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Organic compounds in meteorites and their origins

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Cosmo- and Geochemistry

Part of the book series: Topics in Current Chemistry ((TOPCURRCHEM,volume 99))

Abstract

C1 and C2 carbonaceous chondrites contain several percent of organic matter, mainly as a bridged aromatic polymer containing COOH, OH, and CO groups, as well as heterocyclic rings containing N, O, and S. The remaining 5–30% includes the following compound classes, either present initially or generated by solvolysis: alkanes (mainly normal), alkenes, arenes, alicyclics, alcohols, aliphatic carboxylic acids, purines, pyrimidines, and other basic N-compounds, amino acids, porphyrin-like pigments, carbynes, etc.

On the basis of laboratory experiments, it appears that these compounds formed in the solar nebula, by catalytic (Fischer-Tropsch) reactions of CO, H2, and NH3 at 360–400 K, ∼ 10−5 atm. The onset of these reactions was triggered by the formation of suitable catalysts (magnetite, hydrated silicates) at these temperatures. Such reactions may be a source of prebiotic carbon compounds on the inner planets, and interstellar molecules.

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Authors and Affiliations

  1. Chemistry Division, Argonne National Laboratory, 60439, Argonne, IL, USA

    Ryoichi Hayatsu

  2. Enrico Fermi Institute and Dept. of Chemistry, University of Chicago, 60637, Chicago, IL, USA

    Edward Anders

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  1. Ryoichi Hayatsu
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  2. Edward Anders
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© 1981 Springer-Verlag

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Hayatsu, R., Anders, E. (1981). Organic compounds in meteorites and their origins. In: Cosmo- and Geochemistry. Topics in Current Chemistry, vol 99. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-10920-X_13

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  • DOI: https://doi.org/10.1007/3-540-10920-X_13

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  • Print ISBN: 978-3-540-10920-4

  • Online ISBN: 978-3-540-38806-7

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