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(Pre)-white dwarf stars as measuring tools for yields of AGB nucleosynthesis

Published online by Cambridge University Press:  09 October 2020

Lisa Löbling Open the ORCID record for Lisa Löbling [Opens in a new window]
Lisa Löbling*
Affiliation:
Institut für Astronomie und Astrophysik, Sand 1, 72076 Tübingen, Germany email: loebling@astro.uni-tuebingen.de
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Abstract

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In the helium-rich intershell region of asymptotic giant branch (AGB) stars, slow neutron-capture nucleosynthesis produces heavy elements beyond iron. If the stars experience a final-flash of the He-burning shell, a pulse-driven convection zone establishes, the stars become hydrogen-deficient and exhibit former intershell material at their surfaces. In their subsequent evolution towards the white-dwarf cooling sequence, but still at constant luminosity, a strong stellar wind prevents diffusion to wipe out the information about AGB yields. We present and interpret the analysis results of hydrogen-rich and -deficient post-AGB stars, discuss difficulties in their analysis and review the implications on the understanding of post-AGB evolution.

Keywords

atomic datatechniques: spectroscopicstars: abundancesstars: AGB and post-AGBstars: atmosphereswhite dwarfsplanetary nebulae
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S357: White Dwarfs as Probes of Fundamental Physics: Tracers of Planetary, Stellar and Galactic Evolution , October 2019 , pp. 158 - 161
Copyright
© International Astronomical Union 2020

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