Neutron star calculations with the phenomenological three-nucleon force

TL;DR

This paper investigates how three-nucleon forces influence neutron star structure by modeling beta-stable nuclear matter and solving the TOV equation, providing insights into the effects of three-body interactions on neutron star properties.

Contribution

It introduces a detailed analysis of three-nucleon interactions' impact on neutron star structure using the Urbana v14 potential and compares results with two-body models.

Findings

Three-nucleon forces significantly affect neutron star bulk properties.

Results align with dynamical stability conditions.

Comparison with other models highlights the importance of three-body interactions.

Abstract

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.