Unified neutron star EOSs and neutron star structures in RMF models

In the framework of Thomas-Fermi approximation, we study systematically EOSs and microscopic structures neutron star matter in a vast density range with $n_\mathrm{b}\approx 10^{-10}$-2 $\mathrm{fm}^{-3}$, where various covariant functionals are adopted, i.e., those nonlinear self couplings (NL3, PK1, TM1, GM1, MTVTC) density-dependent (DD-LZ1, DDME-X, PKDD, DD-ME2, DD2, TW99). It is found that generally coincide each other at $n_\mathrm{b}\lesssim 10^{-4}$ fm${}^{-3}$ 0.1 fm${}^{-3}\lesssim n_\mathrm{b} \lesssim 0.3$ fm${}^{-3}$, while regions they sensitive to effective interactions between nucleons. By adopting larger slope symmetry energy $L$, curvature parameter $K_\mathrm{sym}$ drip increase, droplet size, proton number nucleus, core-crust transition density, onset non-spherical nuclei decrease. All predict stars maximum masses exceeding two-solar-mass limit, DD-LZ1, DDME-X optimum radii according observational constraints. Nevertheless, corresponding skewness coefficients $J$ much lager than expected, only MTVTC TW99 meet start-of-art constraints on $J$. More accurate measurements radius PSR J0740+6620 mass thus essential identify functional satisfies all from nuclear physics astrophysical observations. Approximate linear correlations stars' $M=1.4 M_{\odot}$ $2 M_{\odot}$, $L$ observed as well, which mainly attributed curvature-slope adopted here.