In this paper, we utilize the Brueckner-Hartree-Fock (BHF) method to compute the static properties of neutron stars (NS) at zero temperature. We specifically apply a microscopic equation of state for pure neutron matter (PNM). Three-body forces have also been included at different densities. To accurately replicate the nuclear matter saturation point, we have incorporated recent and realistic two-body nuclear interactions. Specifically, we have used the Argonne V18 and CD-Bonn NN potentials, integrated via the Urbana model, to account for the three-body force. We have calculated the properties of neutron stars by numerically solving the Tolman-Oppenheimer-Volkov structure equations. Our results indicate a maximum mass configuration of M = 1.7 ± 0.05 Mʘ (M = 2.12 ± 0.04 Mʘ) when using CD-Bonn (Argonne 18) interaction, respectively. These values are consistent with the observed range of neutron star masses. Furthermore, we have discussed the sensitivity of using modern NN potentials and compared our results with other theoretical predictions and observed data.