Aspects of anisotropic dark matter stars in f(R,T) gravity

We study the structure and stability of compact stars that have a polytropic equation of state with anisotropic pressure in the context of [Formula: see text] gravity theory. Assuming a quasi-local relationship, we quantify the anisotropy characteristics inherent in the star. In light of this premise, we derive the modified Tolman–Oppenheimer–Volkoff (TOV) equations for [Formula: see text], and integrate them for a wide range of values of the parameters involved. Here, we attempt to see how the relationships among stellar mass, radius and compactness are influenced by various model parameters. Our investigation incorporates various stability criteria, such as the static stability condition, adiabatic indices and the causality of sound speed, thereby emphasizing the dynamic characteristics of these stellar objects. The results show that the framework of [Formula: see text] gravity makes it possible for stars to be more massive and stable than those predicted by GR.