the gross physical properties of a stellar configuration. Accordingly, the mass-radius relationship has been analyzed.

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On relativistic models of strange stars

Cited by 50 publications

References 20 publications

Generalised model for anisotropic compact stars

Generalised model for anisotropic compact stars

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

Anisotropic extension of Finch and Skea stellar model

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