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A Molecular Line Survey of CRL 2688 at 1 mm and 3 mm Wavelengths

Published online by Cambridge University Press:  21 March 2013

Yong Zhang ,
Sun Kwok ,
Jun-ichi Nakashima  and
Dinh-V Trung
Yong Zhang
Affiliation:
Department of Physics, University of Hong Kong, Pokfulam Road, Hong Kong, China email: [email protected], [email protected], [email protected]
Sun Kwok
Affiliation:
Department of Physics, University of Hong Kong, Pokfulam Road, Hong Kong, China email: [email protected], [email protected], [email protected]
Jun-ichi Nakashima
Affiliation:
Department of Physics, University of Hong Kong, Pokfulam Road, Hong Kong, China email: [email protected], [email protected], [email protected]
Dinh-V Trung
Affiliation:
Institute of Physics, Vietnamese Academy of Science and Technology, 10 DaoTan Street, BaDinh, Hanoi, Vietnam email: [email protected]
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Abstract

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It is well established that circumstellar envelopes (CSEs) around evolved stars are active sites of molecular synthesis, and CSEs are one of the major sources of chemical enrichment in the interstellar space. The investigation of molecular compositions in CSEs is essential to understand the chemical evolution of the Galaxy. In order to study circumstellar chemistry in different environments, we have been systematically performing molecular line surveys of a sample of evolved stars from asymptotic giant branch (AGB) stars, proto-planetary nebulae (PPNs), to planetary nebulae (PNs). The dynamical time scales in different evolutionary stages can impose a time limit on the reaction time scales. Here we report our results for CRL 2688.

Keywords

stars: AGB and post-AGB — line: identification — ISM: molecules — radio lines: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S292: Molecular Gas, Dust, and Star Formation in Galaxies , August 2012 , pp. 68
Copyright
Copyright © International Astronomical Union 2013

References

Cernicharo, J., Agúndez, M., & Guélin, M. 2011, IAU Symp. 280, p. 237CrossRefGoogle Scholar
He, J.-H., Dinh-V-Trung, , Kwok, S.et al. 2008, ApJS, 177, 275Google Scholar
Zhang, Y., Kwok, S., & Dinh-V-Trung, , 2008, ApJ, 678, 328CrossRefGoogle Scholar
Zhang, Y., Kwok, S., & Dinh-V-Trung, , 2009a, ApJ, 691, 1660CrossRefGoogle Scholar
Zhang, Y., Kwok, S., & Nakashima, J. 2009b, ApJ, 700, 1262Google Scholar