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Hot subluminous stars

  • Ulrich Heber
V. Evolved Stars
Part of the Lecture Notes in Physics book series (LNP, volume 401)

Abstract

Spectroscopic analyses of blue horizontal branch stars, subluminous B- and O-stars are reviewed. These classes of stars trace stellar evolution from the horizontal branch towards the white dwarf cooling sequence. The resulting atmospheric parameters and abundances are used to obtain constraints on the evolutionary status of the different classes of stars. The sdB stars form a homogeneous group and can be identified with models of the extended horizontal branch. Abundance anomalies (deficiency of helium and some metals, enrichment of 3He) observed in Horizontal Branch stars and sdB stars are caused by atmospheric diffusion. The class of subluminous O stars is much less homogenous and two subclasses can be defined: the “compact” sdO stars probably evolved from the extended horizontal branch and are hence successors of the sdBs, whereas some sdOs of relatively low gravity are in a post-AGB stage of evolution. Hot subdwarfs in binary systems can be formed by case B or case C mass transfer.

Keywords

Globular Cluster Planetary Nebula Horizontal Branch Helium Abundance Visual Binary 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer-Verlag 1992

Authors and Affiliations

  • Ulrich Heber
    • 1
  1. 1.Institut für Theoretische Physik und Sternwarte der Universität KielKielGermany

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