Abstract
The propagation of uncertainties in reaction cross sections and rates of neutron-, proton-, and α-induced reactions into the final isotopic abundances obtained in nucleosynthesis models is an important issue in studies of nucleosynthesis and Galactic Chemical Evolution. We developed a Monte Carlo method to allow large-scale postprocessing studies of the impact of nuclear uncertainties on nucleosynthesis. Temperature-dependent rate uncertainties combining realistic experimental and theoretical uncertainties are used. From detailed statistical analyses uncertainties in the final abundances are derived as probability density distributions. Furthermore, based on rate and abundance correlations an automated procedure identifies the most important reactions in complex flow patterns from superposition of many zones or tracers. The method already has been applied to a number of nucleosynthesis processes.
Highlights
Low-energy reaction cross sections with light projectiles are required to determine astrophysical reaction rates and to constrain the production of nuclides in various astrophysical environments
Our studies address an important question in the context of astrophysical applications: how uncertainties in cross sections of reactions induced by neutrons, protons, and α-particles propagate into the final isotopic abundances obtained in nucleosynthesis models
This information is important for astronomers to interpret their observational data, for groups studying the enrichment of the Galaxy over time with heavy elements, and in general for disentangling uncertainties in nuclear physics from those in the astrophysical modelling
Summary
Low-energy reaction cross sections with light projectiles are required to determine astrophysical reaction rates and to constrain the production of nuclides in various astrophysical environments. Our studies address an important question in the context of astrophysical applications: how uncertainties in cross sections of reactions induced by neutrons, protons, and α-particles propagate into the final isotopic abundances obtained in nucleosynthesis models This information is important for astronomers to interpret their observational data, for groups studying the enrichment of the Galaxy over time with heavy elements, and in general for disentangling uncertainties in nuclear physics from those in the astrophysical modelling. The stellar reactivity includes a sum over reactions proceeding on excited states (starting from the ground state with μ = 0), R∗ = This means that projectiles with Maxwell-Boltzmann distributed energies are acting on each level μ separately. This can be seen more when explicitly inserting the population coefficient, leading to [1, 2]
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