New ab initio constrained extended Skyrme equations of state for simulations of neutron stars, supernovae, and binary mergers - I. Subsaturation density domain

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Fig. 11.

Mass fraction of unbound nucleons (bottom panels) and their proton fraction (top panels) as functions of baryonic particle density for the cases considered in Fig. 7. We note that the X-range is not the same as in Fig. 7.

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