Modeling He-rich subdwarfs through the hot-flasher scenario
- Autores
- Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel; Unglaub, K.; Weiss, A.
- Año de publicación
- 2009
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present 1D numerical simulations aimed at studying the hot-flasher scenario for the formation of He-rich subdwarf stars. Sequences were calculated for a wide range of metallicities and with the He core flash at different points of the post-RGB evolution (i.e. different remnant masses). We followed the complete evolution from the ZAMS, through the hot-flasher event, and to the subdwarf stage for all kinds of hot-flashers. This allows us to present a homogeneous set of abundances for different metallicities and all flavors of hot-flashers. We extend the scope of our work by analyzing the effects in the predicted surface abundances of some standard assumptions in convective mixing and the effects of element diffusion. We find that the hot-flasher scenario is a viable explanation for the formation of He-sdO stars. Our results also show that element diffusion may produce the transformation of (post hot-flasher) He-rich atmospheres into He-deficient ones. If this is so, then the hot-flasher scenario is able to reproduce both the observed properties and distribution of He-sdO stars.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata - Materia
-
Ciencias Astronómicas
Estrellas Celestiales
Simulación - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/82797
Ver los metadatos del registro completo
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Modeling He-rich subdwarfs through the hot-flasher scenarioMiller Bertolami, Marcelo MiguelAlthaus, Leandro GabrielUnglaub, K.Weiss, A.Ciencias AstronómicasEstrellas CelestialesSimulaciónWe present 1D numerical simulations aimed at studying the hot-flasher scenario for the formation of He-rich subdwarf stars. Sequences were calculated for a wide range of metallicities and with the He core flash at different points of the post-RGB evolution (i.e. different remnant masses). We followed the complete evolution from the ZAMS, through the hot-flasher event, and to the subdwarf stage for all kinds of hot-flashers. This allows us to present a homogeneous set of abundances for different metallicities and all flavors of hot-flashers. We extend the scope of our work by analyzing the effects in the predicted surface abundances of some standard assumptions in convective mixing and the effects of element diffusion. We find that the hot-flasher scenario is a viable explanation for the formation of He-sdO stars. Our results also show that element diffusion may produce the transformation of (post hot-flasher) He-rich atmospheres into He-deficient ones. If this is so, then the hot-flasher scenario is able to reproduce both the observed properties and distribution of He-sdO stars.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2009info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/82797enginfo:eu-repo/semantics/altIdentifier/issn/1742-6588info:eu-repo/semantics/altIdentifier/doi/10.1088/1742-6596/172/1/012014info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:15:36Zoai:sedici.unlp.edu.ar:10915/82797Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:15:37.078SEDICI (UNLP) - Universidad Nacional de La Platafalse |
| dc.title.none.fl_str_mv |
Modeling He-rich subdwarfs through the hot-flasher scenario |
| title |
Modeling He-rich subdwarfs through the hot-flasher scenario |
| spellingShingle |
Modeling He-rich subdwarfs through the hot-flasher scenario Miller Bertolami, Marcelo Miguel Ciencias Astronómicas Estrellas Celestiales Simulación |
| title_short |
Modeling He-rich subdwarfs through the hot-flasher scenario |
| title_full |
Modeling He-rich subdwarfs through the hot-flasher scenario |
| title_fullStr |
Modeling He-rich subdwarfs through the hot-flasher scenario |
| title_full_unstemmed |
Modeling He-rich subdwarfs through the hot-flasher scenario |
| title_sort |
Modeling He-rich subdwarfs through the hot-flasher scenario |
| dc.creator.none.fl_str_mv |
Miller Bertolami, Marcelo Miguel Althaus, Leandro Gabriel Unglaub, K. Weiss, A. |
| author |
Miller Bertolami, Marcelo Miguel |
| author_facet |
Miller Bertolami, Marcelo Miguel Althaus, Leandro Gabriel Unglaub, K. Weiss, A. |
| author_role |
author |
| author2 |
Althaus, Leandro Gabriel Unglaub, K. Weiss, A. |
| author2_role |
author author author |
| dc.subject.none.fl_str_mv |
Ciencias Astronómicas Estrellas Celestiales Simulación |
| topic |
Ciencias Astronómicas Estrellas Celestiales Simulación |
| dc.description.none.fl_txt_mv |
We present 1D numerical simulations aimed at studying the hot-flasher scenario for the formation of He-rich subdwarf stars. Sequences were calculated for a wide range of metallicities and with the He core flash at different points of the post-RGB evolution (i.e. different remnant masses). We followed the complete evolution from the ZAMS, through the hot-flasher event, and to the subdwarf stage for all kinds of hot-flashers. This allows us to present a homogeneous set of abundances for different metallicities and all flavors of hot-flashers. We extend the scope of our work by analyzing the effects in the predicted surface abundances of some standard assumptions in convective mixing and the effects of element diffusion. We find that the hot-flasher scenario is a viable explanation for the formation of He-sdO stars. Our results also show that element diffusion may produce the transformation of (post hot-flasher) He-rich atmospheres into He-deficient ones. If this is so, then the hot-flasher scenario is able to reproduce both the observed properties and distribution of He-sdO stars. Facultad de Ciencias Astronómicas y Geofísicas Instituto de Astrofísica de La Plata |
| description |
We present 1D numerical simulations aimed at studying the hot-flasher scenario for the formation of He-rich subdwarf stars. Sequences were calculated for a wide range of metallicities and with the He core flash at different points of the post-RGB evolution (i.e. different remnant masses). We followed the complete evolution from the ZAMS, through the hot-flasher event, and to the subdwarf stage for all kinds of hot-flashers. This allows us to present a homogeneous set of abundances for different metallicities and all flavors of hot-flashers. We extend the scope of our work by analyzing the effects in the predicted surface abundances of some standard assumptions in convective mixing and the effects of element diffusion. We find that the hot-flasher scenario is a viable explanation for the formation of He-sdO stars. Our results also show that element diffusion may produce the transformation of (post hot-flasher) He-rich atmospheres into He-deficient ones. If this is so, then the hot-flasher scenario is able to reproduce both the observed properties and distribution of He-sdO stars. |
| publishDate |
2009 |
| dc.date.none.fl_str_mv |
2009 |
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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 |
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publishedVersion |
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http://sedici.unlp.edu.ar/handle/10915/82797 |
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http://sedici.unlp.edu.ar/handle/10915/82797 |
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eng |
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eng |
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info:eu-repo/semantics/altIdentifier/issn/1742-6588 info:eu-repo/semantics/altIdentifier/doi/10.1088/1742-6596/172/1/012014 |
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openAccess |
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