Neutron stars in f (R, Lm, T) gravity

This study explores the behavior of compact stars within the framework of f(R,L-m,T) gravity, focusing on the functional form f(R,L-m,T)=R+alpha TLm. The modified Tolman-Oppenheimer-Volkoff (TOV) equations are derived and numerically solved for several values of the free parameter alpha by considering both quark and hadronic matter-described by realistic equations of state (EoSs). Furthermore, the stellar structure equations are adapted for two different choices of the matter Lagrangian density (namely, L-m=p and and L-m=-rho), laying the groundwork for our numerical analysis. As expected, we recover the traditional TOV equations in General Relativity (GR) when alpha -> 0. Remarkably, we found that the two choices for L-m have appreciably different effects on the mass-radius diagrams. Results showcase the impact of alpha on compact star properties, while final remarks summarize key findings and discuss implications, including compatibility with observational data from NGC 6397's neutron star. Overall, this research enhances comprehension of f(R,L-m,T) gravity's effects on compact star internal structures, offering insights for future investigations.