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

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.

On the effect of anisotropy on stellar models

“…Because we have one function more than the number of equations is necessary the assignation of an additional equation or fix one of the functions, in particular we give a form of the redshift factor y [33] which allows us integrate the system. Finding solutions for the equation system (4)- (6) does not implies that these are physically acceptables, minimal conditions over the metric functions are required and over the density and pressures also in order to get a viable model [19,[34][35][36][37]]:…”

Anisotropic fluid spheres of embedding class one using Karmarkar condition

“…In recent times there has been made a considerable effort in modelling observed astrophysical objects in the presence of anisotropy. Some recent research papers addressing this physical feature include the work of Sharma and Ratanpal [4], Ngubelanga et al [5,6], Sunzu et al [7,8], Murad and Fatema [9,10] and Murad [11], and the references therein. The physical analyses contained in these treatments confirm the importance of including nonzero anisotropy in modelling astrophysical objects.…”

A family of solutions to the Einstein–Maxwell system of equations describing relativistic charged fluid spheres

“…and t = m(1 + kx)/k. We, thus have generated two class of solutions (32) and (33) to the differential equation (6) for the assumed electric field (9) making use of the infinite series solution (22). It should be stressed that the class of solutions can be used to study stellar properties in the presence as well as absence of charge.…”

“…It should be stressed that the class of solutions can be used to study stellar properties in the presence as well as absence of charge. By setting α = 0 and β = 0 (d = 0 or 3 2 ) in (32) and (33), one obtains solutions for an uncharged sphere.…”