The evolution of ultra-massive carbon-oxygen white dwarfs

Autores
Camisassa, María Eugenia; Althaus, Leandro Gabriel; Koester, Detlev; Torres, Santiago; Pons, Pilar Gil; Corsico, Alejandro Hugo
Año de publicación
2022
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Ultra-massive white dwarfs ( M WD1 . 05 M ) are considered powerful tools to study Type Ia supernovae explosions, merger events, the occurrence of physical processes in the superasymptotic giant branch phase, and the existence of high magnetic fields. Traditionally, ultra-massive white dwarfs are expected to harbour oxygen-neon (ONe) cores. However, new observations and recent theoretical studies suggest that the progenitors of some ultra-massive white dwarfs can avoid carbon burning, leading to the formation of ultra-massive white dwarfs harbouring carbon-oxygen (CO) cores. Here, we present a set of ultra-massive white dwarf evolutionary sequences with CO cores for a wide range of metallicity and masses. We take into account the energy released by latent heat and phase separation during the crystallization process and by 22Ne sedimentation. Realistic chemical profiles resulting from the full computation of progenitor evolution are considered. We compare our CO ultra-massive white dwarf models with ONe models. We conclude that CO ultra-massive white dwarfs evolve significantly slower than their ONe counterparts mainly for three reasons: their larger thermal content, the effect of crystallization, and the effect of 22Ne sedimentation. We also provide colours in several photometric bands on the basis of new model atmospheres. These CO ultra-massive white dwarf models, together with the ONe ultra-massive white dwarf models, provide an appropriate theoretical framework to study the ultra-massive white dwarf population in our Galaxy.
Fil: Camisassa, María Eugenia. State University of Colorado at Boulder; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Althaus, Leandro Gabriel. Universidad Nacional de La Plata; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Koester, Detlev. Christian Albrechts Universitat Zu Kiel; Alemania
Fil: Torres, Santiago. Christian Albrechts Universitat Zu Kiel; Alemania
Fil: Pons, Pilar Gil. Universidad Politécnica de Catalunya; España
Fil: Corsico, Alejandro Hugo. Instituto de Estudios Espaciales de Cataluña; España. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Materia
STARS: EVOLUTION
STARS: INTERIOR
WHITE DWARFS
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/211932
Acceder
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network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The evolution of ultra-massive carbon-oxygen white dwarfsCamisassa, María EugeniaAlthaus, Leandro GabrielKoester, DetlevTorres, SantiagoPons, Pilar GilCorsico, Alejandro HugoSTARS: EVOLUTIONSTARS: INTERIORWHITE DWARFShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Ultra-massive white dwarfs ( M WD1 . 05 M ) are considered powerful tools to study Type Ia supernovae explosions, merger events, the occurrence of physical processes in the superasymptotic giant branch phase, and the existence of high magnetic fields. Traditionally, ultra-massive white dwarfs are expected to harbour oxygen-neon (ONe) cores. However, new observations and recent theoretical studies suggest that the progenitors of some ultra-massive white dwarfs can avoid carbon burning, leading to the formation of ultra-massive white dwarfs harbouring carbon-oxygen (CO) cores. Here, we present a set of ultra-massive white dwarf evolutionary sequences with CO cores for a wide range of metallicity and masses. We take into account the energy released by latent heat and phase separation during the crystallization process and by 22Ne sedimentation. Realistic chemical profiles resulting from the full computation of progenitor evolution are considered. We compare our CO ultra-massive white dwarf models with ONe models. We conclude that CO ultra-massive white dwarfs evolve significantly slower than their ONe counterparts mainly for three reasons: their larger thermal content, the effect of crystallization, and the effect of 22Ne sedimentation. We also provide colours in several photometric bands on the basis of new model atmospheres. These CO ultra-massive white dwarf models, together with the ONe ultra-massive white dwarf models, provide an appropriate theoretical framework to study the ultra-massive white dwarf population in our Galaxy.Fil: Camisassa, María Eugenia. State University of Colorado at Boulder; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Althaus, Leandro Gabriel. Universidad Nacional de La Plata; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Koester, Detlev. Christian Albrechts Universitat Zu Kiel; AlemaniaFil: Torres, Santiago. Christian Albrechts Universitat Zu Kiel; AlemaniaFil: Pons, Pilar Gil. Universidad Politécnica de Catalunya; EspañaFil: Corsico, Alejandro Hugo. Instituto de Estudios Espaciales de Cataluña; España. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaWiley Blackwell Publishing, Inc2022-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/211932Camisassa, María Eugenia; Althaus, Leandro Gabriel; Koester, Detlev; Torres, Santiago; Pons, Pilar Gil; et al.; The evolution of ultra-massive carbon-oxygen white dwarfs; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 511; 4; 4-2022; 5198-52060035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/511/4/5198/6540971info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stac348info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2202.03495v2info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:39:29Zoai:ri.conicet.gov.ar:11336/211932instacron: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 09:39:29.731CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The evolution of ultra-massive carbon-oxygen white dwarfs
title The evolution of ultra-massive carbon-oxygen white dwarfs
spellingShingle The evolution of ultra-massive carbon-oxygen white dwarfs
Camisassa, María Eugenia
STARS: EVOLUTION
STARS: INTERIOR
WHITE DWARFS
title_short The evolution of ultra-massive carbon-oxygen white dwarfs
title_full The evolution of ultra-massive carbon-oxygen white dwarfs
title_fullStr The evolution of ultra-massive carbon-oxygen white dwarfs
title_full_unstemmed The evolution of ultra-massive carbon-oxygen white dwarfs
title_sort The evolution of ultra-massive carbon-oxygen white dwarfs
dc.creator.none.fl_str_mv Camisassa, María Eugenia
Althaus, Leandro Gabriel
Koester, Detlev
Torres, Santiago
Pons, Pilar Gil
Corsico, Alejandro Hugo
author Camisassa, María Eugenia
author_facet Camisassa, María Eugenia
Althaus, Leandro Gabriel
Koester, Detlev
Torres, Santiago
Pons, Pilar Gil
Corsico, Alejandro Hugo
author_role author
author2 Althaus, Leandro Gabriel
Koester, Detlev
Torres, Santiago
Pons, Pilar Gil
Corsico, Alejandro Hugo
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv STARS: EVOLUTION
STARS: INTERIOR
WHITE DWARFS
topic STARS: EVOLUTION
STARS: INTERIOR
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 Ultra-massive white dwarfs ( M WD1 . 05 M ) are considered powerful tools to study Type Ia supernovae explosions, merger events, the occurrence of physical processes in the superasymptotic giant branch phase, and the existence of high magnetic fields. Traditionally, ultra-massive white dwarfs are expected to harbour oxygen-neon (ONe) cores. However, new observations and recent theoretical studies suggest that the progenitors of some ultra-massive white dwarfs can avoid carbon burning, leading to the formation of ultra-massive white dwarfs harbouring carbon-oxygen (CO) cores. Here, we present a set of ultra-massive white dwarf evolutionary sequences with CO cores for a wide range of metallicity and masses. We take into account the energy released by latent heat and phase separation during the crystallization process and by 22Ne sedimentation. Realistic chemical profiles resulting from the full computation of progenitor evolution are considered. We compare our CO ultra-massive white dwarf models with ONe models. We conclude that CO ultra-massive white dwarfs evolve significantly slower than their ONe counterparts mainly for three reasons: their larger thermal content, the effect of crystallization, and the effect of 22Ne sedimentation. We also provide colours in several photometric bands on the basis of new model atmospheres. These CO ultra-massive white dwarf models, together with the ONe ultra-massive white dwarf models, provide an appropriate theoretical framework to study the ultra-massive white dwarf population in our Galaxy.
Fil: Camisassa, María Eugenia. State University of Colorado at Boulder; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Althaus, Leandro Gabriel. Universidad Nacional de La Plata; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Koester, Detlev. Christian Albrechts Universitat Zu Kiel; Alemania
Fil: Torres, Santiago. Christian Albrechts Universitat Zu Kiel; Alemania
Fil: Pons, Pilar Gil. Universidad Politécnica de Catalunya; España
Fil: Corsico, Alejandro Hugo. Instituto de Estudios Espaciales de Cataluña; España. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
description Ultra-massive white dwarfs ( M WD1 . 05 M ) are considered powerful tools to study Type Ia supernovae explosions, merger events, the occurrence of physical processes in the superasymptotic giant branch phase, and the existence of high magnetic fields. Traditionally, ultra-massive white dwarfs are expected to harbour oxygen-neon (ONe) cores. However, new observations and recent theoretical studies suggest that the progenitors of some ultra-massive white dwarfs can avoid carbon burning, leading to the formation of ultra-massive white dwarfs harbouring carbon-oxygen (CO) cores. Here, we present a set of ultra-massive white dwarf evolutionary sequences with CO cores for a wide range of metallicity and masses. We take into account the energy released by latent heat and phase separation during the crystallization process and by 22Ne sedimentation. Realistic chemical profiles resulting from the full computation of progenitor evolution are considered. We compare our CO ultra-massive white dwarf models with ONe models. We conclude that CO ultra-massive white dwarfs evolve significantly slower than their ONe counterparts mainly for three reasons: their larger thermal content, the effect of crystallization, and the effect of 22Ne sedimentation. We also provide colours in several photometric bands on the basis of new model atmospheres. These CO ultra-massive white dwarf models, together with the ONe ultra-massive white dwarf models, provide an appropriate theoretical framework to study the ultra-massive white dwarf population in our Galaxy.
publishDate 2022
dc.date.none.fl_str_mv 2022-04
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/11336/211932
Camisassa, María Eugenia; Althaus, Leandro Gabriel; Koester, Detlev; Torres, Santiago; Pons, Pilar Gil; et al.; The evolution of ultra-massive carbon-oxygen white dwarfs; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 511; 4; 4-2022; 5198-5206
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/211932
identifier_str_mv Camisassa, María Eugenia; Althaus, Leandro Gabriel; Koester, Detlev; Torres, Santiago; Pons, Pilar Gil; et al.; The evolution of ultra-massive carbon-oxygen white dwarfs; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 511; 4; 4-2022; 5198-5206
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/511/4/5198/6540971
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stac348
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2202.03495v2
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
application/pdf
dc.publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
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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