Regular models with quadratic equation of state

Maharaj, S. D.; Takisa, P. Mafa

doi:10.1007/s10714-012-1347-2

Cited by 137 publications

(83 citation statements)

References 30 publications

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“…We determine here two probable EoS in isotropic and anisotropic case both in D = 4 and D = 5. The EoS obtained here are found to have similar to that recently considered by Maharaj and Mafa Takisa Maharaj & Mafa Takisa (2012). From Tables-6 and 7 we note that equation of state becomes softer in higher dimensions.…”

Section: Equation Of State (Eos)supporting

confidence: 86%

Relativistic anisotropic star and its maximum mass in higher dimensions

Paul

Chattopadhyay²,

Karmakar

2015

Astrophys Space Sci

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We present a class of relativistic solutions of cold compact anisotropic stars in hydrostatic equilibrium in the framework of higher dimensions using spheroidal geometry. The solutions obtained with Vaidya-Tikekar metric are used to construct stellar models of compact objects and studied their physical features. The effects of anisotropy and extra dimensions on the global properties namely, compactness, mass, radius, equation of state are determined in higher dimensions in terms of the spheroidicity parameter (λ). It is noted that for a given configuration, compactness of a star is found smaller in higher dimensions compared to that in four space-time dimensions. It is also noted that the maximum mass of compact objects increase with the increase of space-time dimensions which however attains a maximum when D = 5 for a large (λ = 100), thereafter it decreases as one increases number of extra dimensions. The effect of extra dimensions on anisotropy is also studied.

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Section: Equation Of State (Eos)supporting

confidence: 86%

Relativistic anisotropic star and its maximum mass in higher dimensions

Paul

Chattopadhyay²,

Karmakar

2015

Astrophys Space Sci

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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%

“…According to these views, in such massive stellar objects the radial pressure may not be equal to the tangential pressure. Since the pioneering work of Bowers and Liang [127], there has been an extensive literature devoted to the study of anisotropic spherically symmetric static general relativistic configurations (see [75,76,79,82,97, and the references therein).…”

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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“…In a general relativistic context models which are charged and anisotropic were found by Feroze and Siddiqui (2011). A class of models, generalising the results of Feroze and Siddiqui (2011) and containing models with linear equations of state, was found by Maharaj and Mafa Takisa (2012). These solutions have the desirable property of regularity at the stellar centre.…”

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confidence: 93%

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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Regular models with quadratic equation of state

Cited by 137 publications

References 30 publications

Relativistic anisotropic star and its maximum mass in higher dimensions

Relativistic anisotropic star and its maximum mass in higher dimensions

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

Compact stars with quadratic equation of state

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