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H- and He-burning Central Stars and the Evolution to White Dwarfs

Published online by Cambridge University Press:  26 May 2016

T. Blöcker
T. Blöcker*
Affiliation:
Max–Planck–Institut für Radioastronomie, 53121 Bonn, Germany

Abstract

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The structure and evolution of central stars of planetary nebulae (CSPNe) is reviewed. CSPNe represent the rapid transitional stage between the Asymptotic Giant Branch (AGB) and the white-dwarf domain. It is shown that the whole evolution off the AGB through the central-star regime depends on the evolutionary history. The detailed evolution into a white dwarf is controlled by the internal stellar structure which, in turn, is determined by the duration of the preceding AGB evolution and therefore by the AGB mass-loss history. The evolution of hydrogen-deficient central stars has been a matter of debate since many years. Convective overshoot appears to be a key ingredient to model these objects. Various thermal-pulse scenarios with inclusion of overshoot are discussed, leading to surface abundances in general agreement with those observed for Wolf-Rayet central stars.

Type
Part III: Planetary Nebulae in the Scheme of Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 209: Planetary Nebulae: Their Evolution and Role in the Universe , 2003 , pp. 101 - 108
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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