New cooling sequences for old white dwarfs

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...

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Detalles Bibliográficos
Autores principales: Renedo, I., Althaus, Leandro Gabriel, Miller Bertolami, Marcelo Miguel, Romero, A. D., Córsico, Alejandro Hugo, Rohrmann, R.D., García-Berro, E.
Formato: Articulo
Lenguaje:Inglés
Publicado: 2010
Materias:
Ciencias Astronómicas
Stars: evolution
Stars: interiors
White dwarfs
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/82493
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-82493
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
Stars: evolution
Stars: interiors
White dwarfs
spellingShingle Ciencias Astronómicas
Stars: evolution
Stars: interiors
White dwarfs
Renedo, I.
Althaus, Leandro Gabriel
Miller Bertolami, Marcelo Miguel
Romero, A. D.
Córsico, Alejandro Hugo
Rohrmann, R.D.
García-Berro, E.
New cooling sequences for old white dwarfs
topic_facet Ciencias Astronómicas
Stars: evolution
Stars: interiors
White dwarfs
description 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 stellar masses 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.
format Articulo
Articulo
author Renedo, I.
Althaus, Leandro Gabriel
Miller Bertolami, Marcelo Miguel
Romero, A. D.
Córsico, Alejandro Hugo
Rohrmann, R.D.
García-Berro, E.
author_facet Renedo, I.
Althaus, Leandro Gabriel
Miller Bertolami, Marcelo Miguel
Romero, A. D.
Córsico, Alejandro Hugo
Rohrmann, R.D.
García-Berro, E.
author_sort Renedo, I.
title New cooling sequences for old white dwarfs
title_short New cooling sequences for old white dwarfs
title_full New cooling sequences for old white dwarfs
title_fullStr New cooling sequences for old white dwarfs
title_full_unstemmed New cooling sequences for old white dwarfs
title_sort new cooling sequences for old white dwarfs
publishDate 2010
url http://sedici.unlp.edu.ar/handle/10915/82493
work_keys_str_mv AT renedoi newcoolingsequencesforoldwhitedwarfs
AT althausleandrogabriel newcoolingsequencesforoldwhitedwarfs
AT millerbertolamimarcelomiguel newcoolingsequencesforoldwhitedwarfs
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AT corsicoalejandrohugo newcoolingsequencesforoldwhitedwarfs
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AT garciaberroe newcoolingsequencesforoldwhitedwarfs
bdutipo_str Repositorios
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