Relativistic model for anisotropic compact stars using Karmarkar condition

In this work we have obtained some families of relativistic anisotropic compact stars by solving of Einstein’s field equations. The field equations have been solved by suitable particular choice of the metric potential eλ\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$e^{\lambda }$\end{document} and embedding class one condition. The physical analysis of this model indicates that the obtained relativistic stellar structure for anisotropic matter distribution is physically reasonable model for compact star whose energy density of the order 1015g/cm3\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$10^{15}~\mbox{g}/\mbox{cm}^{3}$\end{document}. Using the Tolman-Oppenheimer-Volkoff equations, we explore the hydrostatic equilibrium and the stability of the compact stars like PSR J1614-2230, 4U 1608-52, SAX J1808.4-3658, LMC X-4, RX J1856-37, Vela X-1, 4U 1820-30, EXO 1785-248, PSR J1903+327, 4U 1538-52, SMC X-1, Her X-1 and Cen X-3. We also estimated the mass and radius of such compact stars.