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Organic compounds in meteoritesThe problem of whether organic compounds originated in meteorites as a primary condensate from a solar gas or whether they were introduced as a secondary product into the meteorite during its residence in a parent body is examined by initially attempting to reconstruct the physical conditions during condensation (temperature, pressure, time) from clues in the inorganic matrix of the meteorite. The condensation behavior of carbon under these conditions is then analyzed on the basis of thermodynamic calculations, and compounds synthesized in model experiments on the condensation of carbon are compared with those actually found in meteorites. Organic compounds in meteorites seem to have formed by catalytic reactions of carbon monoxide, hydrogen, and ammonia in the solar nebula at 360 to 400 K temperature and about 3 to 7.6 microtorr pressure. The onset of these reactions was triggered by the formation of suitable catalysts (magnetite, hydrated silicates) at these temperatures.
Document ID
19740029965
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Anders, E.
Hayatsu, R.
(Chicago, University Chicago, Ill., United States)
Studier, M. H.
(Argonne National Laboratory Argonne, Ill., United States)
Date Acquired
August 7, 2013
Publication Date
November 23, 1973
Publication Information
Publication: Science
Volume: 182
Subject Category
Space Sciences
Accession Number
74A12715
Funding Number(s)
CONTRACT_GRANT: NGR-14-001-203
Distribution Limits
Public
Copyright
Other

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