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Relic interstellar grains in Murchison meteorite

Yang, Jongmann and Epstein, Samuel (1984) Relic interstellar grains in Murchison meteorite. Nature, 311 (5986). pp. 544-547. ISSN 0028-0836. doi:10.1038/311544a0.

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Isotopic analyses of hydrogen, carbon and nitrogen in meteorites provide important information about the origin and history of these elements both in meteorites and in the Solar System. Here we show that, in the Murchison meteorite, the D/H ratios of hydrogen are unusually high in several separates and in one case up to 30 times the cosmic value of 2 × 10^(−5). Many phases show high ^(13)C/^(12)C ratios, up to 2.5 times the terrestrial value of 0.011. These ^(13)C-rich and D-rich components of the two chemical elements are not correlated. Also they are heterogeneously distributed, suggesting that different components in the meteorite originated from different astrophysical sites and at different times. The D-rich hydrogen in the meteorite is probably due to molecules formed by ion–molecule reactions in interstellar clouds while the tiny amount of ^(13)C-rich carbon is probably due to nucleosynthesis in red giant stars as suggested by Swart et al. Both of these heavy-isotope enriched components survived homogenization in the accumulation and subsequent history of the meteorites.

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Additional Information:© 1984 Nature Publishing Group. Received 16 May; accepted 24 July 1984. We thank Dr I. R. Kaplan for nitrogen analyses, J. Ruth for technical assistance, and Dr. E. Olson for a specimen of Murchison meteorite. This research was funded by NASA (NGL-05-002-190) and by NSF (EAR-7816873).
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Issue or Number:5986
Record Number:CaltechAUTHORS:20140311-110627561
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Official Citation:Relic interstellar grains in Murchison meteorite 544-547 Jongmann Yang & Samuel Epstein doi:10.1038/311544a0
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:44244
Deposited By: Ruth Sustaita
Deposited On:11 Mar 2014 21:04
Last Modified:10 Nov 2021 16:49

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