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The initial/final mass relation for stellar evolution with mass loss

Published online by Cambridge University Press:  12 April 2016

Volker Weidemann
Volker Weidemann*
Affiliation:
Institut f.Theoretische Physik und Sternwarte Universität Kiel, Fed.Rep. Germany

Extract

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The relation between initial and final masses is discussed under consideration of changing theoretical concepts and new empirical data on masses of white dwarfs and nuclei of planetary nebulae. It is concluded that presently adopted schemes of evolution need revision, and that no universal relation exists.

The strongest evidence for large amounts of mass loss during stellar evolution has been provided by the existence of white dwarfs – with masses typically of 0.6 m (m = M/Mʘ), much below the galactic turn-off masses – and by the phenomenon of planetary nebula production before a star descends into the white dwarf region.

Type
Session VI - Mass Loss and Stellar Evolution: Low Mass Stars
Information
International Astronomical Union Colloquium , Volume 59: Effects of Mass Loss on Stellar Evolution , 1981 , pp. 339 - 344
Copyright
Copyright © Reidel 1981

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