Hostname: page-component-848d4c4894-8bljj Total loading time: 0 Render date: 2024-07-05T17:41:28.610Z Has data issue: false hasContentIssue false
  • English
  • Français

White Dwarf Stars: Evolution of the Envelope Composition

Published online by Cambridge University Press:  30 March 2016

James Liebert
James Liebert*
Affiliation:
Steward Observatory University of ArizonaTucson, AZ 85721U.S.A.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Over the last several years, evidence has been unfolding that the surface abundances of white dwarfs may evolve as the stars cool. It is possible that some post-AGB stars enter the white dwarf sequence with far less hydrogen and helium than predicted by standard theory of the quenching of shell sources, and with atmospheres dominated by C and O. The interplay of diffusion and episodes of convective mixing may lead first to He-rich atmospheres, then H-rich, and finally He-rich again.

Type
Joint Commission Meetings
Information
Highlights of Astronomy , Volume 9: Highlights of Astronomy. As presented at the XXIst General Assembly of the IAU, 1991 , 1992 , pp. 639 - 641
Copyright
Copyright © Kluwer 1992

References

REFERENCES

Fontaine, G. and Wesemael, F. 1987, in IAU Coll. 95, The Second Conference on Faint Blue Stars, eds. Philip, A. G. D., et al. (Schenectady NY: L. Davis Press), p. 319.Google Scholar
Liebert, J. 1991, in Evolution of Stars: The Photospheric Abundance Connection, eds. Michaud, G. and Tutukov, A. (Dordrecht: Kluwer), p. 411.CrossRefGoogle Scholar
Werner, K. 1991, Astr. Ap., in press.Google Scholar
Werner, K, Heber, U. and Hunger, K. 1991, Astron. Astrophys., 244, 437.Google Scholar