Hostname: page-component-788cddb947-55tpx Total loading time: 0 Render date: 2024-10-10T15:18:01.074Z Has data issue: false hasContentIssue false

The Evolution of Central Stars of Planetary Nebulae

Published online by Cambridge University Press:  15 December 2006

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
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Type
Contributed Papers
Copyright
© 2006 International Astronomical Union