New chemical profiles for the asteroseismology of ZZ CETI stars

L. G. Althaus, A. H. Córsico, Agnes Kim, A. D. Romero, I. Renedo, E. García-Berro, M. M. Miller Bertolami

Research output: Contribution to journalArticle

35 Citations (Scopus)

Abstract

We compute new chemical profiles for the core and envelope of white dwarfs appropriate for pulsational studies of ZZ Ceti stars. These profiles are extracted from the complete evolution of progenitor stars, evolved through the main sequence and the thermally pulsing asymptotic giant branch (AGB) stages, and from time-dependent element diffusion during white dwarf evolution. We discuss the importance of the initial-final mass relationship for the white dwarf carbon-oxygen composition. In particular, we find that the central oxygen abundance may be underestimated by about 15% if the white dwarf mass is assumed to be the hydrogen-free core mass before the first thermal pulse. We also discuss the importance for the chemical profiles expected in the outermost layers of ZZ Ceti stars of the computation of the thermally pulsing AGB phase and of the phase in which element diffusion is relevant. We find a strong dependence of the outer layer chemical stratification on the stellar mass. In particular, in the less massive models, the double-layered structure in the helium layer built up during the thermally pulsing AGB phase is not removed by diffusion by the time the ZZ Ceti stage is reached. Finally, we perform adiabatic pulsation calculations and discuss the implications of our new chemical profiles for the pulsational properties of ZZ Ceti stars. We find that the whole g-mode period spectrum and the mode-trapping properties of these pulsating white dwarfs as derived from our new chemical profiles are substantially different from those based on chemical profiles widely used in existing asteroseismological studies. Thus, we expect the asteroseismological models derived from our chemical profiles to be significantly different from those found thus far.

Original languageEnglish (US)
Pages (from-to)897-907
Number of pages11
JournalAstrophysical Journal
Volume717
Issue number2
DOIs
StatePublished - Jan 1 2010

Fingerprint

asteroseismology
stars
profiles
oxygen
chemical
stratification
stellar mass
helium
trapping
envelopes
hydrogen
carbon
pulses

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Althaus, L. G., Córsico, A. H., Kim, A., Romero, A. D., Renedo, I., García-Berro, E., & Miller Bertolami, M. M. (2010). New chemical profiles for the asteroseismology of ZZ CETI stars. Astrophysical Journal, 717(2), 897-907. https://doi.org/10.1088/0004-637X/717/2/897
Althaus, L. G. ; Córsico, A. H. ; Kim, Agnes ; Romero, A. D. ; Renedo, I. ; García-Berro, E. ; Miller Bertolami, M. M. / New chemical profiles for the asteroseismology of ZZ CETI stars. In: Astrophysical Journal. 2010 ; Vol. 717, No. 2. pp. 897-907.
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Althaus, LG, Córsico, AH, Kim, A, Romero, AD, Renedo, I, García-Berro, E & Miller Bertolami, MM 2010, 'New chemical profiles for the asteroseismology of ZZ CETI stars', Astrophysical Journal, vol. 717, no. 2, pp. 897-907. https://doi.org/10.1088/0004-637X/717/2/897

New chemical profiles for the asteroseismology of ZZ CETI stars. / Althaus, L. G.; Córsico, A. H.; Kim, Agnes; Romero, A. D.; Renedo, I.; García-Berro, E.; Miller Bertolami, M. M.

In: Astrophysical Journal, Vol. 717, No. 2, 01.01.2010, p. 897-907.

Research output: Contribution to journalArticle

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AU - Córsico, A. H.

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N2 - We compute new chemical profiles for the core and envelope of white dwarfs appropriate for pulsational studies of ZZ Ceti stars. These profiles are extracted from the complete evolution of progenitor stars, evolved through the main sequence and the thermally pulsing asymptotic giant branch (AGB) stages, and from time-dependent element diffusion during white dwarf evolution. We discuss the importance of the initial-final mass relationship for the white dwarf carbon-oxygen composition. In particular, we find that the central oxygen abundance may be underestimated by about 15% if the white dwarf mass is assumed to be the hydrogen-free core mass before the first thermal pulse. We also discuss the importance for the chemical profiles expected in the outermost layers of ZZ Ceti stars of the computation of the thermally pulsing AGB phase and of the phase in which element diffusion is relevant. We find a strong dependence of the outer layer chemical stratification on the stellar mass. In particular, in the less massive models, the double-layered structure in the helium layer built up during the thermally pulsing AGB phase is not removed by diffusion by the time the ZZ Ceti stage is reached. Finally, we perform adiabatic pulsation calculations and discuss the implications of our new chemical profiles for the pulsational properties of ZZ Ceti stars. We find that the whole g-mode period spectrum and the mode-trapping properties of these pulsating white dwarfs as derived from our new chemical profiles are substantially different from those based on chemical profiles widely used in existing asteroseismological studies. Thus, we expect the asteroseismological models derived from our chemical profiles to be significantly different from those found thus far.

AB - We compute new chemical profiles for the core and envelope of white dwarfs appropriate for pulsational studies of ZZ Ceti stars. These profiles are extracted from the complete evolution of progenitor stars, evolved through the main sequence and the thermally pulsing asymptotic giant branch (AGB) stages, and from time-dependent element diffusion during white dwarf evolution. We discuss the importance of the initial-final mass relationship for the white dwarf carbon-oxygen composition. In particular, we find that the central oxygen abundance may be underestimated by about 15% if the white dwarf mass is assumed to be the hydrogen-free core mass before the first thermal pulse. We also discuss the importance for the chemical profiles expected in the outermost layers of ZZ Ceti stars of the computation of the thermally pulsing AGB phase and of the phase in which element diffusion is relevant. We find a strong dependence of the outer layer chemical stratification on the stellar mass. In particular, in the less massive models, the double-layered structure in the helium layer built up during the thermally pulsing AGB phase is not removed by diffusion by the time the ZZ Ceti stage is reached. Finally, we perform adiabatic pulsation calculations and discuss the implications of our new chemical profiles for the pulsational properties of ZZ Ceti stars. We find that the whole g-mode period spectrum and the mode-trapping properties of these pulsating white dwarfs as derived from our new chemical profiles are substantially different from those based on chemical profiles widely used in existing asteroseismological studies. Thus, we expect the asteroseismological models derived from our chemical profiles to be significantly different from those found thus far.

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Althaus LG, Córsico AH, Kim A, Romero AD, Renedo I, García-Berro E et al. New chemical profiles for the asteroseismology of ZZ CETI stars. Astrophysical Journal. 2010 Jan 1;717(2):897-907. https://doi.org/10.1088/0004-637X/717/2/897