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Evidence for a Single Stellar Environment of R-Process Nucelosynthesis from Live ^(247)Cm in the Early Solar System

Tissot, F. L. H. and Dauphas, N. and Grossman, L. (2016) Evidence for a Single Stellar Environment of R-Process Nucelosynthesis from Live ^(247)Cm in the Early Solar System. In: 47th Lunar and Planetary Science Conference, March 21-25, 2016, The Woodlands, TX.

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The Early Solar System (ESS) abundance of short-lived radionuclides (SLR) can be interpreted in terms of a free-decay interval (Δ) or a mixing timescale (τ), which correspond to complete or partial isolation from fresh nucleosynthetic inputs of the molecular could core parental to the solar system. For r-nuclides, however, the abundances measured in ESS materials require less isolation for ^(107)Pd and ^(182)Hf (Δ~ 5 Myr) than for ^(129)I (Δ=100±7 Myr) and ^(244)Pu (Δ=158±85 Myr) [1]. To make sense of these observations, models have proposed the existence of up to three different r-processes producing, respectively, the light r-nuclides, the heavy r-nuclides and the actinides [1-4]. In this work [5], we determined the ESS abundance of another short-lived r-nuclide, the long sought after ^(247)Cm [e.g., 6-7], and show how this additional constraint is consistent with either three different r-processes, or, and more likely, a single stellar environment of r-process nucleosynthesis and a partial s-process origin for ^(107)Pd and ^(182)Hf.

Item Type:Conference or Workshop Item (Paper)
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URLURL TypeDescription Website
Tissot, F. L. H.0000-0001-6622-2907
Dauphas, N.0000-0002-1330-2038
Additional Information:© 2016 Lunar and Planetary Institute.
Record Number:CaltechAUTHORS:20180618-110835845
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:87191
Deposited By: Tony Diaz
Deposited On:18 Jun 2018 20:34
Last Modified:09 Mar 2020 13:18

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