Evolutionary and pulsational properties of low-mass white dwarf stars with oxygen cores resulting from close binary evolution

Autores
Althaus, Leandro Gabriel; Córsico, Alejandro Hugo; Gautschy, A.; Han, Z.; Serenelli, Aldo Marcelo; Panei, Jorge Alejandro
Año de publicación
2004
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The present work is designed to explore the evolutionary and pulsational properties of low-mass white dwarfs with carbon/oxygen cores. In particular, we follow the evolution of a 0.33-M⊙ white dwarf remnant in a self-consistent way with the predictions of nuclear burning, element diffusion and the history of the white dwarf progenitor. Attention is focused on the occurrence of hydrogen shell flashes induced by diffusion processes during cooling phases. The evolutionary stages prior to the white dwarf formation are also fully accounted for by computing the conservative binary evolution of an initially 2.5-M⊙ Population I star with a 1.25-M ⊙ companion, and with period Pi = 3d. Evolution is followed down to the domain of the ZZ Ceti stars on the white dwarf cooling branch. We find that chemical diffusion induces the occurrence of an additional hydrogen thermonuclear flash, which leads to stellar models with thin hydrogen envelopes. As a result, a fast cooling is encountered at advanced stages of evolution. In addition, we explore the adiabatic pulsational properties of the resulting white dwarf models. As compared with their helium-core counterparts, low-mass oxygen-core white dwarfs are characterized by a pulsational spectrum much more featured, an aspect which could eventually be used for distinguishing both types of stars, if low-mass white dwarfs were in fact found to pulsate as ZZ Ceti-type variables. Finally, we perform a non-adiabatic pulsational analysis on the resulting carbon/oxygen low-mass white dwarf models.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
Binaries: general
Stars: evolution
Stars: interiors
Stars: oscillations
White dwarfs
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/84476

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repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Evolutionary and pulsational properties of low-mass white dwarf stars with oxygen cores resulting from close binary evolutionAlthaus, Leandro GabrielCórsico, Alejandro HugoGautschy, A.Han, Z.Serenelli, Aldo MarceloPanei, Jorge AlejandroCiencias AstronómicasBinaries: generalStars: evolutionStars: interiorsStars: oscillationsWhite dwarfsThe present work is designed to explore the evolutionary and pulsational properties of low-mass white dwarfs with carbon/oxygen cores. In particular, we follow the evolution of a 0.33-M⊙ white dwarf remnant in a self-consistent way with the predictions of nuclear burning, element diffusion and the history of the white dwarf progenitor. Attention is focused on the occurrence of hydrogen shell flashes induced by diffusion processes during cooling phases. The evolutionary stages prior to the white dwarf formation are also fully accounted for by computing the conservative binary evolution of an initially 2.5-M⊙ Population I star with a 1.25-M ⊙ companion, and with period P<SUB>i</SUB> = 3d. Evolution is followed down to the domain of the ZZ Ceti stars on the white dwarf cooling branch. We find that chemical diffusion induces the occurrence of an additional hydrogen thermonuclear flash, which leads to stellar models with thin hydrogen envelopes. As a result, a fast cooling is encountered at advanced stages of evolution. In addition, we explore the adiabatic pulsational properties of the resulting white dwarf models. As compared with their helium-core counterparts, low-mass oxygen-core white dwarfs are characterized by a pulsational spectrum much more featured, an aspect which could eventually be used for distinguishing both types of stars, if low-mass white dwarfs were in fact found to pulsate as ZZ Ceti-type variables. Finally, we perform a non-adiabatic pulsational analysis on the resulting carbon/oxygen low-mass white dwarf models.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2004info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf125-136http://sedici.unlp.edu.ar/handle/10915/84476enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2004.07183.xinfo: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:UNLP2025-09-29T11:16:15Zoai:sedici.unlp.edu.ar:10915/84476Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:15.447SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Evolutionary and pulsational properties of low-mass white dwarf stars with oxygen cores resulting from close binary evolution
title Evolutionary and pulsational properties of low-mass white dwarf stars with oxygen cores resulting from close binary evolution
spellingShingle Evolutionary and pulsational properties of low-mass white dwarf stars with oxygen cores resulting from close binary evolution
Althaus, Leandro Gabriel
Ciencias Astronómicas
Binaries: general
Stars: evolution
Stars: interiors
Stars: oscillations
White dwarfs
title_short Evolutionary and pulsational properties of low-mass white dwarf stars with oxygen cores resulting from close binary evolution
title_full Evolutionary and pulsational properties of low-mass white dwarf stars with oxygen cores resulting from close binary evolution
title_fullStr Evolutionary and pulsational properties of low-mass white dwarf stars with oxygen cores resulting from close binary evolution
title_full_unstemmed Evolutionary and pulsational properties of low-mass white dwarf stars with oxygen cores resulting from close binary evolution
title_sort Evolutionary and pulsational properties of low-mass white dwarf stars with oxygen cores resulting from close binary evolution
dc.creator.none.fl_str_mv Althaus, Leandro Gabriel
Córsico, Alejandro Hugo
Gautschy, A.
Han, Z.
Serenelli, Aldo Marcelo
Panei, Jorge Alejandro
author Althaus, Leandro Gabriel
author_facet Althaus, Leandro Gabriel
Córsico, Alejandro Hugo
Gautschy, A.
Han, Z.
Serenelli, Aldo Marcelo
Panei, Jorge Alejandro
author_role author
author2 Córsico, Alejandro Hugo
Gautschy, A.
Han, Z.
Serenelli, Aldo Marcelo
Panei, Jorge Alejandro
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Binaries: general
Stars: evolution
Stars: interiors
Stars: oscillations
White dwarfs
topic Ciencias Astronómicas
Binaries: general
Stars: evolution
Stars: interiors
Stars: oscillations
White dwarfs
dc.description.none.fl_txt_mv The present work is designed to explore the evolutionary and pulsational properties of low-mass white dwarfs with carbon/oxygen cores. In particular, we follow the evolution of a 0.33-M⊙ white dwarf remnant in a self-consistent way with the predictions of nuclear burning, element diffusion and the history of the white dwarf progenitor. Attention is focused on the occurrence of hydrogen shell flashes induced by diffusion processes during cooling phases. The evolutionary stages prior to the white dwarf formation are also fully accounted for by computing the conservative binary evolution of an initially 2.5-M⊙ Population I star with a 1.25-M ⊙ companion, and with period P<SUB>i</SUB> = 3d. Evolution is followed down to the domain of the ZZ Ceti stars on the white dwarf cooling branch. We find that chemical diffusion induces the occurrence of an additional hydrogen thermonuclear flash, which leads to stellar models with thin hydrogen envelopes. As a result, a fast cooling is encountered at advanced stages of evolution. In addition, we explore the adiabatic pulsational properties of the resulting white dwarf models. As compared with their helium-core counterparts, low-mass oxygen-core white dwarfs are characterized by a pulsational spectrum much more featured, an aspect which could eventually be used for distinguishing both types of stars, if low-mass white dwarfs were in fact found to pulsate as ZZ Ceti-type variables. Finally, we perform a non-adiabatic pulsational analysis on the resulting carbon/oxygen low-mass white dwarf models.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
description The present work is designed to explore the evolutionary and pulsational properties of low-mass white dwarfs with carbon/oxygen cores. In particular, we follow the evolution of a 0.33-M⊙ white dwarf remnant in a self-consistent way with the predictions of nuclear burning, element diffusion and the history of the white dwarf progenitor. Attention is focused on the occurrence of hydrogen shell flashes induced by diffusion processes during cooling phases. The evolutionary stages prior to the white dwarf formation are also fully accounted for by computing the conservative binary evolution of an initially 2.5-M⊙ Population I star with a 1.25-M ⊙ companion, and with period P<SUB>i</SUB> = 3d. Evolution is followed down to the domain of the ZZ Ceti stars on the white dwarf cooling branch. We find that chemical diffusion induces the occurrence of an additional hydrogen thermonuclear flash, which leads to stellar models with thin hydrogen envelopes. As a result, a fast cooling is encountered at advanced stages of evolution. In addition, we explore the adiabatic pulsational properties of the resulting white dwarf models. As compared with their helium-core counterparts, low-mass oxygen-core white dwarfs are characterized by a pulsational spectrum much more featured, an aspect which could eventually be used for distinguishing both types of stars, if low-mass white dwarfs were in fact found to pulsate as ZZ Ceti-type variables. Finally, we perform a non-adiabatic pulsational analysis on the resulting carbon/oxygen low-mass white dwarf models.
publishDate 2004
dc.date.none.fl_str_mv 2004
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/84476
url http://sedici.unlp.edu.ar/handle/10915/84476
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0035-8711
info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2004.07183.x
dc.rights.none.fl_str_mv 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)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
125-136
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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