First measurement of 87Rb({\alpha}, xn) cross sections at weak r-process energies in supernova {\nu}-driven ejecta to investigate elemental abundances in low-metallicity stars

TL;DR

This study reports the first measurement of 87Rb({}, xn) reaction cross sections at energies relevant to the weak r-process in supernova ejecta, aiming to improve nuclear physics inputs for stellar nucleosynthesis models.

Contribution

It provides the first experimental cross section data for 87Rb({}, xn) reactions at weak r-process energies, reducing uncertainties in nuclear reaction rates used in astrophysical models.

Findings

Measured cross sections agree with statistical model estimates using Atomki-V2 -OMP.

Re-evaluated reaction rates were incorporated into nucleosynthesis calculations.

Conditions in -driven ejecta still fail to reproduce observed elemental abundances.

Abstract

Observed abundances of Z ~ 40 elements in metal-poor stars vary from star to star, indicating that the rapid and slow neutron capture processes may not contribute alone to the synthesis of elements beyond iron. The weak r-process was proposed to produce Z ~ 40 elements in a subset of old stars. Thought to occur in the {\nu}-driven ejecta of a core-collapse supernova, ({\alpha}, xn) reactions would drive the nuclear flow toward heavier masses at T = 2-5 GK. However, current comparisons between modelled and observed yields do not bring satisfactory insights into the stellar environment, mainly due to the uncertainties of the nuclear physics inputs where the dispersion in a given reaction rate often exceeds one order of magnitude. Involved rates are calculated with the statistical model where the choice of an {\alpha}-optical-model potential ({\alpha}OMP) leads to such a poor precision. The first experiment on 87Rb({\alpha}, xn) reactions at weak r-process energies is reported here. Total inclusive cross sections were assessed at Ec.m. = 8.1 - 13 MeV (3.7 - 7.6 GK) with the active target MUlti-Sampling Ionization Chamber (MUSIC). With a N = 50 seed nucleus, the measured values agree with statistical model estimates using the {\alpha}OMP Atomki-V2. A re-evaluated reaction rate was incorporated into new nucleosynthesis calculations, focusing on {\nu}-driven ejecta conditions known to be sensitive to this specific rate. These conditions were found to fail to reproduce the lighter-heavy element abundances in metal-poor stars.