Constraining nucleosynthesis in neutrino-driven winds: observations, simulations and nuclear physics

Abstract

A promising astrophysical site to produce the lighter heavy elements of the first $r$-process peak ($Z=38-47$) is the moderately neutron rich ($0.4<Y_e<0.5$) neutrino-driven ejecta of explosive environments, such as core-collapse supernovae and neutron star mergers, where the weak $r$-process operates. This nucleosynthesis exhibits uncertainties from the absence of experimental data from $(\alpha ,xn)$ reactions on neutron-rich nuclei, which are currently based on statistical model estimates. In this work, we report on a new study of the nuclear reaction impact using a Monte Carlo approach and improved $(\alpha ,xn)$ rates based on the Atomki-V2 $\alpha$ Optical Model Potential ($\alpha$OMP). We compare our results with observations from an up-to-date list of metal-poor stars with [Fe/H] $<$ -1.5 to find conditions of the neutrino-driven wind where the lighter heavy elements can be synthesized. We identified a list of $(\alpha ,xn)$ reaction rates that affect key elemental ratios in different astrophysical conditions. Our study aims on motivating more nuclear physics experiments on $(\alpha ,xn)$ reactions using current and the new generation of radioactive beam facilities and also more observational studies of metal-poor stars.

arXiv comment16 pages, 8 figures, submitted to ApJ

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