Analytical stellar models of neutron stars in teleparallel gravity

In this paper, we use the theory of teleparallel gravity to develop three analytical models and obtain a new class of solutions describing compact stellar structures. We investigate the anisotropic nature of stellar configurations in general and solve teleparallel gravity equations. To thoroughly analyze the various parameters of the stars, we develop three models by choosing various physically acceptable forms of metric potential ed(r)\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$e^{d(r)}$$\end{document} and radial pressure pr(r)\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$p_r(r)$$\end{document}. We also analyze the impact of teleparallel gravity’s parameters β\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\beta$$\end{document} and β1\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\beta _1$$\end{document} on the description of the stellar structures. We calculated model parameters so that models describing various observed neutron stars obey all physical conditions necessary to be potentially stable and causal. By analyzing the impact of various parameters of teleparallel gravity on the description of anisotropic stellar structures, we show that these three models can describe anisotropic neutron stars ranging from low density to high density. Finally, we obtain a quadratic equation of state for each model describing various neutron stars, which can be utilized to find compositions of the stellar structures. It is extremely useful to find models that can exhibit quadratic EOS, because various authors have discovered that the material compositions of real neutron stars and strange stars exhibit quadratic EOS. Since a nonlinear f(T) model gives a high deviation of EOS from the quadratic behavior, we work with a linear f(T) function by using a diagonal tetrad to model realistic compact stars.