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Chemical Peculiarities, Mass Loss, and Final Evolution of AGB Stars in the Magellanic Clouds

Published online by Cambridge University Press:  12 April 2016

P.R. Wood
P.R. Wood*
Affiliation:
Mount Stromlo and Siding Spring Observatories Private Bag, Woden P.O., A.C.T. 2606Australia

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The Magellanic Clouds are sufficiently close that evolved stars which exhibit chemical peculiarities and the effects of mass loss can be readily observed. Such objects include carbon stars, S stars, long-period variables, OH/IR stars and planetary nebulae. Because of the relatively well-known distances of the Magellanic Clouds, the intrinsic luminosities of these objects can be accurately determined, in contrast to the situation in the Galaxy where the great majority of asymptotic giant branch (AGB) stars occur in the field population. In this review, observations of AGB stars in the Magellanic Clouds will be discussed with particular reference to those features which can shed light on mass loss and chemical peculiarities resulting from stellar evolution.

Type
Part I. Chemical Peculiarities as Probe of Stellar Evolution
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 31 - 37
Copyright
Copyright © Springer-Verlag 1988

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