Can a nearby supernova explain the ¹⁰Be excess in the Early Solar System?

Excess of ¹⁰Be in the meteorites has mostly been studied in the context of non-thermal, in-situ nucleosynthesis due to cosmic rays or Solar energetic particles from Sun in its early phase. Recently, a low mass core-collapse supernova has been postulated as a possible source of ¹⁰Be. However, in CCSNe a major uncertainty for the production of ¹⁰Be in CCSNe is the ¹⁰Be(p,α)⁷Li reaction rate. We will show that a newly found resonance state in ¹¹B (Er ~ 190 keV) is the single-most important state in the Gamow window which increases the reaction rate by many orders of magnitude. As the new reaction rate decreases the ¹⁰Be yield, we will show that low mass CCSN is unlikely to produce enough ¹⁰Be to explain the observed excess in meteorites. Remaining uncertainties in ¹⁰Be(p,α)⁷Li reaction rate and experimental plans to further constrain this reaction rate will be discussed.