AGB star intershell abundances inferred from analyses of extremely hot H-deficient post-AGB stars

Details AGB star intershell abundances inferred from analyses of extremely hot H-deficient post-AGB stars AGB star intershell abundances inferred from analyses of extremely hot H-deficient post-AGB stars

2006-03-09

arxiv.org/abs/astro-ph/0603225v1

Astronomy and Astrophysics

Astrophysics

To appear in Proceedings of The VIII Torino Workshop on Nucleosynthesis in AGB stars: Constraints on AGB Nucleosynthesis from

Scientific paper

The hydrogen-deficiency in extremely hot post-AGB stars of spectral class PG1159 is probably caused by a (very) late helium-shell flash or a AGB final thermal pulse that consumes the hydrogen envelope, exposing the usually-hidden intershell region. Thus, the photospheric element abundances of these stars allow to draw conclusions about details of nuclear burning and mixing processes in the precursor AGB stars. We compare predicted element abundances to those determined by quantitative spectral analyses performed with advanced non-LTE model atmospheres. A good qualitative and quantitative agreement is found for many species (He, C, N, O, Ne, F, Si) but discrepancies for others (P, S, Fe) point at shortcomings in stellar evolution models for AGB stars.

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