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.
Bibliographical noteFunding Information:
We acknowledge useful discussions with Camilla J. Hansen, Maria Lugaro, Marco Pignatari, and Claudia Travaglio. We thank an anonymous referee for a detailed and constructive report that helped improve the paper. This work was supported in part by the Helmholtz-University Young Investigator grant No. VH-NG-825, Deutsche Forschungsgemeinschaft through SFB 1245, BMBF under grant No. 05P15RDFN1, ERC 677912 EUROPIUM, and the US DOE grant DE-FG02-87ER40328.
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- nuclear reactions, nucleosynthesis, abundances
- supernovae: general