Study of physical properties of charged compact star model in [formula omitted] gravity

Abstract

In the realm of the torsion-dependent extended theory of gravity, we investigate the spherically symmetric and static self-gravitating structures of the anisotropic fluid. For the fluid, we assume the linear equation of state pr=αρ−β and utilize the f(T) gravity with f(T)=cT+d. Using the Tolman–Kuchowicz (TK) ansatz, for the metric functions, we find the solution of the Einstein–Maxwell field equation. The Reissner–Nordström line element is taken to describe the star’s external spacetime. For the investigation of the physical viability of the suggested model, the matching of the internal spacetime with that of external spacetime and experimentally estimated data relating to the pulsar Her X-1 have been used. The velocities of the pressure waves and the relativistic adiabatic index have both been used to examine the stability of the star. It is demonstrated that all physically relevant parameters are consistent and well-behaved. The maximum allowable mass and the corresponding radius have been obtained from our present model through the M−R plot. From our analysis, we have shown that the mass of four different compact stars found in literature namely the lighter components of GW190814 event, PSR J0952-0607, PSR J0740+6620, and PSR J1614-2230 has been achieved for four different values of α.