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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

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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

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