The impact of chemical differentiation of white dwarfs on thermonuclear supernovae
- Autores
- Bravo, Eduardo; Althaus, Leandro Gabriel; García Berro, Enrique; Domínguez, Inmaculada
- Año de publicación
- 2011
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Aims. Gravitational settling of 22Ne in cooling white dwarfs can affect the outcome of thermonuclear supernovae. We investigate how the supernova energetics and nucleosynthesis are in turn influenced by this process. We use realistic chemical profiles derived from state-of-the-art white dwarf cooling sequences. The cooling sequences provide a link between the white dwarf chemical structure and the age of the supernova progenitor system. Methods. The cooling sequence of a 1 M⊙ white dwarf was computed until freezing using an up-to-date stellar evolutionary code. We computed explosions of both Chandrasekhar mass and sub-Chandrasekhar mass white dwarfs, assuming spherical symmetry and neglecting convective mixing during the pre-supernova carbon simmering phase to maximize the effects of chemical separation. Results. Neither gravitational settling of 22Ne nor chemical differentiation of 12C and 16O have an appreciable impact on the properties of type Ia supernovae, unless there is a direct dependence of the flame properties (density of transition from deflagration to detonation) on the chemical composition. At a fixed transition density, the maximum variation in the supernova magnitude obtained from progenitors of different ages is ~0.06 mag, and even assuming an unrealistically large diffusion coefficient of 22Ne it would be less than ~0.09 mag. However, if the transition density depends on the chemical composition (all other things being equal) the oldest SNIa can be as much as 0.4 mag brighter than the youngest ones (in our models the age difference is 7.4 Gyr). In addition, our results show that 22Ne sedimentation cannot be invoked to account for the formation of a central core of stable neutron-rich Fe-group nuclei in the ejecta of sub-Chandrasekhar models, as required by observations of type Ia supernovae.
Fil: Bravo, Eduardo. Universidad Politecnica de Catalunya; España
Fil: Althaus, Leandro Gabriel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Universidad Politecnica de Catalunya; España. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina
Fil: García Berro, Enrique. Universidad Politecnica de Catalunya; España. Institut d’Estudis Espacials de Catalunya; España
Fil: Domínguez, Inmaculada. Universidad de Granada; España - Materia
-
White dwarfs
Disfusion
Supernovae
Star evolution - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/10288
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oai:ri.conicet.gov.ar:11336/10288 |
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The impact of chemical differentiation of white dwarfs on thermonuclear supernovaeBravo, EduardoAlthaus, Leandro GabrielGarcía Berro, EnriqueDomínguez, InmaculadaWhite dwarfsDisfusionSupernovaeStar evolutionhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. Gravitational settling of 22Ne in cooling white dwarfs can affect the outcome of thermonuclear supernovae. We investigate how the supernova energetics and nucleosynthesis are in turn influenced by this process. We use realistic chemical profiles derived from state-of-the-art white dwarf cooling sequences. The cooling sequences provide a link between the white dwarf chemical structure and the age of the supernova progenitor system. Methods. The cooling sequence of a 1 M⊙ white dwarf was computed until freezing using an up-to-date stellar evolutionary code. We computed explosions of both Chandrasekhar mass and sub-Chandrasekhar mass white dwarfs, assuming spherical symmetry and neglecting convective mixing during the pre-supernova carbon simmering phase to maximize the effects of chemical separation. Results. Neither gravitational settling of 22Ne nor chemical differentiation of 12C and 16O have an appreciable impact on the properties of type Ia supernovae, unless there is a direct dependence of the flame properties (density of transition from deflagration to detonation) on the chemical composition. At a fixed transition density, the maximum variation in the supernova magnitude obtained from progenitors of different ages is ~0.06 mag, and even assuming an unrealistically large diffusion coefficient of 22Ne it would be less than ~0.09 mag. However, if the transition density depends on the chemical composition (all other things being equal) the oldest SNIa can be as much as 0.4 mag brighter than the youngest ones (in our models the age difference is 7.4 Gyr). In addition, our results show that 22Ne sedimentation cannot be invoked to account for the formation of a central core of stable neutron-rich Fe-group nuclei in the ejecta of sub-Chandrasekhar models, as required by observations of type Ia supernovae.Fil: Bravo, Eduardo. Universidad Politecnica de Catalunya; EspañaFil: Althaus, Leandro Gabriel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Universidad Politecnica de Catalunya; España. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; ArgentinaFil: García Berro, Enrique. Universidad Politecnica de Catalunya; España. Institut d’Estudis Espacials de Catalunya; EspañaFil: Domínguez, Inmaculada. Universidad de Granada; EspañaEdp Sciences2011-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/10288Bravo, Eduardo; Althaus, Leandro Gabriel; García Berro, Enrique; Domínguez, Inmaculada; The impact of chemical differentiation of white dwarfs on thermonuclear supernovae; Edp Sciences; Astronomy And Astrophysics; 526; 2-2011; 26-340004-6361enginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201015506info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2011/02/aa15506-10/aa15506-10.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:40:48Zoai:ri.conicet.gov.ar:11336/10288instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 09:40:48.311CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
The impact of chemical differentiation of white dwarfs on thermonuclear supernovae |
title |
The impact of chemical differentiation of white dwarfs on thermonuclear supernovae |
spellingShingle |
The impact of chemical differentiation of white dwarfs on thermonuclear supernovae Bravo, Eduardo White dwarfs Disfusion Supernovae Star evolution |
title_short |
The impact of chemical differentiation of white dwarfs on thermonuclear supernovae |
title_full |
The impact of chemical differentiation of white dwarfs on thermonuclear supernovae |
title_fullStr |
The impact of chemical differentiation of white dwarfs on thermonuclear supernovae |
title_full_unstemmed |
The impact of chemical differentiation of white dwarfs on thermonuclear supernovae |
title_sort |
The impact of chemical differentiation of white dwarfs on thermonuclear supernovae |
dc.creator.none.fl_str_mv |
Bravo, Eduardo Althaus, Leandro Gabriel García Berro, Enrique Domínguez, Inmaculada |
author |
Bravo, Eduardo |
author_facet |
Bravo, Eduardo Althaus, Leandro Gabriel García Berro, Enrique Domínguez, Inmaculada |
author_role |
author |
author2 |
Althaus, Leandro Gabriel García Berro, Enrique Domínguez, Inmaculada |
author2_role |
author author author |
dc.subject.none.fl_str_mv |
White dwarfs Disfusion Supernovae Star evolution |
topic |
White dwarfs Disfusion Supernovae Star evolution |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Aims. Gravitational settling of 22Ne in cooling white dwarfs can affect the outcome of thermonuclear supernovae. We investigate how the supernova energetics and nucleosynthesis are in turn influenced by this process. We use realistic chemical profiles derived from state-of-the-art white dwarf cooling sequences. The cooling sequences provide a link between the white dwarf chemical structure and the age of the supernova progenitor system. Methods. The cooling sequence of a 1 M⊙ white dwarf was computed until freezing using an up-to-date stellar evolutionary code. We computed explosions of both Chandrasekhar mass and sub-Chandrasekhar mass white dwarfs, assuming spherical symmetry and neglecting convective mixing during the pre-supernova carbon simmering phase to maximize the effects of chemical separation. Results. Neither gravitational settling of 22Ne nor chemical differentiation of 12C and 16O have an appreciable impact on the properties of type Ia supernovae, unless there is a direct dependence of the flame properties (density of transition from deflagration to detonation) on the chemical composition. At a fixed transition density, the maximum variation in the supernova magnitude obtained from progenitors of different ages is ~0.06 mag, and even assuming an unrealistically large diffusion coefficient of 22Ne it would be less than ~0.09 mag. However, if the transition density depends on the chemical composition (all other things being equal) the oldest SNIa can be as much as 0.4 mag brighter than the youngest ones (in our models the age difference is 7.4 Gyr). In addition, our results show that 22Ne sedimentation cannot be invoked to account for the formation of a central core of stable neutron-rich Fe-group nuclei in the ejecta of sub-Chandrasekhar models, as required by observations of type Ia supernovae. Fil: Bravo, Eduardo. Universidad Politecnica de Catalunya; España Fil: Althaus, Leandro Gabriel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Universidad Politecnica de Catalunya; España. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina Fil: García Berro, Enrique. Universidad Politecnica de Catalunya; España. Institut d’Estudis Espacials de Catalunya; España Fil: Domínguez, Inmaculada. Universidad de Granada; España |
description |
Aims. Gravitational settling of 22Ne in cooling white dwarfs can affect the outcome of thermonuclear supernovae. We investigate how the supernova energetics and nucleosynthesis are in turn influenced by this process. We use realistic chemical profiles derived from state-of-the-art white dwarf cooling sequences. The cooling sequences provide a link between the white dwarf chemical structure and the age of the supernova progenitor system. Methods. The cooling sequence of a 1 M⊙ white dwarf was computed until freezing using an up-to-date stellar evolutionary code. We computed explosions of both Chandrasekhar mass and sub-Chandrasekhar mass white dwarfs, assuming spherical symmetry and neglecting convective mixing during the pre-supernova carbon simmering phase to maximize the effects of chemical separation. Results. Neither gravitational settling of 22Ne nor chemical differentiation of 12C and 16O have an appreciable impact on the properties of type Ia supernovae, unless there is a direct dependence of the flame properties (density of transition from deflagration to detonation) on the chemical composition. At a fixed transition density, the maximum variation in the supernova magnitude obtained from progenitors of different ages is ~0.06 mag, and even assuming an unrealistically large diffusion coefficient of 22Ne it would be less than ~0.09 mag. However, if the transition density depends on the chemical composition (all other things being equal) the oldest SNIa can be as much as 0.4 mag brighter than the youngest ones (in our models the age difference is 7.4 Gyr). In addition, our results show that 22Ne sedimentation cannot be invoked to account for the formation of a central core of stable neutron-rich Fe-group nuclei in the ejecta of sub-Chandrasekhar models, as required by observations of type Ia supernovae. |
publishDate |
2011 |
dc.date.none.fl_str_mv |
2011-02 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion 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://hdl.handle.net/11336/10288 Bravo, Eduardo; Althaus, Leandro Gabriel; García Berro, Enrique; Domínguez, Inmaculada; The impact of chemical differentiation of white dwarfs on thermonuclear supernovae; Edp Sciences; Astronomy And Astrophysics; 526; 2-2011; 26-34 0004-6361 |
url |
http://hdl.handle.net/11336/10288 |
identifier_str_mv |
Bravo, Eduardo; Althaus, Leandro Gabriel; García Berro, Enrique; Domínguez, Inmaculada; The impact of chemical differentiation of white dwarfs on thermonuclear supernovae; Edp Sciences; Astronomy And Astrophysics; 526; 2-2011; 26-34 0004-6361 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201015506 info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2011/02/aa15506-10/aa15506-10.html |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
Edp Sciences |
publisher.none.fl_str_mv |
Edp Sciences |
dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
reponame_str |
CONICET Digital (CONICET) |
collection |
CONICET Digital (CONICET) |
instname_str |
Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.name.fl_str_mv |
CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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13.070432 |