Compact stellar model in the presence of pressure anisotropy in modified Finch Skea space–time

A new model of an anisotropic compact star is obtained in our present paper by assuming the pressure anisotropy. The proposed model is singularity free. The model is obtained by considering a physically reasonable choice for the metric potential grr\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$g_{rr}$$\end{document}, which depends on a dimensionless parameter n. The effect of n is discussed numerically, analytically, and through plotting. We have concentrated a wide range for n (10≤n≤1000\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$10\le n \le 1000$$\end{document}) for drawing the profiles of different physical parameters. The maximum allowable mass for different values of n has been obtained by the M–R plot. We have checked that the stability of the model is increased for a larger value of n. For the viability of the model, we have considered two compact stars PSR J1614-2230 and EXO 1785-248. We have shown that the expressions for the anisotropy factor and the metric component may serve as generating functions for uncharged stellar models in the context of general theory of relativity.