Anisotropic strange stars in f(R,𝒯) gravity: A conformal killing vector approach to stability and observational signatures

This study investigates anisotropic compact star configurations within the framework of [Formula: see text] gravity, employing a conformal Killing vector approach to model ultra-dense strange quark stars. Adopting the MIT bag equation of state (EOS) for strange quark matter (SQM) and a linear relation between tangential pressure and energy density, we derive exact solutions to the Einstein field equations under the modified gravity formalism. Key parameters, including the coupling constant [Formula: see text], bag constant B and anisotropy coefficient [Formula: see text], are analyzed for the representative candidate [Formula: see text]. Our results confirm the absence of geometric singularities, with metric potentials exhibiting regular behavior. Effective energy density, radial pressure and tangential pressure peak at the stellar center and decline monotonically toward the surface, while anisotropy increases radially, reaching maxima at the boundary. The model satisfies all energy conditions and adheres to the Buchdahl limit. Mass–radius relations reveal proportional increases in total mass M and radius R with rising [Formula: see text], contrasting general relativity (GR) predictions. Stability analyses via the modified Tolman–Oppenheimer–Volkoff (TOV) equation demonstrate equilibrium through force balance, with an emergent repulsive force [Formula: see text] attributed to matter-geometry coupling. Stability is further validated by Herrera’s cracking criterion and adiabatic indices. Surface redshift decreases with [Formula: see text], while compactification factors remain consistent with ultra-dense characteristics. Tabulated results highlight decreasing central density, surface density and compactness ([Formula: see text]) with increasing [Formula: see text]. This work establishes a robust, singularity-free anisotropic stellar model in [Formula: see text] gravity, offering insights into the interplay of modified gravity, anisotropy and quark matter in describing compact astrophysical objects.