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NLTE Analysis and Chemical Composition of Hot Low-Mass Stars

Published online by Cambridge University Press:  19 July 2016

U. Heber ,
K. Hunger  and
K. Werner
U. Heber
Affiliation:
Institut für Theoretische Physik und Sternwarte, Olshausenstr. 40, D-2300 Kiel 1, Federal Republic of Germany
K. Hunger
Affiliation:
Institut für Theoretische Physik und Sternwarte, Olshausenstr. 40, D-2300 Kiel 1, Federal Republic of Germany
K. Werner
Affiliation:
Institut für Theoretische Physik und Sternwarte, Olshausenstr. 40, D-2300 Kiel 1, Federal Republic of Germany

Abstract

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Spectroscopic analyses of hot pre-white dwarfs, i.e. subluminous O and B stars, are presented. In the B-type stars, the resulting abundance patterns are indicative of atmospheric diffusion (gravitational settling). Amongst the O-type subdwarfs, a new group of comparatively luminous stars is identified. Their position in the HR-diagram suggests that, unlike the “classical” sdOs, they are in a post-AGB stage of evolution. Spectroscopic evidence is presented showing that the born-again post-AGB star scenario of Iben et al. (1983) can explain their origin.

Type
VI. Chemical Composition of Stars
Information
Symposium - International Astronomical Union , Volume 132: The Impact of Veryhigh S/N Spectroscopy on Stellar Physics , 1988 , pp. 389 - 394
Copyright
Copyright © Kluwer 1988 

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