Stable and self-consistent compact star models in teleparallel gravity

In the framework of Teleparallel Gravity, we derive a charged non-vacuum solution for a physically symmetric tetrad fieldwith two unknown functions of radial coordinate. The field equations result in a closed-form adopting particular metric potentials and a suitable anisotropy function combined with the charge. Under these circumstances, it is possible to obtain a set of configurations compatible with observed pulsars. Specifically, boundary conditions for the interior spacetime are applied to the exterior Reissner-Nordstrom metric to constrain the radial pressure that has to vanish through the boundary. Starting from these considerations, we are able to fix the model parameters. The pulsar PSR J 1614-2230, with estimated mass M = 1.97 +/- 0.04 M-circle dot, and radius R = 9.69 +/- 0.2 km is used to test numerically the model. The stability is studied, through the causality conditions and adiabatic index, adopting the Tolman-Oppenheimer-Volkov equation. The massradius (M, R) relation is derived. Furthermore, the compatibility of themodel with other observed pulsars is also studied. We reasonably conclude that themodel can represent realistic compact objects.