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

TL;DR

This paper investigates how uncertainties in nuclear reaction rates affect the synthesis of lighter heavy elements in neutrino-driven winds of explosive astrophysical events, using simulations and observations to identify key reactions and motivate future experiments.

Contribution

It introduces a Monte Carlo approach with improved reaction rates to analyze nucleosynthesis in neutrino-driven winds, highlighting reactions that influence elemental ratios and guiding future nuclear physics experiments.

Findings

Identified key $(eta,xn)$ reactions affecting elemental ratios.

Compared nucleosynthesis predictions with metal-poor star observations.

Motivated experimental efforts on $(eta,xn)$ reactions with radioactive beams.

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.