Dependence of the Results of Nucleosynthesis on the Equation of State for Neutron-Star Matter

The results of calculations of nucleosynthesis of heavy elements during the explosion of a low-mass neutron star are presented. The low-mass neutron star is formed as a result of the exchange of matter in the last stages of the evolution of a close binary system of neutron stars with a large initial mass asymmetry. Two variants of the scenario, which use different approximations of the equation of state of neutron star matter: BSk22 and BSk25, are considered. Their usage lead to different expansion dynamics of the shells of a low-mass neutron star. It is shown that the character of shock wave propagation and the abundance of heavy elements formed in the inner layers of the outer crust with for these two scenarios are different, although the composition of the outer crust before the explosion differs insignificantly. These differences in the scenarios result in a noticeable difference in the calculated abundances of heavy elements both in these layers and in the entire examined part of the outer crust.