Study of self-bound compact stars in $$f(\mathscr {T})$$ gravity and observational constraints on the model parameters

Abstract

AbstractThe present study is based on $$f(\mathscr {T})$$ f ( T ) gravity, where we impose possible observational constraints on the model parameters to obtain physically plausible features of compact stars, specifically neutron stars. To do so, as a first step, we consider the field equations in the $$f(\mathscr {T})$$ f ( T ) gravity framework. We then solve the field equations to generate a set of new exact solutions in $$f(\mathscr {T})$$ f ( T ) gravity where model parameters are found by using boundary conditions. A few tests are performed to asses the stability of the model and compare the obtained results with observations of compact stars, in particular with the compact binary merger event GW190814. We observe the maximum mass of the star beyond the $$3M_{\odot }$$ 3 M ⊙ when the surface density is of the order $$10^{14}$$ 10 14 gm/cm$$^3$$ 3 for the higher torsion parameter, which implies that an anisotropic solution in teleparallel gravity is more suitable for modeling of massive compact objects in lower $$mass-gap$$ m a s s - g a p , and thus the model presented herein provides a satisfactory physical scenario with respect to the observational signature.