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The Evolution of Central Stars of Planetary Nebulae

Published online by Cambridge University Press:  15 December 2006

Falk Herwig ,
Bernd Freytag  and
Klaus Werner
Falk Herwig
Affiliation:
Theoretical Astrophysics Group, Los Alamos National Laboratory, Los Alamos, NM 87545, USA email: fherwig@lanl.gov
Bernd Freytag
Affiliation:
Theoretical Astrophysics Group, Los Alamos National Laboratory, Los Alamos, NM 87545, USA email: fherwig@lanl.gov Department of Astronomy and Space Physics at Uppsala University, Sweden email: bf@astro.uu.se
Klaus Werner
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D-72076 Tübingen, Germany email: werner@astro.uni-tuebingen.de
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Abstract

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The evolution of central stars of planetary nebulae can proceed in several distinct ways, either leading to H-deficiency or to H-normal surface composition. Several new simulations of the evolution channels that lead to H-deficiency are now available, mainly the born-again scenarios that are triggered by a He-shell flash during the hot pre-white dwarf evolution phase. A realistic AGB progenitor evolution is important for correct HRD tracks, that allow mass determinations. New hydrodynamic simulations of He-shell flash convection including cases with H-ingestion are now performed, and allow a determination of the convective extra-mixing efficiency. This has direct consequences for the intershell abundance distribution of AGB stars that can be observed in the H-deficient CSPN.

Keywords

stars: AGB and post-AGBstars: evolutionhydrodynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 103 - 110
Copyright
© 2006 International Astronomical Union