New cooling sequences for old white dwarfs
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hdl:2117/10019
Document typeArticle
Defense date2010-07
Rights accessRestricted access - publisher's policy
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Abstract
We present full evolutionary calculations appropriate for the study of hydrogen-rich DA white dwarfs. This is
done by evolving white dwarf progenitors from the zero-age main sequence, through the core hydrogen-burning
phase, the helium-burning phase, and the thermally pulsing asymptotic giant branch phase to the white dwarf stage.
Complete evolutionary sequences are computed for a wide range of stellarmasses and for two different metallicities,
Z = 0.01, which is representative of the solar neighborhood, and Z = 0.001, which is appropriate for the study of old
stellar systems, like globular clusters. During the white dwarf cooling stage, we self-consistently compute the phase
in which nuclear reactions are still important, the diffusive evolution of the elements in the outer layers and, finally,
we also take into account all the relevant energy sources in the deep interior of the white dwarf, such as the release
of latent heat and the release of gravitational energy due to carbon–oxygen phase separation upon crystallization.
We also provide colors and magnitudes for these sequences, based on a new set of improved non-gray white dwarf
model atmospheres, which include the most up-to-date physical inputs like the Lyα quasi-molecular opacity. The
calculations are extended down to an effective temperature of 2500 K. Our calculations provide a homogeneous set
of evolutionary cooling tracks appropriate for mass and age determinations of old DA white dwarfs and for white
dwarf cosmochronology of the different Galactic populations.
CitationRenedo, I. [et al.]. New cooling sequences for old white dwarfs. "The astrophysical journal letters", Juliol 2010, vol. 717, núm. 1, p. 183-195.
Publisher versionhttp://iopscience.iop.org/0004-637X/717/1/183
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