Neutron star calculations with the phenomenological three-nucleon force

In this work, we have studied the effect of three-nucleon interaction on the neutron stars structure. In our calculations, we have considered the neutron star matter as a beta-stable nuclear matter. We have put the results concerning the TBF effect in perspective against two-body results and other calculations of three-nucleon interactions, using the Urbana v 14 potential and the parabolic approximation of the nuclear matter energy for approximating the problem of asymmetric nuclear matter. As such, solving the Tolman–Oppenheimer–Volkoff equation, we have estimated bulk properties of neutron stars and investigated how the present calculations would agree with the expected dynamical stability condition.