The formation of DA white dwarfs with thin hydrogen envelopes
- Autores
- Althaus, Leandro Gabriel; Miller Bertolami, Marcelo Miguel; Córsico, Alejandro Hugo; García Berro, E.; Gil-Pons, P.
- Año de publicación
- 2005
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- 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 M⊙ 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 M⊙ in agreement with asteroseismological inferences for some ZZ Ceti stars.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata - Materia
-
Ciencias Astronómicas
Stars: abundances
Stars: AGB stars: interiors
Stars: evolution
Stars: oscillations
Stars: white dwarfs - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/83410
Ver los metadatos del registro completo
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The formation of DA white dwarfs with thin hydrogen envelopesAlthaus, Leandro GabrielMiller Bertolami, Marcelo MiguelCórsico, Alejandro HugoGarcía Berro, E.Gil-Pons, P.Ciencias AstronómicasStars: abundancesStars: AGB stars: interiorsStars: evolutionStars: oscillationsStars: white dwarfsWe 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 M⊙ 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 M⊙ in agreement with asteroseismological inferences for some ZZ Ceti stars.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2005info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfL1-L4http://sedici.unlp.edu.ar/handle/10915/83410enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:200500159info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-10-22T16:56:37Zoai:sedici.unlp.edu.ar:10915/83410Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-10-22 16:56:37.512SEDICI (UNLP) - Universidad Nacional de La Platafalse |
| dc.title.none.fl_str_mv |
The formation of DA white dwarfs with thin hydrogen envelopes |
| title |
The formation of DA white dwarfs with thin hydrogen envelopes |
| spellingShingle |
The formation of DA white dwarfs with thin hydrogen envelopes Althaus, Leandro Gabriel Ciencias Astronómicas Stars: abundances Stars: AGB stars: interiors Stars: evolution Stars: oscillations Stars: white dwarfs |
| title_short |
The formation of DA white dwarfs with thin hydrogen envelopes |
| title_full |
The formation of DA white dwarfs with thin hydrogen envelopes |
| title_fullStr |
The formation of DA white dwarfs with thin hydrogen envelopes |
| title_full_unstemmed |
The formation of DA white dwarfs with thin hydrogen envelopes |
| title_sort |
The formation of DA white dwarfs with thin hydrogen envelopes |
| dc.creator.none.fl_str_mv |
Althaus, Leandro Gabriel Miller Bertolami, Marcelo Miguel Córsico, Alejandro Hugo García Berro, E. Gil-Pons, P. |
| author |
Althaus, Leandro Gabriel |
| author_facet |
Althaus, Leandro Gabriel Miller Bertolami, Marcelo Miguel Córsico, Alejandro Hugo García Berro, E. Gil-Pons, P. |
| author_role |
author |
| author2 |
Miller Bertolami, Marcelo Miguel Córsico, Alejandro Hugo García Berro, E. Gil-Pons, P. |
| author2_role |
author author author author |
| dc.subject.none.fl_str_mv |
Ciencias Astronómicas Stars: abundances Stars: AGB stars: interiors Stars: evolution Stars: oscillations Stars: white dwarfs |
| topic |
Ciencias Astronómicas Stars: abundances Stars: AGB stars: interiors Stars: evolution Stars: oscillations Stars: white dwarfs |
| dc.description.none.fl_txt_mv |
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 M⊙ 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 M⊙ in agreement with asteroseismological inferences for some ZZ Ceti stars. Facultad de Ciencias Astronómicas y Geofísicas Instituto de Astrofísica de La Plata |
| description |
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 M⊙ 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 M⊙ in agreement with asteroseismological inferences for some ZZ Ceti stars. |
| publishDate |
2005 |
| dc.date.none.fl_str_mv |
2005 |
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info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion Articulo http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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http://sedici.unlp.edu.ar/handle/10915/83410 |
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eng |
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eng |
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info:eu-repo/semantics/altIdentifier/issn/0004-6361 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:200500159 |
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info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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