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 Be10, reinforcing the idea that a supernova triggered the formation of the Solar System. We present a detailed study of the production of Be10 by the ν process in supernovae, which is very sensitive to the reaction rate of the major destruction channel, Be10(p,α)7Li. With data from recent nuclear experiments that show the presence of a resonant state in B11 at ≈193 keV, we derive new values for the Be10(p,α)7Li reaction rate, which are significantly higher than previous estimates. We show that, with the new Be10(p,α)7Li reaction rate, a low-mass CCSN is unlikely to produce enough Be10 to explain the observed Be10/Be9 ratio in meteorites, even for a wide range of neutrino spectra considered in our models.
| Original language | English |
|---|---|
| Article number | 015803 |
| Journal | Physical Review C |
| Volume | 106 |
| Issue number | 1 |
| DOIs | |
| State | Published - Jul 2022 |
Funding
This work was supported by the U.S. Department of Energy, Office of Science, Office of Nuclear Physics and Office of Advanced Scientific Computing Research, Scientific Discovery through Advanced Computing (SciDAC) program. Research at Oak Ridge National Laboratory is supported under contract DE-AC05-00OR22725 from the U.S. Department of Energy to UT-Battelle, LLC. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231 using NERSC award NP-ERCAP0020269. J.S.R., R.J.D., and T.A. were supported by National Science Foundation through Grant No. Phys-2011890. R.J.D. utilized resources from the Notre Dame Center for Research Computing and was supported by the Joint Institute for Nuclear Astrophysics through Grant No. PHY-1430152 (JINA Center for the Evolution of the Elements). R.M. and G.M.-P. acknowledge the support of the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) – Project-ID 279384907 – SFB 1245 “Nuclei: From Fundamental Interactions to Structure and Stars”. This research made extensive use of numpy , matplotlib , and of the SAO/NASA Astrophysics Data System (ADS).