Abstract
The majority of all stars (Мi < 8М⊙) end their lives as white dwarfs (WD). On the tip of the Asymptotic Giant Branch (AGB) the star ejects its outer layers which become a Planetary Nebula and the stellar core evolves rapidly towards very high effective temperatures (Тeff >100kK). When the nuclear burning in the H or He shell ceases the star enters the WD cooling sequence. The evolution starting from the AGB is separated in a H—rich and a H—deficient sequence where the latter contributes with a number fraction of ≈20%. In this paper we describe our recent effort in the analysis of one group of these stars, the PG 1159 stars.
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Dreizler, S., Werner, K., Rauch, T., Heber, U., Reid, I.N., Koesterke, L. (1997). NLTE Analyses of PG 1159 Stars: Constraints for the Structure and Evolution of Post-AGB Stars. In: Bedding, T.R., Booth, A.J., Davis, J. (eds) Fundamental Stellar Properties: The Interaction Between Observation and Theory. International Astronomical Union / Union Astronomique Internationale, vol 189. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-5602-8_49
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DOI: https://doi.org/10.1007/978-94-011-5602-8_49
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