Abstract
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.
Highlights
The central energy density of compact stellar object could be of the order of 1015 g cm−3, several times higher than the normal nuclear matter density, and due to the absence of reliable information as regards the behavior of matter at such ultra-high density insight into the structure can be obtained by reference to applicable analytic solutions to the equation of relativistic stellar structure [4]
Through a numerical and a graphical analysis we have demonstrated that the models obtained in Sect. 2.3 satisfy the physical requirements for a wide range of values of m, n, p, δ, a, and K, giving us a possibility for different charge variations and anisotropy within the fluid spheres
In this work we have studied some particular simple families of relativistic charged stellar models obtained by solving Einstein–Maxwell field equations for a static spherically symmetric locally anisotropic fluid distribution
Summary
The central energy density of compact stellar object could be of the order of 1015 g cm−3, several times higher than the normal nuclear matter density, and due to the absence of reliable information as regards the behavior of matter at such ultra-high density insight into the structure can be obtained by reference to applicable analytic solutions to the equation of relativistic stellar structure [4]. 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]. The solutions obtained in this work are expected to provide simplified but mathematically easy to analyze charged stellar models with non-zero super-high surface density, which could reasonably model the stellar core of an electrically charged strange quark star by satisfying applicable physical boundary conditions.
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