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CO in OH/IR-Stars - on Excitation and Mass Loss

Published online by Cambridge University Press:  12 April 2016

A. Heske ,
H.J. Habing ,
W.E.C.J. van der Veen ,
A. Omont  and
T. Forveille
A. Heske
Affiliation:
Sterrewacht Leiden, The Netherlands
H.J. Habing
Affiliation:
Sterrewacht Leiden, The Netherlands
W.E.C.J. van der Veen
Affiliation:
Sterrewacht Leiden, The Netherlands
A. Omont
Affiliation:
Observatoire de Grenoble
T. Forveille
Affiliation:
Observatoire de Grenoble

Extract

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Observations of CO in long period variables have been widely used to determine mass loss rates by applying models for CO line formation (e.g. Knapp and Morris, 1985) which use a simple method to take the impact from infrared radiation into account. Recent 00(2-1) and (1-0) observations of some more evolved OH/IR stars yielded much too low mass loss rates using these simple models, thus indicating that they cannot be extrapolated to far evolved AGB stars with optically thick circumstellar envelopes.

Type
5. Chromospheres, Winds and Mass Loss
Information
International Astronomical Union Colloquium , Volume 106: Evolution of Peculiar Red Giant Stars , 1989 , pp. 368
Copyright
Copyright © Cambridge University Press 1989