The ages and colours of cool helium-core white dwarf stars

Autores
Serenelli, Aldo Marcelo; Althaus, Leandro Gabriel; Benvenuto, Omar Gustavo
Año de publicación
2001
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The purpose of this work is to explore the evolution of helium-core white dwarf stars in a self-consistent way with the predictions of detailed non-grey model atmospheres and element diffusion. To this end, we consider helium-core white dwarf models with stellar masses of 0.406, 0.360, 0.327, 0.292, 0.242, 0.196 and 0.169 Msolar and follow their evolution from the end of mass-loss episodes, during their pre-white dwarf evolution, down to very low surface luminosities. We find that when the effective temperature decreases below 4000K, the emergent spectrum of these stars becomes bluer within time-scales of astrophysical interest. In particular, we analyse the evolution of our models in the colour-colour and in the colour-magnitude diagrams and find that helium-core white dwarfs with masses ranging from ~0.18 to 0.3Msolar can reach the turn-off in their colours and become blue again within cooling times much less than 15Gyr and then remain brighter than MV~16.5. In view of these results, many low-mass helium white dwarfs could have had enough time to evolve to the domain of collision-induced absorption from molecular hydrogen, showing blue colours.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
stars: atmospheres
stars: evolution
stars: fundamental parameters
stars: interiors
white dwarfs
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-nd/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/2055

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/2055
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling The ages and colours of cool helium-core white dwarf starsSerenelli, Aldo MarceloAlthaus, Leandro GabrielBenvenuto, Omar GustavoCiencias Astronómicasstars: atmospheresstars: evolutionstars: fundamental parametersstars: interiorswhite dwarfsThe purpose of this work is to explore the evolution of helium-core white dwarf stars in a self-consistent way with the predictions of detailed non-grey model atmospheres and element diffusion. To this end, we consider helium-core white dwarf models with stellar masses of 0.406, 0.360, 0.327, 0.292, 0.242, 0.196 and 0.169 Msolar and follow their evolution from the end of mass-loss episodes, during their pre-white dwarf evolution, down to very low surface luminosities. We find that when the effective temperature decreases below 4000K, the emergent spectrum of these stars becomes bluer within time-scales of astrophysical interest. In particular, we analyse the evolution of our models in the colour-colour and in the colour-magnitude diagrams and find that helium-core white dwarfs with masses ranging from ~0.18 to 0.3Msolar can reach the turn-off in their colours and become blue again within cooling times much less than 15Gyr and then remain brighter than MV~16.5. In view of these results, many low-mass helium white dwarfs could have had enough time to evolve to the domain of collision-induced absorption from molecular hydrogen, showing blue colours.Facultad de Ciencias Astronómicas y Geofísicas2001info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf607-616http://sedici.unlp.edu.ar/handle/10915/2055enginfo:eu-repo/semantics/altIdentifier/url/http://fcaglp.fcaglp.unlp.edu.ar/evolgroup/Papers/ARTICLES/2001/MNRAS_325_607_2001.pdfinfo:eu-repo/semantics/altIdentifier/url/http://mnras.oxfordjournals.org/content/325/2/607info:eu-repo/semantics/altIdentifier/issn/1365-2966info:eu-repo/semantics/altIdentifier/doi/10.1046/j.1365-8711.2001.04449.xinfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-nd/4.0/Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T10:48:37Zoai:sedici.unlp.edu.ar:10915/2055Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 10:48:38.92SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv The ages and colours of cool helium-core white dwarf stars
title The ages and colours of cool helium-core white dwarf stars
spellingShingle The ages and colours of cool helium-core white dwarf stars
Serenelli, Aldo Marcelo
Ciencias Astronómicas
stars: atmospheres
stars: evolution
stars: fundamental parameters
stars: interiors
white dwarfs
title_short The ages and colours of cool helium-core white dwarf stars
title_full The ages and colours of cool helium-core white dwarf stars
title_fullStr The ages and colours of cool helium-core white dwarf stars
title_full_unstemmed The ages and colours of cool helium-core white dwarf stars
title_sort The ages and colours of cool helium-core white dwarf stars
dc.creator.none.fl_str_mv Serenelli, Aldo Marcelo
Althaus, Leandro Gabriel
Benvenuto, Omar Gustavo
author Serenelli, Aldo Marcelo
author_facet Serenelli, Aldo Marcelo
Althaus, Leandro Gabriel
Benvenuto, Omar Gustavo
author_role author
author2 Althaus, Leandro Gabriel
Benvenuto, Omar Gustavo
author2_role author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
stars: atmospheres
stars: evolution
stars: fundamental parameters
stars: interiors
white dwarfs
topic Ciencias Astronómicas
stars: atmospheres
stars: evolution
stars: fundamental parameters
stars: interiors
white dwarfs
dc.description.none.fl_txt_mv The purpose of this work is to explore the evolution of helium-core white dwarf stars in a self-consistent way with the predictions of detailed non-grey model atmospheres and element diffusion. To this end, we consider helium-core white dwarf models with stellar masses of 0.406, 0.360, 0.327, 0.292, 0.242, 0.196 and 0.169 Msolar and follow their evolution from the end of mass-loss episodes, during their pre-white dwarf evolution, down to very low surface luminosities. We find that when the effective temperature decreases below 4000K, the emergent spectrum of these stars becomes bluer within time-scales of astrophysical interest. In particular, we analyse the evolution of our models in the colour-colour and in the colour-magnitude diagrams and find that helium-core white dwarfs with masses ranging from ~0.18 to 0.3Msolar can reach the turn-off in their colours and become blue again within cooling times much less than 15Gyr and then remain brighter than MV~16.5. In view of these results, many low-mass helium white dwarfs could have had enough time to evolve to the domain of collision-induced absorption from molecular hydrogen, showing blue colours.
Facultad de Ciencias Astronómicas y Geofísicas
description The purpose of this work is to explore the evolution of helium-core white dwarf stars in a self-consistent way with the predictions of detailed non-grey model atmospheres and element diffusion. To this end, we consider helium-core white dwarf models with stellar masses of 0.406, 0.360, 0.327, 0.292, 0.242, 0.196 and 0.169 Msolar and follow their evolution from the end of mass-loss episodes, during their pre-white dwarf evolution, down to very low surface luminosities. We find that when the effective temperature decreases below 4000K, the emergent spectrum of these stars becomes bluer within time-scales of astrophysical interest. In particular, we analyse the evolution of our models in the colour-colour and in the colour-magnitude diagrams and find that helium-core white dwarfs with masses ranging from ~0.18 to 0.3Msolar can reach the turn-off in their colours and become blue again within cooling times much less than 15Gyr and then remain brighter than MV~16.5. In view of these results, many low-mass helium white dwarfs could have had enough time to evolve to the domain of collision-induced absorption from molecular hydrogen, showing blue colours.
publishDate 2001
dc.date.none.fl_str_mv 2001
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/10915/2055
url http://sedici.unlp.edu.ar/handle/10915/2055
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://fcaglp.fcaglp.unlp.edu.ar/evolgroup/Papers/ARTICLES/2001/MNRAS_325_607_2001.pdf
info:eu-repo/semantics/altIdentifier/url/http://mnras.oxfordjournals.org/content/325/2/607
info:eu-repo/semantics/altIdentifier/issn/1365-2966
info:eu-repo/semantics/altIdentifier/doi/10.1046/j.1365-8711.2001.04449.x
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-nd/4.0/
Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-nd/4.0/
Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)
dc.format.none.fl_str_mv application/pdf
607-616
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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