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- W148931315 abstract "Iron‐60 decays to 60Ni with a half‐life of 1.49 million years (Myr). Because 60Fe is produced only in stars, its initial abundance in the solar system provides a constraint on the stellar contribution of radionuclides to the solar system and on the nature of the stellar source. The initial abundance of 60Fe in the solar system has been only loosely constrained from sulfides, of which 60Fe‐60Ni systems are easily disturbed, in primitive chondrites. In this study, we show that 60Fe was present in chondrules, silicate spherules commonly found in chondrites, with initial 60Fe/56Fe ratios ((60Fe/56Fe)0) of (2.2–3.7) × 10−7 at the time of their formation. By applying the time difference of 1.5–2.0 Myr between formation of the oldest known solar‐system solids (Ca‐Al‐rich inclusions) and chondrules, a (60Fe/56Fe)0 ratio for the initial solar system of (5–10) × 10−7 is estimated. This new solidly based (60Fe/56Fe)0 ratio is consistent with predictions for nucleosynthesis in a supernova or in an intermediate‐mass AGB star just before the solar‐system formation, but too high for the source to have been a low‐mass AGB star. Because encounters between a molecular cloud and an AGB star are rare, our results appear to be the best evidence found to date for a contribution of material from a nearby supernova to the solar system." @default.
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- W148931315 date "2006-01-01" @default.
- W148931315 modified "2023-09-25" @default.
- W148931315 title "The Abundance Of Live 60Fe In The Early Solar System" @default.
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- W148931315 doi "https://doi.org/10.1063/1.2234417" @default.
- W148931315 hasPublicationYear "2006" @default.
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