Compact objects in f(R, T) gravity with Finch–Skea geometry

We obtain a class of anisotropic spherically symmetric relativistic solutions of compact objects in hydrostatic equilibrium in the f(R,T)=R+2χT\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$f(R,T) =R+2\chi T$$\end{document} modified gravity, where R is the Ricci scalar, T is the trace of the energy momentum tensor and χ\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\chi $$\end{document} is a dimensionless coupling parameter. The relativistic solutions are employed to obtain realistic stellar models for compact stars, and the physical quantities, energy density, anisotropy parameter, radial and tangential pressures and TOV equations are studied numerically for different model parameters. We construct anisotropic stellar models with modified Finch–Skea ansatz in the f(R, T)-theory of gravity for known mass and radius which obey all the conditions for a physically realistic star. The equation of state for the interior matter is also predicted which is of the form p=f(ρ)\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$p= f(\rho )$$\end{document}. The stellar models satisfy causality conditions, and the adiabatic index is examined.