The ages and colours of cool helium-core white dwarf stars
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,...
Guardado en:
| Autores principales: | , , |
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| Formato: | Articulo |
| Lenguaje: | Inglés |
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2001
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| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/2055 http://fcaglp.fcaglp.unlp.edu.ar/evolgroup/Papers/ARTICLES/2001/MNRAS_325_607_2001.pdf http://mnras.oxfordjournals.org/content/325/2/607 |
| Aporte de: |
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I19-R120-10915-2055 |
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| record_format |
dspace |
| institution |
Universidad Nacional de La Plata |
| institution_str |
I-19 |
| repository_str |
R-120 |
| collection |
SEDICI (UNLP) |
| language |
Inglés |
| topic |
Ciencias Astronómicas stars: atmospheres stars: evolution stars: fundamental parameters stars: interiors white dwarfs |
| spellingShingle |
Ciencias Astronómicas stars: atmospheres stars: evolution stars: fundamental parameters stars: interiors white dwarfs Serenelli, Aldo Marcelo Althaus, Leandro Gabriel Benvenuto, Omar Gustavo The ages and colours of cool helium-core white dwarf stars |
| topic_facet |
Ciencias Astronómicas stars: atmospheres stars: evolution stars: fundamental parameters stars: interiors white dwarfs |
| 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. |
| format |
Articulo Articulo |
| author |
Serenelli, Aldo Marcelo Althaus, Leandro Gabriel Benvenuto, Omar Gustavo |
| author_facet |
Serenelli, Aldo Marcelo Althaus, Leandro Gabriel Benvenuto, Omar Gustavo |
| author_sort |
Serenelli, Aldo Marcelo |
| title |
The ages and colours of cool helium-core white dwarf stars |
| 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 |
ages and colours of cool helium-core white dwarf stars |
| publishDate |
2001 |
| url |
http://sedici.unlp.edu.ar/handle/10915/2055 http://fcaglp.fcaglp.unlp.edu.ar/evolgroup/Papers/ARTICLES/2001/MNRAS_325_607_2001.pdf http://mnras.oxfordjournals.org/content/325/2/607 |
| work_keys_str_mv |
AT serenellialdomarcelo theagesandcoloursofcoolheliumcorewhitedwarfstars AT althausleandrogabriel theagesandcoloursofcoolheliumcorewhitedwarfstars AT benvenutoomargustavo theagesandcoloursofcoolheliumcorewhitedwarfstars AT serenellialdomarcelo agesandcoloursofcoolheliumcorewhitedwarfstars AT althausleandrogabriel agesandcoloursofcoolheliumcorewhitedwarfstars AT benvenutoomargustavo agesandcoloursofcoolheliumcorewhitedwarfstars |
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Repositorios |
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1764820464585146370 |