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Theoretical studies of the nucleosynthesis origin of the heavy elements inour Solar System (S.S.) by the rapid neutron-capture process (r-process) stillface the entwined uncertainties in the possible astrophysical scenarios and thenuclear-physics properties far from stability. In this paper we present resultsfrom the investigation of an r-process in the high-entropy wind (HEW) ofcore-collapse supernovae (here chosen as one of the possible scenarios for thisnucleosynthesis process), using new nuclear-data input calculated in aconsistent approach, for masses and $\beta$-decay properties from the newfinite-range droplet model FRDM(2012). The accuracy of the new mass model is0.56 MeV with respect to {\sc AME2003}, to which it was adjusted. We comparethe new HEW r-process abundance pattern to the latest S.S. r-process residualsand to our earlier calculations with the nuclear-structure quantities based onFRDM(1992). Substantial overall and specific local improvements in thecalculated pattern of the r-process between $A\simeq 110$ and $^{209}$Bi, aswell as remaining deficiencies are discussed in terms of the underlyingspherical and deformed shell structure far from stability.

A high-entropy wind r-process study based on nuclear-structure quantities from the new finite-range droplet model FRDM(2012)