Properties and microscopic structures of dense stellar matter in RMF models

Data tables on the equation of state (EOS) and microscopic structures for cold dense stellar matter with proton fractions Yₚ =0.01-$0.65$ and baryon number densities nb=10⁻⁸-2 \ fm⁻³ are obtained adopting 13 different relativistic density functionals, i.e., NL3, PK1, PK1r, GM1, MTVTC, DD-LZ1, PKDD, DD-ME2, TW99, DD-MEX, DD-MEX1, DD-MEX2, and DD-MEY. The EOSs of dense stellar matter inside neutron stars with baryon number densities nb=7.6× 10⁻¹¹-2 \ fm⁻³ are obtained as well fulfilling $β$-stability condition. In general, the dense stellar matter exhibits droplet phase at nb 0.015\ fm⁻³, while more exotic structures such as rods, slabs, tubes, and bubbles appear sequentially as density increases. The critical proton fractions Yₚᵈrip (≈ 0.26-0.31) for neutron drip are obtained, where neutron gas emerges outside of nuclei at Yₚ< Yₚᵈrip. For dense stellar matter at small densities (nb 10⁻⁵ \ fm⁻³) or large proton fractions (nb0.1 \ fm⁻³ and Yₚ Yₚᵈrip), the EOSs and microscopic structures are generally insensitive to the adopted density functionals. With the onset of neutron drip at Yₚ Yₚᵈrip, the uncertainties emerge and peak at nb ≈ 0.02 \ fm⁻³ within the range 10⁻⁵ nb0.1 \ fm⁻³. At nb0.1 \ fm⁻³, the dense stellar matter becomes uniform and muons eventually appear, where the uncertainties in the EOSs grow significantly.