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Binary post-AGB stars

Published online by Cambridge University Press:  25 May 2016

L.B.F.M. Waters ,
C. Waelkens  and
H. Van Winckel
L.B.F.M. Waters
Affiliation:
Astronomical Institute, University of Amsterdam
C. Waelkens
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven
H. Van Winckel
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven

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Low and intermediate mass stars leave the Asymptotic Giant Branch (AGB) when the mass in their H-rich envelope is less than about 0.01 M⊙, and the high mass loss drops several orders of magnitude. The central star rapidly evolves to the left part of the HR diagram along a track of constant luminosity (e.g. Schönberner 1983). In principle the evolution of the central star to higher Teff and the expansion and cooling of the AGB remnant are easy to calculate. In practice several complicating factors arise which make it much more difficult to predict the morphology and properties of post-AGB stars, such as binarity, post-AGB mass loss and aspherical AGB mass loss. Binarity of post-AGB stars affects the morphology of the circumstellar environment, and it affects evolutionary timescales and surface chemical abundances of the components in the system. This review discusses some properties of binary post-AGB stars.

Type
V. From AGB to Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 313 - 318
Copyright
Copyright © Kluwer 1997 

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