Quiescent nuclear burning in low-metallicity white dwarfs
- Autores
- Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel; Garcia Berro, E.
- Año de publicación
- 2013
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We discuss the impact of residual nuclear burning in the cooling sequences of hydrogen-rich (DA) white dwarfs with very low metallicity progenitors (Z = 0.0001). These cooling sequences are appropriate for the study of very old stellar populations. The results presented here are the product of self-consistent, fully evolutionary calculations. Specifically, we follow the evolution of white dwarf progenitors from the zero-age main sequence through all the evolutionary phases, namely the core hydrogen-burning phase, the helium-burning phase, and the thermally pulsing asymptotic giant branch phase to the white dwarf stage. This is done for the most relevant range of main-sequence masses, covering the most usual interval of white dwarf masses—from 0.53 M ☉ to 0.83 M ☉. Due to the low metallicity of the progenitor stars, white dwarfs are born with thicker hydrogen envelopes, leading to more intense hydrogen burning shells as compared with their solar metallicity counterparts. We study the phase in which nuclear reactions are still important and find that nuclear energy sources play a key role during long periods of time, considerably increasing the cooling times from those predicted by standard white dwarf models. In particular, we find that for this metallicity and for white dwarf masses smaller than about 0.6 M ☉, nuclear reactions are the main contributor to the stellar luminosity for luminosities as low as log (L/L ☉) sime –3.2. This, in turn, should have a noticeable impact in the white dwarf luminosity function of low-metallicity stellar populations.
Fil: Miller Bertolami, Marcelo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Althaus, Leandro Gabriel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Garcia Berro, E.. Universidad Politecnica de Catalunya; España. Institute for Space Studies of Catalonia; España - Materia
-
Stellar Evolution
White Dwarfs - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/8487
Ver los metadatos del registro completo
id |
CONICETDig_d50840dd54bb41285da738a8f2b1c733 |
---|---|
oai_identifier_str |
oai:ri.conicet.gov.ar:11336/8487 |
network_acronym_str |
CONICETDig |
repository_id_str |
3498 |
network_name_str |
CONICET Digital (CONICET) |
spelling |
Quiescent nuclear burning in low-metallicity white dwarfsMiller Bertolami, Marcelo MiguelAlthaus, Leandro GabrielGarcia Berro, E.Stellar EvolutionWhite Dwarfshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We discuss the impact of residual nuclear burning in the cooling sequences of hydrogen-rich (DA) white dwarfs with very low metallicity progenitors (Z = 0.0001). These cooling sequences are appropriate for the study of very old stellar populations. The results presented here are the product of self-consistent, fully evolutionary calculations. Specifically, we follow the evolution of white dwarf progenitors from the zero-age main sequence through all the evolutionary phases, namely the core hydrogen-burning phase, the helium-burning phase, and the thermally pulsing asymptotic giant branch phase to the white dwarf stage. This is done for the most relevant range of main-sequence masses, covering the most usual interval of white dwarf masses—from 0.53 M ☉ to 0.83 M ☉. Due to the low metallicity of the progenitor stars, white dwarfs are born with thicker hydrogen envelopes, leading to more intense hydrogen burning shells as compared with their solar metallicity counterparts. We study the phase in which nuclear reactions are still important and find that nuclear energy sources play a key role during long periods of time, considerably increasing the cooling times from those predicted by standard white dwarf models. In particular, we find that for this metallicity and for white dwarf masses smaller than about 0.6 M ☉, nuclear reactions are the main contributor to the stellar luminosity for luminosities as low as log (L/L ☉) sime –3.2. This, in turn, should have a noticeable impact in the white dwarf luminosity function of low-metallicity stellar populations.Fil: Miller Bertolami, Marcelo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Althaus, Leandro Gabriel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Garcia Berro, E.. Universidad Politecnica de Catalunya; España. Institute for Space Studies of Catalonia; EspañaIOP Publishing2013-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/8487Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel; Garcia Berro, E.; Quiescent nuclear burning in low-metallicity white dwarfs; IOP Publishing; Astrophysical Journal; 775; 1; 9-2013; 22-262041-8205enginfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/2041-8205/775/1/L22/metainfo:eu-repo/semantics/altIdentifier/doi/10.1088/2041-8205/775/1/L22info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:14:55Zoai:ri.conicet.gov.ar:11336/8487instacron: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:34982025-10-22 11:14:56.164CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Quiescent nuclear burning in low-metallicity white dwarfs |
title |
Quiescent nuclear burning in low-metallicity white dwarfs |
spellingShingle |
Quiescent nuclear burning in low-metallicity white dwarfs Miller Bertolami, Marcelo Miguel Stellar Evolution White Dwarfs |
title_short |
Quiescent nuclear burning in low-metallicity white dwarfs |
title_full |
Quiescent nuclear burning in low-metallicity white dwarfs |
title_fullStr |
Quiescent nuclear burning in low-metallicity white dwarfs |
title_full_unstemmed |
Quiescent nuclear burning in low-metallicity white dwarfs |
title_sort |
Quiescent nuclear burning in low-metallicity white dwarfs |
dc.creator.none.fl_str_mv |
Miller Bertolami, Marcelo Miguel Althaus, Leandro Gabriel Garcia Berro, E. |
author |
Miller Bertolami, Marcelo Miguel |
author_facet |
Miller Bertolami, Marcelo Miguel Althaus, Leandro Gabriel Garcia Berro, E. |
author_role |
author |
author2 |
Althaus, Leandro Gabriel Garcia Berro, E. |
author2_role |
author author |
dc.subject.none.fl_str_mv |
Stellar Evolution White Dwarfs |
topic |
Stellar Evolution White Dwarfs |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
We discuss the impact of residual nuclear burning in the cooling sequences of hydrogen-rich (DA) white dwarfs with very low metallicity progenitors (Z = 0.0001). These cooling sequences are appropriate for the study of very old stellar populations. The results presented here are the product of self-consistent, fully evolutionary calculations. Specifically, we follow the evolution of white dwarf progenitors from the zero-age main sequence through all the evolutionary phases, namely the core hydrogen-burning phase, the helium-burning phase, and the thermally pulsing asymptotic giant branch phase to the white dwarf stage. This is done for the most relevant range of main-sequence masses, covering the most usual interval of white dwarf masses—from 0.53 M ☉ to 0.83 M ☉. Due to the low metallicity of the progenitor stars, white dwarfs are born with thicker hydrogen envelopes, leading to more intense hydrogen burning shells as compared with their solar metallicity counterparts. We study the phase in which nuclear reactions are still important and find that nuclear energy sources play a key role during long periods of time, considerably increasing the cooling times from those predicted by standard white dwarf models. In particular, we find that for this metallicity and for white dwarf masses smaller than about 0.6 M ☉, nuclear reactions are the main contributor to the stellar luminosity for luminosities as low as log (L/L ☉) sime –3.2. This, in turn, should have a noticeable impact in the white dwarf luminosity function of low-metallicity stellar populations. Fil: Miller Bertolami, Marcelo Miguel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Althaus, Leandro Gabriel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina Fil: Garcia Berro, E.. Universidad Politecnica de Catalunya; España. Institute for Space Studies of Catalonia; España |
description |
We discuss the impact of residual nuclear burning in the cooling sequences of hydrogen-rich (DA) white dwarfs with very low metallicity progenitors (Z = 0.0001). These cooling sequences are appropriate for the study of very old stellar populations. The results presented here are the product of self-consistent, fully evolutionary calculations. Specifically, we follow the evolution of white dwarf progenitors from the zero-age main sequence through all the evolutionary phases, namely the core hydrogen-burning phase, the helium-burning phase, and the thermally pulsing asymptotic giant branch phase to the white dwarf stage. This is done for the most relevant range of main-sequence masses, covering the most usual interval of white dwarf masses—from 0.53 M ☉ to 0.83 M ☉. Due to the low metallicity of the progenitor stars, white dwarfs are born with thicker hydrogen envelopes, leading to more intense hydrogen burning shells as compared with their solar metallicity counterparts. We study the phase in which nuclear reactions are still important and find that nuclear energy sources play a key role during long periods of time, considerably increasing the cooling times from those predicted by standard white dwarf models. In particular, we find that for this metallicity and for white dwarf masses smaller than about 0.6 M ☉, nuclear reactions are the main contributor to the stellar luminosity for luminosities as low as log (L/L ☉) sime –3.2. This, in turn, should have a noticeable impact in the white dwarf luminosity function of low-metallicity stellar populations. |
publishDate |
2013 |
dc.date.none.fl_str_mv |
2013-09 |
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/11336/8487 Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel; Garcia Berro, E.; Quiescent nuclear burning in low-metallicity white dwarfs; IOP Publishing; Astrophysical Journal; 775; 1; 9-2013; 22-26 2041-8205 |
url |
http://hdl.handle.net/11336/8487 |
identifier_str_mv |
Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel; Garcia Berro, E.; Quiescent nuclear burning in low-metallicity white dwarfs; IOP Publishing; Astrophysical Journal; 775; 1; 9-2013; 22-26 2041-8205 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/2041-8205/775/1/L22/meta info:eu-repo/semantics/altIdentifier/doi/10.1088/2041-8205/775/1/L22 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
IOP Publishing |
publisher.none.fl_str_mv |
IOP Publishing |
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 |
_version_ |
1846781575888371712 |
score |
12.982451 |