Fingering convection in accreting hydrogen white dwarfs
- Autores
- Wachlin, Felipe Carlos; Vauclair, Sylvie; Vauclair, G.; Althaus, Leandro Gabriel
- Año de publicación
- 2019
- Idioma
- español castellano
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- The accretion of heavy material from debris disk on the surface of hydrogen-rich white dwarfs induces a double diffusivity instability known as the fingering convection. It leads to an efficient extra mixing which brings the accreted material deeper in the star than by considering only mixing in the surface dynamical convection zone, in a time scale much shorter than that of gravitational settling. We performed numerical simulations of a continuous accretion of heavy material having a bulk Earth composition on the two well studied DAZ and ZZ Ceti pulsators GD 133 and G 29-38. We find that the existence of fingering convection implies much larger accretion rates to explain the observed abundances than previous estimates based on the standard mixing length theory and gravitational settling only.
Instituto de Astrofísica de La Plata - Materia
-
Ciencias Astronómicas
Física
White dwarfs
Standard mixing length theory
Thermohaline convection - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by/4.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/123832
Ver los metadatos del registro completo
id |
SEDICI_73b87a71e976d9ead47b9418205bc6b4 |
---|---|
oai_identifier_str |
oai:sedici.unlp.edu.ar:10915/123832 |
network_acronym_str |
SEDICI |
repository_id_str |
1329 |
network_name_str |
SEDICI (UNLP) |
spelling |
Fingering convection in accreting hydrogen white dwarfsWachlin, Felipe CarlosVauclair, SylvieVauclair, G.Althaus, Leandro GabrielCiencias AstronómicasFísicaWhite dwarfsStandard mixing length theoryThermohaline convectionThe accretion of heavy material from debris disk on the surface of hydrogen-rich white dwarfs induces a double diffusivity instability known as the fingering convection. It leads to an efficient extra mixing which brings the accreted material deeper in the star than by considering only mixing in the surface dynamical convection zone, in a time scale much shorter than that of gravitational settling. We performed numerical simulations of a continuous accretion of heavy material having a bulk Earth composition on the two well studied DAZ and ZZ Ceti pulsators GD 133 and G 29-38. We find that the existence of fingering convection implies much larger accretion rates to explain the observed abundances than previous estimates based on the standard mixing length theory and gravitational settling only.Instituto de Astrofísica de La Plata2019-06-21info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf183-187http://sedici.unlp.edu.ar/handle/10915/123832spainfo:eu-repo/semantics/altIdentifier/issn/1633-4760info:eu-repo/semantics/altIdentifier/issn/1638-1963info:eu-repo/semantics/altIdentifier/doi/10.1051/eas/1982018info: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:UNLP2025-09-29T11:29:24Zoai:sedici.unlp.edu.ar:10915/123832Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:29:24.786SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
Fingering convection in accreting hydrogen white dwarfs |
title |
Fingering convection in accreting hydrogen white dwarfs |
spellingShingle |
Fingering convection in accreting hydrogen white dwarfs Wachlin, Felipe Carlos Ciencias Astronómicas Física White dwarfs Standard mixing length theory Thermohaline convection |
title_short |
Fingering convection in accreting hydrogen white dwarfs |
title_full |
Fingering convection in accreting hydrogen white dwarfs |
title_fullStr |
Fingering convection in accreting hydrogen white dwarfs |
title_full_unstemmed |
Fingering convection in accreting hydrogen white dwarfs |
title_sort |
Fingering convection in accreting hydrogen white dwarfs |
dc.creator.none.fl_str_mv |
Wachlin, Felipe Carlos Vauclair, Sylvie Vauclair, G. Althaus, Leandro Gabriel |
author |
Wachlin, Felipe Carlos |
author_facet |
Wachlin, Felipe Carlos Vauclair, Sylvie Vauclair, G. Althaus, Leandro Gabriel |
author_role |
author |
author2 |
Vauclair, Sylvie Vauclair, G. Althaus, Leandro Gabriel |
author2_role |
author author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas Física White dwarfs Standard mixing length theory Thermohaline convection |
topic |
Ciencias Astronómicas Física White dwarfs Standard mixing length theory Thermohaline convection |
dc.description.none.fl_txt_mv |
The accretion of heavy material from debris disk on the surface of hydrogen-rich white dwarfs induces a double diffusivity instability known as the fingering convection. It leads to an efficient extra mixing which brings the accreted material deeper in the star than by considering only mixing in the surface dynamical convection zone, in a time scale much shorter than that of gravitational settling. We performed numerical simulations of a continuous accretion of heavy material having a bulk Earth composition on the two well studied DAZ and ZZ Ceti pulsators GD 133 and G 29-38. We find that the existence of fingering convection implies much larger accretion rates to explain the observed abundances than previous estimates based on the standard mixing length theory and gravitational settling only. Instituto de Astrofísica de La Plata |
description |
The accretion of heavy material from debris disk on the surface of hydrogen-rich white dwarfs induces a double diffusivity instability known as the fingering convection. It leads to an efficient extra mixing which brings the accreted material deeper in the star than by considering only mixing in the surface dynamical convection zone, in a time scale much shorter than that of gravitational settling. We performed numerical simulations of a continuous accretion of heavy material having a bulk Earth composition on the two well studied DAZ and ZZ Ceti pulsators GD 133 and G 29-38. We find that the existence of fingering convection implies much larger accretion rates to explain the observed abundances than previous estimates based on the standard mixing length theory and gravitational settling only. |
publishDate |
2019 |
dc.date.none.fl_str_mv |
2019-06-21 |
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 |
format |
article |
status_str |
publishedVersion |
dc.identifier.none.fl_str_mv |
http://sedici.unlp.edu.ar/handle/10915/123832 |
url |
http://sedici.unlp.edu.ar/handle/10915/123832 |
dc.language.none.fl_str_mv |
spa |
language |
spa |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/issn/1633-4760 info:eu-repo/semantics/altIdentifier/issn/1638-1963 info:eu-repo/semantics/altIdentifier/doi/10.1051/eas/1982018 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/4.0/ Creative Commons Attribution 4.0 International (CC BY 4.0) |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
http://creativecommons.org/licenses/by/4.0/ Creative Commons Attribution 4.0 International (CC BY 4.0) |
dc.format.none.fl_str_mv |
application/pdf 183-187 |
dc.source.none.fl_str_mv |
reponame:SEDICI (UNLP) instname:Universidad Nacional de La Plata instacron:UNLP |
reponame_str |
SEDICI (UNLP) |
collection |
SEDICI (UNLP) |
instname_str |
Universidad Nacional de La Plata |
instacron_str |
UNLP |
institution |
UNLP |
repository.name.fl_str_mv |
SEDICI (UNLP) - Universidad Nacional de La Plata |
repository.mail.fl_str_mv |
alira@sedici.unlp.edu.ar |
_version_ |
1844616173254082560 |
score |
13.070432 |