Abstract
Evidence for the presence of short-lived radioactive isotopes when the Solar System formed is preserved in meteorites, providing insights into the conditions at the birth of our Sun. A low-mass core-collapse supernova had been postulated as a candidate for the origin of 10Be, reinforcing the idea that a supernova triggered the formation of the Solar System. We present a detailed study of the production of 10Be by the ν process in supernovae, which is very sensitive to the reaction rate of the major destruction channel, 10Be(p,α)7Li. With data from recent nuclear experiments that show the presence of a resonant state in 11B at ≈193 keV, we derive new values for the 10Be(p,α)7Li reaction rate, which are significantly higher than previous estimates. We show that, with the new 10Be(p,α)7Li reaction rate, a low-mass CCSN is unlikely to produce enough 10Be to explain the observed 10Be/9Be ratio in meteorites, even for a wide range of neutrino spectra considered in our models.
