J. Bliss¹, A. Arcones^1,2, and Y.-Z. Qian^3,4
Astrophysical Journal 866, 105 Link to Article [DOI: 10.3847/1538-4357/aade8d]
¹Institut für Kernphysik, Technische Universität Darmstadt, Schlossgartenstr. 2, Darmstadt D-64289, Germany
²GSI Helmholtzzentrum für Schwerionenforschung GmbH, Planckstr. 1, Darmstadt D-64291, Germany
³School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA
⁴Tsung-Dao Lee Institute, Shanghai 200240, People’s Republic of China

The origin of the so-called p-isotopes and in the solar system remains a mystery, as several astrophysical scenarios fail to account for them. In addition, data on presolar silicon carbide grains of type X (SiC X) exhibit peculiar Mo patterns, especially for . We examine the production of Mo and Ru isotopes in neutrino-driven winds associated with core-collapse supernovae (CCSNe) over a wide range of conditions. We find that proton-rich winds can make dominant contributions to the solar abundance of and significant contributions to those of ⁹⁶Ru, ⁹²Mo, and ⁹⁴Mo. In contrast, neutron-rich winds make negligible contributions to the solar abundances of ^92,94Mo and cannot produce ^96,98Ru, whereas the early ejecta of CCSNe can make dominant contributions to the solar abundance of ⁹²Mo. Furthermore, we show that some neutron-rich winds can account for the peculiar Mo patterns in SiC X grains. Our results can be generalized if conditions similar to those studied here are also obtained for other types of ejecta in either CCSNe or neutron star mergers.