English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We compute new chemical profiles for the core and envelope of white dwarfsappropriate for pulsational studies of ZZ Ceti stars. These profiles areextracted from the complete evolution of progenitor stars, evolved through themain sequence and the thermally-pulsing asymptotic giant branch (AGB) stages,and from time-dependent element diffusion during white dwarf evolution. Wediscuss the importance of the initial-final mass relationship for the whitedwarf carbon-oxygen composition. In particular, we find that the central oxygenabundance may be underestimated by about 15% if the white dwarf mass is assumedto be the hydrogen-free core mass before the first thermal pulse. We alsodiscuss the importance for the chemical profiles expected in the outermostlayers of ZZ Ceti stars of the computation of the thermally-pulsing AGB phaseand of the phase in which element diffusion is relevant. We find a strongdependence of the outer layer chemical stratification on the stellar mass. Inparticular, in the less massive models, the double-layered structure in thehelium layer built up during the thermally-pulsing AGB phase is not removed bydiffusion by the time the ZZ Ceti stage is reached. Finally, we performadiabatic pulsation calculations and discuss the implications of our newchemical profiles for the pulsational properties of ZZ Ceti stars. We find thatthe whole $g-$mode period spectrum and the mode-trapping properties of thesepulsating white dwarfs as derived from our new chemical profiles aresubstantially different from those based on chemical profiles widely used inexisting asteroseismological studies. Thus, we expect the asteroseismologicalmodels derived from our chemical profiles to be significantly different fromthose found thus far.

New chemical profiles for the asteroseismology of ZZ Ceti stars