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Chemistry in Protoplanetary Nebulae

Published online by Cambridge University Press:  07 August 2017

D A Howe ,
T J Millar  and
D A Williams
D A Howe
Affiliation:
Department of Mathematics, UMIST, PO Box 88, Manchester M60 1QD, UK
T J Millar
Affiliation:
Department of Mathematics, UMIST, PO Box 88, Manchester M60 1QD, UK
D A Williams
Affiliation:
Department of Mathematics, UMIST, PO Box 88, Manchester M60 1QD, UK

Abstract

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We have investigated gas-phase chemistry in a remnant red giant wind, during transition to a planetary nebula, using the interacting stellar winds model. Rapid destruction by UV of most existing molecules is predicted, within ~ 100 yrs of the core star heating up, suggesting that the large molecules in CRL 618 may be destroyed within decades. However, significant abundances of some hydrogenated molecules and ions (eg. CH+, CH2+, CH3+, CH, CH2, NH) may form behind the shock predicted by the interacting stellar winds model. Also, survival and/or formation of observable amounts of some molecules (eg. HCN, CN, HC3N) may occur in dense clumps which survive transition, and may explain the existence eg. of HCN in NGC 7027.

Type
Near Stellar Environments
Information
Symposium - International Astronomical Union , Volume 150: Astrochemistry of Cosmic Phenomena , 1992 , pp. 363 - 364
Copyright
Copyright © Kluwer 1992 

References

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