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NLTE analyses of PG 1159 stars: constraints for the structure and evolution of post-AGB stars

Published online by Cambridge University Press:  25 May 2016

S. Dreizler ,
K. Werner ,
T. Rauch ,
U. Heber ,
I.N. Reid  and
L. Koesterke
S. Dreizler
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Germany
K. Werner
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Germany
T. Rauch
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Germany
U. Heber
Affiliation:
Dr. Remeis Sternwarte Bamberg, Universität Erlangen–Nürnberg, Germany
I.N. Reid
Affiliation:
California Institute of Technology, USA
L. Koesterke
Affiliation:
Lehrstuhl Astrophysik, Universität Potsdam, Germany

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The majority of all stars (Mi < 8M⊙) 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 (Teff > 100 kK). 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.

Type
Evolved Stars
Information
Symposium - International Astronomical Union , Volume 189: Fundamental Stellar Properties: The Interaction Between Observation and Theory , 1997 , pp. 369 - 372
Copyright
Copyright © Kluwer 1997 

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