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- W116394594 abstract "Liubin Pan, Steven Desch Evan Scannapieco, & F. X. Timmes 1 Arizona State University, School of Earth and Space Exploration, P.O. Box 871404, Tempe, AZ 85287-1404 From isotopic studies of meteorites, it is known that the early Solar System contained over a half dozen shortlived radionuclides (SLRs) such as Al and Fe, with half-lives ≈ 1 Myr [1]. The origins of these SLRs are consistent with injection of supernova material into the Solar System, either in its molecular cloud stage or into the protoplanetary disk [1]. In fact, the origin of Fe is only plausibly explained by a nearby supernova during the Sun’s origin, within the Sun’s star-forming cluster [1]. Supernovae also appear capable of contaminating forming planetary systems with stable isotopes. The oxygen isotopic abundance of the Sun, compared with field stars, suggests contamination by supernova material [2]. More important, some protostars in the Orion Ic and Id associations show overabundances of Si and O (but not C and N) compared to other stars in these associations, and especially with respect to the earlier-formed Ia and Ib associations. The pattern of overabundance strongly suggests contamination by supernova ejecta. Motivated by these observations, we have undertaken a detailed numerical study of what happens to supernova material as it interacts with nearby molecular cloud material at the periphery of a star-forming region. Our focus is to to determine the depth to which supernova material can penetrate into the molecular gas, and whether it can be incorporated into forming stars." @default.
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- W116394594 date "2010-04-01" @default.
- W116394594 modified "2023-09-27" @default.
- W116394594 title "Mixing of Supernova Ejecta into Molecular Clouds" @default.
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