An EoS in β-equilibrium at T = 0. The core is homogeneous n, p, e matter that begins above 0.07 fm^−3. It is computed using a relativistic mean-field theory constrained by chiral effective field theory calculations of pure neutron matter (from 0.08 fm^−3 to 0.32 fm^−3) and by properties of isospin-symmetric nuclear matter around saturation density [ABHT_2022 ]. The outer crust is the Baym-Pethick-Sutherland (BPS) EoS and spans the density range 6.30 × 10^−12 fm^−3 to 2.57 × 10^−4 fm^−3 [BPSA_1971]. The inner crust is the GPPVA(TM1e) EoS, which models nuclear pasta phases calculated within a self-consistent Thomas- Fermi approach from 2.00 × 10^−3 fm^−3 to 6.24 × 10^−2 fm^−3 [GPPVP_2014]. A first-order phase transition to the core is imposed at a baryon chemical potential of 952.22 MeV.
Nuclear Matter Properties
Neutron Star Properties