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The meteoritic record of presolar and early solar system organic chemistryCarbon, hydrogen, and nitrogen isotopic analyses of various classes of organic compounds done in collaboration with Epstein and Krishnamurthy (Caltech) have shown these compounds to be enriched to varying degrees in the heavier isotopes. These results, in particular the large deuterium enrichments, have been interpreted as indicating an interstellar origin for the meteorite compounds or their precursors. Such isotopic fractionations, of hydrogen especially, are characteristic of low temperature ion-molecule reactions in cold interstellar clouds. There is also evidence from the large corresponding suites of alpha-amino and alpha-hydroxy acids found in meteorites suggesting that aqueous phase chemistry on the meteorite parent body played an important role in the formation of these compounds. These data support the hypothesis that interstellar compounds survived in the solar nebula at a radial distance corresponding to the asteroid belt, were incorporated into the parent body in icy, volatile-rich, planetesinals, and underwent further reactions during a period of aqueous activity within the early parent body to give the present suite of meteorite compounds. This formation hypothesis will be discussed and the results of recent isotopic and molecular analyses bearing on it will be presented.
Document ID
19950032156
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Cronin, John R.
(Arizona State University Tempe, AZ, US, United States)
Pizzarello, Sandra
(Arizona State University Tempe, AZ, US, United States)
Date Acquired
August 16, 2013
Publication Date
June 1, 1994
Publication Information
Publication: Origins of Life and Evolution of the Biosphere
Volume: 24
Issue: 4-Feb
ISSN: 0169-6149
Subject Category
Space Biology
Accession Number
95A63755
Funding Number(s)
CONTRACT_GRANT: NAGW-1899
Distribution Limits
Public
Copyright
Other

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