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
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/2055
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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:UNLP2025-10-22T16:30:18Zoai: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:13292025-10-22 16:30:18.876SEDICI (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 |
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2001 |
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eng |
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eng |
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