Some analytical models of anisotropic strange stars

Abstract

This article was published in the Astrophysics and Space Science [© Springer Science+Business Media Dordrecht 2015] and the definite version is available at : http://10.1007/s10509-015-2582-2 The Journal's website is at: http://link.springer.com/article/10.1007/s10509-015-2582-2Over the years of the concept of local isotropy has become a too stringent condition in modeling relativistic self-gravitating objects. Taking local anisotropy into consideration, in this work, some analytical models of relativistic anisotropic charged strange stars have been developed. The Einstein–Maxwell gravitational field equations have been solved with a particular form of one of the metric potentials. The radial pressure and the energy density have been assumed to follow the usual linear equation of state of strange quark matter, the MIT bag model.Publishe

On the effect of anisotropy on stellar models

“…It is required that the speed of sound is a decreasing monotonic function as a function of the radius [28]. However, this is not a generality [19,39,40], a simple example is the MIT Bag equation of state P = 1 3 (c 2 ρ − 4B g ) applicable for quarks stars, in this case the speed of sound, v 2 = c 2 /3, is constant [41]. So we will only consider the non-violation of causality, although in the Sect.…”

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.…”

New charged anisotropic compact models

“…We can compute the mass function explicitly from (7). In this case we can write the mass function in terms of x by…”

“…In this way we can model relativistic compact objects including dark energy stars, quark stars, gravastars, neutron stars and ultradense matter. For some recent models investigating the properties of charged anisotropic stars see the treatments of Feroze and Siddiqui [1], Thirukkanesh and Ragel [2], Maurya and Gupta [3], Maurya et al [4], Pandya et al [5], Bhar et al [6] and Murad [7].…”