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Molecular Evolution from AGB Stars to Planetary Nebulae

Published online by Cambridge University Press:  21 December 2011

Sun Kwok
Sun Kwok*
Affiliation:
Faculty of Science, The University of Hong Kong, Hong Kong, China email: sunkwok@hku.hk
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Abstract

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The late stages of stellar evolution from the Asymptotic Giant Branch (AGB) to planetary nebulae represent the most active phase of molecular synthesis in a star's life. Over 60 molecular species, including inorganics, organics, radicals, chains, rings, and molecular ions have been detected in the circumstellar envelopes of evolved stars. Most interestingly, complex organic compounds of aromatic and aliphatic structures are synthesized over very short time intervals after the end of the AGB. Also appeared during the post-AGB evolution are the unidentified 21 and 30 μm emission features, which are believed to originate from carbonaceous compounds.

The circumstellar environment is an ideal laboratory for the testing of theories of chemical synthesis. The distinct spectral behavior among AGB stars, proto-planetary nebulae (PPN), and planetary nebulae (PN) and the short evolutionary time scales that separate these stages pose severe constraints on models. In this paper, we will present an observational summary of the chemical synthesis in the late stages of stellar evolution, discuss chemical and physical processes at work, and speculate on the possible effects these chemical products have on the Galaxy and the Solar System.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S280: The Molecular Universe , June 2011 , pp. 203 - 215
Copyright
Copyright © International Astronomical Union 2011

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