Anisotropic quark stars with an interacting quark equation of state in extra dimension

This work revisits a modified version of the hydrostatic equilibrium equation in the presence of pressure anisotropy based on General Relativity with an extra dimension. We examine the structural features of quark stars in various dimensions by solving the Tolman-Oppenheimer-Volkoff (TOV) equation numerically using the interacting quark EoS. From our result, the compact star model with isotropic pressure can be obtained as alpha\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\alpha $$\end{document} approaches zero. The energy-dependent maximum mass and its associated radius, as well as the other characteristics like pressure, energy density, stability, etc., of the quark star, are obtained using the numerical solution. Through our detailed study, we have demonstrated that the conclusions we obtained here are consistent with observable evidence in four-dimensional spacetime. In four dimensions, for different values of alpha\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\alpha $$\end{document}, our obtained results can predict the mass of the compact stars PSR J0740+6620, PSR J1614-2230, Vela X-1, 4U 1608-52, 4U 1820-30, Cen X-3, and EXO 1785-248.