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Abundances in Cool Evolved Stars

Published online by Cambridge University Press:  12 April 2016

Catherine A. Pilachowski
Catherine A. Pilachowski*
Affiliation:
National Optical Astronomy Observatories, Kitt Peak National Observatory PO Box 26732, Tucson, AZ 85726-6732, USA

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Nature has filled the upper right quadrant of the Hertzsprung-Russell diagram with more varieties of peculiar stars and odd chemical compositions than even our most speculative observers and theorists could dream up. To bring some structure to this vast subject I will categorize the phenomena we observe according to our model of stellar evolution, dividing the stars among the first ascent of the giant branch and the core-helium burning phase, the asymptotic giant branch (double shell-burning) phase, and the post-AGB and pre-planetary nebula stars. The types of stars found in these three groups are summarized below.

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. 17 - 30
Copyright
Copyright © Springer-Verlag 1988

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