Based on a 3D supernova simulation of an 11.8 M o progenitor model with an initial solar composition, we study the nucleosynthesis using tracers covering the innermost 0.1 M o of the ejecta. These ejecta are mostly proton-rich and contribute significant amounts of 45Sc and 64Zn. The production of heavier isotopes is sensitive to the electron fraction and hence the neutrino emission from the proto-neutron star. The yields of these isotopes are rather uncertain due to the approximate neutrino transport used in the simulation. In order to obtain the total yields for the whole supernova, we combine the results from the tracers with those for the outer layers from a suitable 1D model. Using the yields of short-lived radionuclides (SLRs), we explore the possibility that an 11.8 M o supernova might have triggered the formation of the solar system and provided some of the SLRs measured in meteorites. In particular, we discuss two new scenarios that can account for at least the data on 41Ca, 53Mn, and 60Fe without exceeding those on the other SLRs.
Bibliographical notePublisher Copyright:
© 2020. The American Astronomical Society. All rights reserved..
- Abundance ratios (11)
- Chemical abundances (224)
- Core-collapse supernovae (304)
- Explosive nucleosynthesis (503)
- Isotopic abundances (867)
- Nuclear abundances (1128)
- Nucleosynthesis (1131)
- Supernova dynamics (1664)
- Supernova neutrinos (1666)