Compact star modeling in f(T) gravity with gravitational decoupling

Abstract

This work examines how complexity affects time-independent, spherical symmetric celestial systems using a radial metric distortion approach (commonly referred to be minimal geometric deformation) in f(T) theory, where T is torsion scalar. We illustrate that the complexity factor, a scalar function derived by dividing the Riemann tensor perpendicularly, has a supplementary feature. The entire complexity of an entity with two associated fluid distributions is just a combination of the complexities associated with each fluid. This work uses the radial metric distortion method to create astrophysically feasible models of anisotropic matter, based on the Tolman and Buchdahl models. The two frameworks generate qualitatively equivalent features for every non-null value of the decoupling constant \((0\le \beta <1)\), while the magnitudes may differ significantly. Remarkably, both models maintain their anisotropic characteristics even after approaching the zero-complexity condition \((\beta =1)\). In conclusion, we investigate the possible accuracy of these new solution categories in representing actual compact structures by delving into their physical ramifications.