Moment of inertia of slowly rotating anisotropic neutron stars in f(R,T) gravity

Within the framework of [Formula: see text] theories gravity, we investigate hydrostatic equilibrium anisotropic neutron stars with a physically relevant equation state (EoS) for radial pressure. In particular, focus on model, where is minimal coupling constant. slowly rotating approximation, derive modified TOV equations and expression relativistic moment inertia. The main properties stars, such as radius, mass inertia, are studied in detail. Our results reveal that consequence term substantial increase surface radius low enough central densities. Nevertheless, slightly modifies total gravitational inertia stars. Furthermore, changes noticeable when anisotropy incorporated into stellar fluid, it possible to obtain higher masses consistent current observational data.