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The Possibility of Detecting DC

Published online by Cambridge University Press:  25 April 2016

N. S. Witte  and
R. D. Brown
N. S. Witte
Affiliation:
Department of Chemistry, Monash University
R. D. Brown
Affiliation:
Department of Chemistry, Monash University
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Extract

IRC + 10216, a bright infrared late type carbon star, is observed to have millimetre range line emission of the species 12CO, 13CO, CS, C2H, HC3N, CN, HCN, SiS and SiO in an extended envelope around the central infrared sources. The infrared emission arises from two concentric dust shells around the star: an inner 0”.2 arc radius shell of 600 K and optically thick, i.e. radiating as 600 K black body, and an outer shell 1″.0 arc radius at 375 K and optically thin for λ ≳ 2μ. A model explaining the line emission in terms of infrared pumping between the two lowest vibrational levels, first proposed by Morris (1975a) for IRC + 10216, was used to calculate antenna temperatures for various rotational transitions of HC3N; since there is a prima facie agreement between the calculated and observed values for HC3N we have attempted the same calculation for DC3N.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 3 , Issue 2 , September 1977 , pp. 146 - 147
Copyright
Copyright © Astronomical Society of Australia 1977

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References

Castor, J. I., Mon. Not. R. Astron. Soc. 149, 111 (1970).Google Scholar
Morris, M., Astrophys. J. 197, 603 (1975a).CrossRefGoogle Scholar
Morris, M., Gilmore, W., Palmer, P., Turner, B. E., and Zuckerman, B., Astrophys. J. (Letters) 199, L47 (1975b)Google Scholar