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

TL;DR

This study investigates the r-process nucleosynthesis in high-entropy winds of supernovae using new nuclear data from the FRDM(2012) model, leading to improved abundance pattern predictions compared to previous models.

Contribution

It introduces a consistent approach using the FRDM(2012) model for nuclear masses and decay properties in r-process simulations, enhancing the accuracy of abundance predictions.

Findings

Improved agreement with Solar System r-process residuals between A≈110 and Bi209.

Substantial local improvements over previous models in specific mass regions.

Remaining deficiencies linked to nuclear shell structure far from stability.

Abstract

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.