Free nucleon fractions (top panel), critical temperatures (middle panel), and relative effective masses (bottom panel) for the basic theoretical models used in this paper for the nonaccreted crust and the core of a neutron star. The unified generalized Skyrme model BSk24 (Pearson et al. 2019) is compared with the variational APR^* model for the core (Akmal et al. 1998), and with the SLy4 model (Douchin & Haensel 2001) for the crust EoS and composition, as well as with the results of BBST for the effective masses. For the critical temperatures T_crit of proton singlet, neutron singlet, and neutron triplet pairing types of superfluidity we employ the results of BS, MSH, and BEEHS, respectively, as parametrized by Ho et al. (2015). For comparison, by dotted lines in the middle panel we show the results of GIPSF for the neutron-singlet superfluidity in the neutron star crust, also parametrized by Ho et al. (2015), and the results of Ding et al. (2016) for the neutron-triplet superfluidity in the neutron star core, calculated with allowance for short-range correlations and polarization (SRC+P) for the effective potential models N3LO (upper dotted curves) and Av18 (lower dotted curves).