Field theoretical model for nuclear and neutron matter. II Neutron stars
Abstract
An evaluation is made of the consequences of two novel equations of state for neutron matter for relativistic stellar configurations, in view of recent observational evidence. The equations were obtained by solving a Lagrangian general field model for nuclear interaction which contains numerous models previously considered as particular cases. The first of the two equations stems from a particular determination of the free parameters of the Serot (1979) model, and yields a satisfactory description of the saturation properties of symmetric nuclear matter and of the symmetry energy at nuclear density. The second equation is arrived at through a determination of the free parameters in the linear sigma-model having an explicit, symmetry-breaking term, and is coupled to the omega and rho mesons in a renormalizable fashion. Attention is given to the configurations generated by solutions of the general relativistic stellar structure equations, using the two equations of state; both are found to lead to equilibrium configurations that are compatible with the current status of observational evidence.