Speaker
Description
Using a consistent statistical approach through the Backward-Forward Monte-Carlo method, we investigate both the parameter (statistic) and model (systematic) uncertainties associated with theoretical nuclear reaction rates of relevance during the i-process, and with theoretical nuclear masses of relevance during the r-process.
- For the i-process, we explore the impact on the i-process elemental production, and subsequently on the surface enrichment, for low-mass low-metallicity stars during the early AGB phase.
- For the r-process, we show the impact on the r-process production during Neutron Star Merger events.
These studies allow us to quantify the relative importance of parameters versus model uncertainties with respect to the surface abundances in AGB stars and to the r-process production during Neutron Star mergers.
We identify and provide a list of important reaction rates that would need to be better constrained in the future in order to improve our understanding of the i-process. We identify similarly important nuclear masses in the r-process production.
