Abstract

The light neutron-rich nuclei can be synthesized via (α,n) reactions in the so-called weak r-process. The abundances of these species are derived using reaction network calculations. Such a simulation has astrophysical and nuclear physics inputs, one of the most uncertain parameter is the α-nucleus optical potential. (α,n) cross section measurements can be used to evaluate α-optical potentials. For this purpose, the activation cross section measurement of the 100Mo(α,n)103Ru reaction is in progress at Atomki.

Highlights

  • The synthesis of the heavy elements beyond iron is dominantly driven by neutroncapture reactions [1, 2]

  • The neutron-rich nuclei between 56Fe and 109Ag can be synthesized in a neutrino-driven wind following the birth or merge of neutron stars in the weak r-process [3, 4]

  • The network relies on astrophysical inputs — such as the temperature of the astrophysical site, the timescale of the process, the initial isotopic abundances etc. — and nuclear physics inputs like the reaction rates

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Summary

Introduction

The synthesis of the heavy elements beyond iron is dominantly driven by neutroncapture reactions [1, 2]. The neutron-rich nuclei between 56Fe and 109Ag can be synthesized in a neutrino-driven wind following the birth or merge of neutron stars in the weak r-process [3, 4]. The cross sections need to be measured at low energies where the predictions, calculated using different α-OMP’s, are reasonably different. Such experiments are typically carried out using the activation technique. By carrying out a new cross section measurement using thick molybdenum targets, a more precise database can be obtained and this reaction can be used to evaluate the α-OMPs used in weak-r process calculations. The activation cross section measurement of the 100Mo(α,n)103Ru reaction in the 7.9 MeV ≤ Eα ≤ 13.0 MeV energy range is in progress at Atomki using natural isotopic composition targets

Activity measurement
Determination of the detection efficiency
Findings
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