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Abundances in Hot Evolved Stars

Published online by Cambridge University Press:  12 April 2016

D. Husfeld
D. Husfeld*
Affiliation:
Universitäts-Sternwarte München Scheinerstr. 1, D-8000 München 80, Germany

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In the upper left corner of the HR-diagram various stars have been found that are clearly not members of the hydrogen main sequence. The majority of them lie to the left and below the main sequence, indicating that they are highly evolved stars close to the extinction of their thermonuclear power source and hence to rapid cooling towards the white dwarf domain. The implication is that a “short” time ago they were red giants and as such experienced phenomena like mixing, dredge-up and heavy mass loss. Therefore, one expects the hot evolved stars to display the consequences of the afore mentioned processes that are up to now not satisfactorily understood.

Type
Part I. Chemical Peculiarities as Probe of Stellar Evolution
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 59 - 69
Copyright
Copyright © Springer-Verlag 1988

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