Pure Neutron Matter Constraints and Nuclear Symmetry Energy

Abstract

In this review, we will discuss the results of our recent work to study the general optimization of the pure isovector parameters of the popular relativistic mean-field (RMF) and Skyrme-Hartree-Fock (SHF) nuclear energy-density functionals (EDFs), using constraints on the pure neutron matter (PNM) equation of state (EoS) from recent {\sl ab initio} calculations. By using RMF and SHF parameterizations that give equivalent predictions for ground-state properties of doubly magic nuclei and properties of symmetric nuclear matter (SNM) and PNM, we found that such optimization leads to broadly consistent symmetry energy $J$ and its slope parameter $L$ at saturation density within a tight range of $\sigma (J)<2$ MeV and $\sigma (L)<6$ MeV. We demonstrate that a clear model dependence shows up (a) in the curvature parameter of the symmetry energy $K_{\mathrm{sym}}$, (b) the symmetry energy at supra-saturation densities, and (c) the radius of neutron stars.

arXiv commentTalk given at the 11th International Conference on Nucleus-Nucleus Collisions (NN2012), San Antonio, Texas, USA, May 27-June 1, 2012. To appear in the NN2012 Proceedings in Journal of Physics: Conference Series (JPCS)

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Cited by in corpus (4)

• Energy density functional for nuclei and neutron stars
• Effects of the liquid-gas phase transition and cluster formation on the symmetry energy
• Diversities in the properties of neutron stars at a fixed neutron-skin thickness in ${}^{208}$Pb nucleus
• The EOS of neutron matter and the effect of $\Lambda$ hyperons to neutron star structure