Exact anisotropic sphere with polytropic equation of state

Thirukkanesh, S.; Ragel, F. C.

doi:10.1007/s12043-012-0268-7

Cited by 143 publications

(118 citation statements)

References 27 publications

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“…Models IV and VII are found physically viable in the study of compact astrophysical stellar objects. The numerous publications following Tolman's approach include [29,. As might be expected with Tolman's method, unphysical pressure-density configurations are found more frequently than physical ones.…”

Section: Introductionmentioning

confidence: 91%

“…In a very recent past a polytropic quark star model has been suggested [28,29] in order to establish a general framework in which theoretical quark star models could be tested by observations. The key difference between polytropic quark stars and the polytropic model studied previously for normal (i.e., non-quarkian) stars is that the quark star models with nonvanishing density at the stellar surface may not be avoidable due to the strong interaction between quarks which is relevant to the effect of color confinement.…”

Section: Introductionmentioning

confidence: 99%

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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: 91%

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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“…The popular polytropic EOS from Newtonian gravity was shown to lead in the anisotropic Newtonian case to the well-known LaneEmden equations [103] and to their relativistic generalisation in Einstein's gravity [104]. A simple solution for a simple ansatz for λ has been found [105]. Finally a solution with λ and the modified Van der Vaals EOS was presented recently [106].…”

Section: Introductionmentioning

confidence: 98%

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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“…Their approach has the remarkable feature of yielding a quadratic equation of state when appropriate physical bounds are applied. Thirukkanesh and Ragel (2012) and Mafa Takisa and Maharaj (2013a) generated exact anisotropic spheres which are uncharged and charged, respectively. These models have a polytropic equation of state in general; however for particular parameter values quadratic equations of state arise.…”

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confidence: 99%

Compact stars with quadratic equation of state

Ngubelanga

Maharaj

Ray

2015

Astrophys Space Sci

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We provide new exact solutions to the EinsteinMaxwell system of equations for matter configurations with anisotropy and charge. The spacetime is static and spherically symmetric. A quadratic equation of state is utilised for the matter distribution. By specifying a particular form for one of the gravitational potentials and the electric field intensity we obtain new exact solutions in isotropic coordinates. In our general class of models, an earlier model with a linear equation of state is regained. For particular choices of parameters we regain the masses of the stars PSR J1614-2230, 4U 1608-52, PSR J1903+0327, EXO 1745-248 and SAX J1808.4-3658. A comprehensive physical analysis for the star PSR J1903+0327 reveals that our model is reasonable.

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Exact anisotropic sphere with polytropic equation of state

Cited by 143 publications

References 27 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

Analytical study of anisotropic compact star models

Compact stars with quadratic equation of state

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