A Relativistic Model for Strange Quark Star

Kalam, Mehedi; Usmani, A. A.; Rahaman, Farook; Hossein, Sk. Monowar; Karar, Indrani; Sharma, Ranjan

doi:10.1007/s10773-013-1629-9

Cited by 134 publications

(99 citation statements)

References 15 publications

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“…It is interesting to note that all the data fall within the observed range of the corresponding star's physical parameters [12,22,31,[44][45][46][47]. It would be interesting to perform a comparative study with the data of our Table 3 with that of Table 4 of Maurya et al [25] where they have prepared the table for the value of n = 3.3 only for different compact stars whereas in the present study our table includes a wide range of n = 3 to n = 10,000.…”

Section: Discussionmentioning

confidence: 97%

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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: Discussionmentioning

confidence: 97%

“…It is to further noteworthy that this low value surface redshift is not at unavailable in the literature where Shee et al [43] obtained a numerical value for Z as 0.30 (also see Refs. [12,[44][45][46][47] for a low value surface redshift).…”

Section: Discussionmentioning

confidence: 99%

Generalised model for anisotropic compact stars

Gupta²,

et al. 2016

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“…[45,56,[67][68][69][70]82,95,99,100,102,105,106]. Models with such LEOS are discussed in [65,[93][94][95][96][97][98][99]. Obviously p r 0 = β (ρ 0 − ρ s ) > 0, p rs = 0.…”

Section: Solutions With Linear Eos and Simple Energy Densitymentioning

confidence: 99%

“…There are models with in addition given m, [93,94] or λ [95][96][97][98][99]. There are also models with quadratic EOS and λ [100][101][102].…”

Section: Introductionmentioning

confidence: 99%

Analytical study of anisotropic compact star models

Иванов

2017

Eur. Phys. J. C

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A simple classification is given of the anisotropic relativistic star models, resembling the one of charged isotropic solutions. On the ground of this database, and taking into account the conditions for physically realistic star models, a method is proposed for generating all such solutions. It is based on the energy density and the radial pressure as seeding functions. Numerous relations between the realistic conditions are found and the need for a graphic proof is reduced just to one pair of inequalities. This general formalism is illustrated with an example of a class of solutions with linear equation of state and simple energy density. It is found that the solutions depend on three free constants and concrete examples are given. Some other popular models are studied with the same method.

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“…In recent years, however, several authors followed an alternative approach to present analytical stellar models of electrically neutral/charged compact strange stars within the framework of linear equation of state based on MIT bag model together with a particular choice of metric potentials/mass function [74,[78][79][80][81][82][83][84][85]. Some works also studied the viability of nonlinear EOS based on suitable geometry for the description in the interior 3-spaces of such compact star [11,86].…”

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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A Relativistic Model for Strange Quark Star

Cited by 134 publications

References 15 publications

Generalised model for anisotropic compact stars

Generalised model for anisotropic compact stars

Analytical study of anisotropic compact star models

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

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