The formation of DA white dwarfs with thin hydrogen envelopes

Abstract

We study the formation and evolution of DA white dwarfs, the progenitors of which have experienced a late thermal pulse (LTP) shortly after the departure from the thermally pulsing AGB. To this end, we compute the complete evolution of an initially 2.7 Mo star all the way from the zero-age main sequence to the white dwarf stage. We find that most of the original H-rich material of the post-AGB remnant is burnt during the post-LTP evolution, with the result that, at entering its white dwarf cooling track, the remaining H envelope becomes 10^-6 Mo in agreement with asteroseismological inferences for some ZZ Ceti stars.

4 pages including 3 figures. Accepted for publication in Astronomy and Astrophysics Letters

References in corpus (3)

• The formation and evolution of hydrogen-deficient post-AGB white dwarfs: the emerging chemical profile and the expectations for the PG1159-DB-DQ evolutionary connection
• Evolution on the AGB and beyond: On the formation of H-deficient post-AGB stars
• New evolutionary models for massive ZZ Ceti stars: I. First results for their pulsational properties

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