  Theoretical studies of the nucleosynthesis origin of the heavy elements in
our Solar System (S.S.) by the rapid neutron-capture process (r-process) still
face the entwined uncertainties in the possible astrophysical scenarios and the
nuclear-physics properties far from stability. In this paper we present results
from the investigation of an r-process in the high-entropy wind (HEW) of
core-collapse supernovae (here chosen as one of the possible scenarios for this
nucleosynthesis process), using new nuclear-data input calculated in a
consistent approach, for masses and $\beta$-decay properties from the new
finite-range droplet model FRDM(2012). The accuracy of the new mass model is
0.56 MeV with respect to {\sc AME2003}, to which it was adjusted. We compare
the new HEW r-process abundance pattern to the latest S.S. r-process residuals
and to our earlier calculations with the nuclear-structure quantities based on
FRDM(1992). Substantial overall and specific local improvements in the
calculated pattern of the r-process between $A\simeq 110$ and $^{209}$Bi, as
well as remaining deficiencies are discussed in terms of the underlying
spherical and deformed shell structure far from stability.
