Nucleosynthetic osmium isotope anomalies in acid leachates of the Murchison meteorite |
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| Authors: | L Reisberg N Dauphas A Luguet DG Pearson R Gallino C Zimmermann |
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| Institution: | 1. Centre de Recherches Pétrographiques et Géochimiques (CRPG), Nancy Université, CNRS, BP 20, 54501 Vandoeuvre-lès-Nancy cedex, France;2. Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, 5734 South Ellis Ave., Chicago, IL 60637, USA;3. Department of Earth Sciences, University of Durham, Durham DH1 3LE, UK;4. Mineralogisch-Petrologisches Institut, Bonn Universitat, Poppelsdorfer Schloss, Bonn 53115, Germany;5. Dipartimento di Fisica Generale, Universita'' di Torino, via Pietro Giuria 1, 10125 Torino, Italy;6. Center for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, PO Box 28M, Victoria 3800, Australia;1. Institut für Planetologie, University of Münster, Wilhelm-Klemm-Strasse 10, 48149, Münster, Germany;2. Nuclear and Chemical Sciences Division, Lawrence Livermore National Laboratory, Livermore, 7000 East Avenue, CA 94550, USA;3. Department of Earth and Space Sciences, University of Washington, Seattle, WA 98195, USA;4. Institute of Meteoritics, University of New Mexico, Albuquerque, NM 87131, USA;1. Institut für Geologie, Universität Bern, Baltzerstrasse 1+3, 3012 Bern, Switzerland;2. Institut für Planetologie, Universität Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany;1. Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Wilhelm Klemm-Strasse 10, 48149 Münster, Germany;2. ETH Zürich, Institute of Geochemistry and Petrology, Clausiusstrasse 25, 8092 Zürich, Switzerland;3. Origins Laboratory, Department of the Geophysical Sciences, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60637, USA;1. Institut für Planetologie, University of Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany;2. Institut für Geologie und Mineralogie, University of Köln, Zülpicherstrasse 49, 50923 Köln, Germany;3. Lawrence Livermore National Laboratory, Livermore, CA 94550, USA;1. Department of Earth Science and Engineering, Imperial College London, London SW7 2AZ, UK;2. School of Earth Sciences, University of Bristol, Bristol BS8 1RJ, UK;3. Department of Earth Sciences, The Natural History Museum, London SW7 5BD, UK;4. Institute of Applied Geosciences, TNO, Utrecht, The Netherlands |
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| Abstract: | We present osmium isotopic results obtained by sequential leaching of the Murchison meteorite, which reveal the existence of very large internal anomalies of nucleosynthetic origin (ε184Os from ? 108 to 460; ε186Os from ? 14.1 to 12.6; ε188Os from ? 2.6 to 1.6; ε190Os from ? 1.7 to 1.1). Despite these large variations, the isotopic composition of the total leachable osmium (weighted average of the leachates) is close to that of bulk chondrites. This is consistent with efficient large-scale mixing of Os isotopic anomalies in the protosolar nebula. The Os isotopic anomalies are correlated, and can be explained by the variable contributions of components derived from the s, r and p-processes of nucleosynthesis. Surprisingly, much of the s-process rich osmium is released by relatively mild leaching, suggesting the existence of an easily leachable s-process rich presolar phase, or alternatively, of a chemically resistant r-process rich phase. Taken together with previous evidence for a highly insoluble s-process rich carrier, such as SiC, these results argue for the presence of several presolar phases with anomalous nucleosynthetic compositions in the Murchison meteorite. The s-process composition of Os released by mild leaching diverges slightly from that released by aggressive digestion techniques, perhaps suggesting that the presolar phases attacked by these differing procedures condensed in different stellar environments. The correlation between ε190Os and ε188Os can be used to constrain the s-process 190Os/188Os ratio to be 1.275 ± 0.043. Such a ratio can be reproduced in a nuclear reaction network for a MACS value for 190Os of ~ 200 ± 22 mbarn at 30 keV. More generally, these results can help refine predictions of the s-process in the Os mass region, which can be used in turn to constrain the amount of cosmoradiogenic 187Os in the solar system and hence the age of the Galaxy.We also present evidence for extensive internal variation of 184Os abundances in the Murchison meteorite. A steep anti-correlation is observed between ε184Os and ε188Os. Since 184Os is formed uniquely by the p-process, this anti-correlation cannot be explained by variable addition or subtraction of s-process Os to average solar system material. Instead, this suggests that p-process rich presolar grains (e.g., supernova condensates) may be present in meteorites in sufficient quantities to influence the Os isotopic compositions of the leachates. Nevertheless, 184Os is a low abundance isotope and we cannot exclude the possibility that the measured anomalies for this isotope reflect unappreciated analytical artifacts. |
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