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Interstellar Grains in Meteorites: Diamond and Silicon Carbide

Published online by Cambridge University Press:  23 September 2016

Edward Anders ,
Roy S. Lewis ,
Tang Ming  and
Ernst Zinner
Edward Anders
Affiliation:
Enrico Fermi Institute and Department of Chemistry, University of Chicago 5640 S. Ellis Avenue, Chicago IL 60637-1433 USA
Roy S. Lewis
Affiliation:
Enrico Fermi Institute and Department of Chemistry, University of Chicago 5640 S. Ellis Avenue, Chicago IL 60637-1433 USA
Tang Ming
Affiliation:
Enrico Fermi Institute and Department of Chemistry, University of Chicago 5640 S. Ellis Avenue, Chicago IL 60637-1433 USA
Ernst Zinner
Affiliation:
McDonnell Center for Space Sciences, Washington University, St. Louis, MO 63130 USA

Abstract

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Well-preserved interstellar grains occur in carbonaceous chondrites. Diamond (10-100å) contains r- and p-process Xe (suggesting a supernovae connection), and appears to have formed by stellar condensation, not by interstellar shocks. SiC (mainly 0.1-1 μm) is labeled either with s-process Xe, Kr (red giant?) or with Ne22, N15 (nova?), and shows large isotopic variations in N (100x), C (16x), and Si (1.3x). As Si is unaffected by H, He-burning, the Si variations reflect the isotopic heterogeneity of the ISM on the scale of individual stars; the Si compositions found thus far require at least 6 separate stars.

Type
Section VII : Interstellar Dust and the Solar System
Information
Symposium - International Astronomical Union , Volume 135: Interstellar Dust , 1989 , pp. 389 - 402
Copyright
Copyright © Kluwer 1989 

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