Structural properties of magnetized neutron stars under f(R,T) gravity framework

This work investigates the structural properties of neutron stars in the presence of a strong magnetic field within the framework of [Formula: see text] modified gravity, where the matter–geometry coupling leads to deviations from general relativity at high matter densities. We present here the mass–radius sequences, as well as the mass and pressure distributions for various values of the modified gravity parameter and the central magnetic field. The modified Tolman– Oppenheimer–Volkoff equations are numerically solved using isotropic equations of state, specifically the APR, FPS and SLy models. Comparing the corresponding results in the context of general relativity suggests that more negative values of the modified gravity parameter result in higher maximum gravitational masses. In contrast, strong central magnetic fields of up to [Formula: see text] [Formula: see text]Gauss cause only a slight decrease in maximum mass without disrupting spherical symmetry. Our findings are in agreement with the observed data from the surface gravitational redshift, GW170817, PSR and NICER.