Neutron Stars in the Context of f (T, T) Gravity

In this work, we investigate the existence of neutron stars (NS) in the framework of f (T, T) gravity, where T is the torsion tensor and T is the trace of the energy-momentum tensor. The hydrostatic equilibrium equations are obtained, however, with p and rho quantities passed on by effective quantities (rho) over bar and (rho) over bar, whose mass-radius diagrams are obtained using modern equations of state (EoS) of nuclear matter derived from relativistic mean field models and compared with the ones computed by the Tolman-Oppenheimer-Volkoff (TOV) equations. Substantial changes in the mass-radius profiles of NS are obtained even for small changes in the free parameter of this modified theory. The results indicate that the use of f (T, T) gravity in the study of NS provides good results for the masses and radii of some important astrophysical objects, as, for example, the NS of low-mass X-ray binary in NGC 6397, the millisecond pulsar PSR J0740+6620 and the GW170817 event. In addition, radii results inferred from the Lead Radius Experiment (PREX-2) can also be described for certain parameter values.