Neutron stars in a Skyrme Model with Λ hyperons

In order to calculate neutron-star properties, it is necessary to have an Equation of State (EOS) linking pressure to the total energy density of the dense matter. At densities closer to the the nuclear saturation density (ρ0 = 0.17fm-3), the matter is mostly composed of neutrons, protons and leptons (electrons and muons) in β equilibrium. As density increases, new hadronic degrees of freedom may appear. Hyperons are one of them as the equilibrium conditions in neutron stars makes the formation of hyperons energetically favorable. The role of hyperons on the neutron star properties have been studied by several authors. In this paper, the best fit ΛN interactions is employed obtained to discuss the implications of hyperons on the EOS and structure of neutron stars