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Molecular abundances in IRC + 10216

Nature volume 281, pages 263–266 (1979)Cite this article

Abstract

The observed molecular column-densities in IRC + 10216 can be matched by chemical equilibrium calculations for T∼1,250K, P∼100dyn cm−2, and no graphite grain formation. Condensation of silicon carbide into grains may explain the low observed abundances of SiO and SiS. A compressed gaseous shell may be formed between successive dust shells lost by the central variable carbon star during each of its cycles.

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Authors and Affiliations

  1. Astronomy Centre, University of Sussex, Falmer, Brighton, UK

    E. M. McCabe & R. Connon Smith

  2. Department of Astronomy, University of Texas, Austin, Texas, 78712

    R. E. S. Clegg

Authors
  1. E. M. McCabe
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  2. R. Connon Smith
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  3. R. E. S. Clegg
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McCabe, E., Smith, R. & Clegg, R. Molecular abundances in IRC + 10216. Nature 281, 263–266 (1979). https://doi.org/10.1038/281263a0

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