Data tables on the equation of state (EOS) and microscopic structures for cold dense stellar matter with proton fractions $Y_p =0.01$-$0.65$ and baryon number densities $n_\text{ b}=10^{ -8}$-$2 \ \mathrm{ fm}^{ -3}$ 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 $n_\text{ b}=7.6\times 10^{ -11}$-$2 \ \mathrm{ fm}^{ -3}$ are obtained as well fulfilling $\beta$-stability condition. In general, the dense stellar matter exhibits droplet phase at $n_\mathrm{ b}\lesssim 0.015\ \mathrm{ fm}^{ -3}$, while more exotic structures such as rods, slabs, tubes, and bubbles appear sequentially as density increases. The critical proton fractions $Y_p^\mathrm{ drip}$ ($\approx 0.26$-0.31) for neutron drip are obtained, where neutron gas emerges outside of nuclei at $Y_p< Y_p^\mathrm{ drip}$. For dense stellar matter at small densities ($n_\text{ b}\lesssim 10^{ -5} \ \mathrm{ fm}^{ -3}$) or large proton fractions ($n_\text{ b}\lesssim0.1 \ \mathrm{ fm}^{ -3}$ and $Y_p\gtrsim Y_p^\mathrm{ drip}$), the EOSs and microscopic structures are generally insensitive to the adopted density functionals. With the onset of neutron drip at $Y_p\lesssim Y_p^\mathrm{ drip}$, the uncertainties emerge and peak at $n_\text{ b} \approx 0.02 \ \mathrm{ fm}^{ -3}$ within the range $10^{ -5} \lesssim n_\text{ b}\lesssim0.1 \ \mathrm{ fm}^{ -3}$. At $n_\text{ b}\gtrsim0.1 \ \mathrm{ fm}^{ -3}$, the dense stellar matter becomes uniform and muons eventually appear, where the uncertainties in the EOSs grow significantly.
Categories: astro-ph.HE nucl-th