Evolution of DB white dwarfs in the Canuto and Mazzitelli theory of convection
- Autores
- Althaus, Leandro Gabriel; Benvenuto, Omar Gustavo
- Año de publicación
- 1996
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We compute the evolution of DB (helium-rich envelope) white dwarf models with masses between 0.4 and 1 Mo and metallicities of Z=O.OOI and 0.004, taking into account Canuto & Mazzitelli's new theory of convection. This theory, which has no free parameters and includes the full spectrum of turbulent eddies, has been successfully tested in different stellar objects and represents a substantial improvement compared with the classical mixing length theory used in most white dwarf studies. Using thermal time-scales we find that, for the range of masses and metallicities assumed in this study, the Canuto & Mazzitelli theory yields theoretical blue edges between 24 200 and 25 600 K, which is in good agreement with observations of pulsating DB white dwarfs. Calculations are performed considering the mixing length theory as well. In this context, our results are consistent with previous computations.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Astronomía
convection
stars: evolution
white dwarfs - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/141312
Ver los metadatos del registro completo
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Evolution of DB white dwarfs in the Canuto and Mazzitelli theory of convectionAlthaus, Leandro GabrielBenvenuto, Omar GustavoAstronomíaconvectionstars: evolutionwhite dwarfsWe compute the evolution of DB (helium-rich envelope) white dwarf models with masses between 0.4 and 1 Mo and metallicities of Z=O.OOI and 0.004, taking into account Canuto & Mazzitelli's new theory of convection. This theory, which has no free parameters and includes the full spectrum of turbulent eddies, has been successfully tested in different stellar objects and represents a substantial improvement compared with the classical mixing length theory used in most white dwarf studies. Using thermal time-scales we find that, for the range of masses and metallicities assumed in this study, the Canuto & Mazzitelli theory yields theoretical blue edges between 24 200 and 25 600 K, which is in good agreement with observations of pulsating DB white dwarfs. Calculations are performed considering the mixing length theory as well. In this context, our results are consistent with previous computations.Facultad de Ciencias Astronómicas y Geofísicas1996-02-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf981-984http://sedici.unlp.edu.ar/handle/10915/141312enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/issn/1365-2966info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/278.4.981info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/4.0/Creative Commons Attribution 4.0 International (CC BY 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:31:57Zoai:sedici.unlp.edu.ar:10915/141312Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:31:57.388SEDICI (UNLP) - Universidad Nacional de La Platafalse |
| dc.title.none.fl_str_mv |
Evolution of DB white dwarfs in the Canuto and Mazzitelli theory of convection |
| title |
Evolution of DB white dwarfs in the Canuto and Mazzitelli theory of convection |
| spellingShingle |
Evolution of DB white dwarfs in the Canuto and Mazzitelli theory of convection Althaus, Leandro Gabriel Astronomía convection stars: evolution white dwarfs |
| title_short |
Evolution of DB white dwarfs in the Canuto and Mazzitelli theory of convection |
| title_full |
Evolution of DB white dwarfs in the Canuto and Mazzitelli theory of convection |
| title_fullStr |
Evolution of DB white dwarfs in the Canuto and Mazzitelli theory of convection |
| title_full_unstemmed |
Evolution of DB white dwarfs in the Canuto and Mazzitelli theory of convection |
| title_sort |
Evolution of DB white dwarfs in the Canuto and Mazzitelli theory of convection |
| dc.creator.none.fl_str_mv |
Althaus, Leandro Gabriel Benvenuto, Omar Gustavo |
| author |
Althaus, Leandro Gabriel |
| author_facet |
Althaus, Leandro Gabriel Benvenuto, Omar Gustavo |
| author_role |
author |
| author2 |
Benvenuto, Omar Gustavo |
| author2_role |
author |
| dc.subject.none.fl_str_mv |
Astronomía convection stars: evolution white dwarfs |
| topic |
Astronomía convection stars: evolution white dwarfs |
| dc.description.none.fl_txt_mv |
We compute the evolution of DB (helium-rich envelope) white dwarf models with masses between 0.4 and 1 Mo and metallicities of Z=O.OOI and 0.004, taking into account Canuto & Mazzitelli's new theory of convection. This theory, which has no free parameters and includes the full spectrum of turbulent eddies, has been successfully tested in different stellar objects and represents a substantial improvement compared with the classical mixing length theory used in most white dwarf studies. Using thermal time-scales we find that, for the range of masses and metallicities assumed in this study, the Canuto & Mazzitelli theory yields theoretical blue edges between 24 200 and 25 600 K, which is in good agreement with observations of pulsating DB white dwarfs. Calculations are performed considering the mixing length theory as well. In this context, our results are consistent with previous computations. Facultad de Ciencias Astronómicas y Geofísicas |
| description |
We compute the evolution of DB (helium-rich envelope) white dwarf models with masses between 0.4 and 1 Mo and metallicities of Z=O.OOI and 0.004, taking into account Canuto & Mazzitelli's new theory of convection. This theory, which has no free parameters and includes the full spectrum of turbulent eddies, has been successfully tested in different stellar objects and represents a substantial improvement compared with the classical mixing length theory used in most white dwarf studies. Using thermal time-scales we find that, for the range of masses and metallicities assumed in this study, the Canuto & Mazzitelli theory yields theoretical blue edges between 24 200 and 25 600 K, which is in good agreement with observations of pulsating DB white dwarfs. Calculations are performed considering the mixing length theory as well. In this context, our results are consistent with previous computations. |
| publishDate |
1996 |
| dc.date.none.fl_str_mv |
1996-02-11 |
| 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 |
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article |
| status_str |
publishedVersion |
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http://sedici.unlp.edu.ar/handle/10915/141312 |
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| dc.language.none.fl_str_mv |
eng |
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eng |
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info:eu-repo/semantics/altIdentifier/issn/0035-8711 info:eu-repo/semantics/altIdentifier/issn/1365-2966 info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/278.4.981 |
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info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/4.0/ Creative Commons Attribution 4.0 International (CC BY 4.0) |
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openAccess |
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