Spherically symmetric charged compact stars

Abstract

In this article we consider the static spherically symmetric metric of embedding class 1. When solving the Einstein-Maxwell field equations we take into account the presence of ordinary baryonic matter together with the electric charge. Specific new charged stellar models are obtained where the solutions are entirely dependent on the electromagnetic field, such that the physical parameters, like density, pressure etc. do vanish for the vanishing charge. We systematically analyze altogether the three sets of Solutions I, II, and III of the stellar models for a suitable functional relation of ν(r ). However, it is observed that only the Solution I provides a physically valid and well-behaved situation, whereas the Solutions II and III are not well behaved and hence not included in the study. Thereafter it is exclusively shown that the Solution I can pass through several standard physical tests performed by us. To validate the solution set presented here a comparison has also been made with that of the compact stars, like R X J 1856 − 37, Her X − 1, P S R 1937 + 21, P S R J 1614 − 2230, and P S R J 0348 + 0432, and we have shown the feasibility of the models.

Generalised model for anisotropic compact stars

“…We find from Table 2 that, for n ≥ 10, the product n A becomes almost a constant (say C). Thus we can conclude that for large values of n (say infinity) we have the metric potential ν = Cr 2 + ln B as considered by Maurya et al [22,27] in the literature. This result therefore helps us in turn to explore the behaviour of the mass and radius of the spherical stellar system as can be observed from Fig.…”

Anisotropic fluid spheres of embedding class one using Karmarkar condition

“…Due to this relation, we can convert all the differential equations in terms of one of the metric coefficients (the full details can be seen in the references by Maurya et al [36,37]). For this purpose we have assumed a totally new metric potential e λ = [1 + 2c r 2 + cosh 2(ar 2 +b)]/[1 + cosh 2(ar 2 +b)] to find the anisotropic solution for realistic fluid spheres.…”

A new solution of embedding class I representing anisotropic fluid sphere in general relativity

“…28 . Many articles have also discussed on embedding class I solutions that can represent compact stars [37][38][39] . The aim of this paper is to generate a new model of anisotropic relativistic anisotropic star satisfying the Karmakar's 29 condition.…”