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
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/2055
Ver los metadatos del registro completo
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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) |
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openAccess |
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http://creativecommons.org/licenses/by-nc-nd/4.0/ Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0) |
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