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Infrared molecular spectra of carbon stars observed by the ISO SWS

Published online by Cambridge University Press:  25 May 2016

W. Aoki ,
T. Tsuji  and
K. Ohnaka
W. Aoki
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo, Japan
T. Tsuji
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo, Japan
K. Ohnaka
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo, Japan

Abstract

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We carried out observations of bright optical carbon stars with the ISO SWS, and detected the absorption features of CO, CS, CH, SiS and HCN in N-type and SC-type stars. The CH fundamental bands in 3-4 μm in N-type stars are stronger than those in SC-type stars. On the other hand, the first overtone bands of SiS at 6.6 μm were detected in WZ Cas (SC-type), while none of them were detected in N-type stars. These results can be explained well by the lower C/O ratio in SC-type stars than in N-type stars. The absorption features of HCN (v1, v2 + v3 and v1 − v2) are stronger in SC-type stars than in N-type stars. This fact can be explained by the cooler atmospheres of our SC-type stars due to the lower C/O ratio as well as due to the lower effective temperature, compared with the N-type stars in our sample. The CS bands and the band heads of the CO fundamental bands are weaker in the observed spectra than in those predicted by our model atmospheres. This result cannot be explained by the present model atmosphere and one possible explanation is the contribution by the emission of CO and CS in the outer atmosphere.

Type
Part 2. Pulsation, Mass Loss, Cool Envelopes
Information
Symposium - International Astronomical Union , Volume 191: Asymptotic Giant Branch Stars , 1999 , pp. 175 - 180
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

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