  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 v14 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.
