The pulsational properties of ultra-massive DB white dwarfs with carbon-oxygen cores coming from single-star evolution

[Context] Ultra-massive white dwarfs are relevant for many reasons: Their role as type Ia supernova progenitors, the occurrence of physical processes in the asymptotic giant branch phase, the existence of high-field magnetic white dwarfs, and the occurrence of double white dwarf mergers. Some hydrog...

Descripción completa

Detalles Bibliográficos
Autores: Córsico, Alejandro H., Althaus, Leandro G., Gil Pons, Pilar, Torres, Santiago
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2021
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/262400
Acceso en línea:http://hdl.handle.net/10261/262400
Access Level:acceso abierto
Palabra clave:Stars: evolution
Stars: interiors
White dwarfs
Asteroseismology
Stars: oscillations
Dense matter
id ES_8036f65d204d8fbebb637faece65e2ba
oai_identifier_str oai:digital.csic.es:10261/262400
network_acronym_str ES
network_name_str España
repository_id_str
dc.title.none.fl_str_mv The pulsational properties of ultra-massive DB white dwarfs with carbon-oxygen cores coming from single-star evolution
title The pulsational properties of ultra-massive DB white dwarfs with carbon-oxygen cores coming from single-star evolution
spellingShingle The pulsational properties of ultra-massive DB white dwarfs with carbon-oxygen cores coming from single-star evolution
Córsico, Alejandro H.
Stars: evolution
Stars: interiors
White dwarfs
Asteroseismology
Stars: oscillations
Dense matter
title_short The pulsational properties of ultra-massive DB white dwarfs with carbon-oxygen cores coming from single-star evolution
title_full The pulsational properties of ultra-massive DB white dwarfs with carbon-oxygen cores coming from single-star evolution
title_fullStr The pulsational properties of ultra-massive DB white dwarfs with carbon-oxygen cores coming from single-star evolution
title_full_unstemmed The pulsational properties of ultra-massive DB white dwarfs with carbon-oxygen cores coming from single-star evolution
title_sort The pulsational properties of ultra-massive DB white dwarfs with carbon-oxygen cores coming from single-star evolution
dc.creator.none.fl_str_mv Córsico, Alejandro H.
Althaus, Leandro G.
Gil Pons, Pilar
Torres, Santiago
author Córsico, Alejandro H.
author_facet Córsico, Alejandro H.
Althaus, Leandro G.
Gil Pons, Pilar
Torres, Santiago
author_role author
author2 Althaus, Leandro G.
Gil Pons, Pilar
Torres, Santiago
author2_role author
author
author
dc.contributor.none.fl_str_mv Ministerio de Economía y Competitividad (España)
Universidad Nacional de La Plata
NASA
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Stars: evolution
Stars: interiors
White dwarfs
Asteroseismology
Stars: oscillations
Dense matter
topic Stars: evolution
Stars: interiors
White dwarfs
Asteroseismology
Stars: oscillations
Dense matter
description [Context] Ultra-massive white dwarfs are relevant for many reasons: Their role as type Ia supernova progenitors, the occurrence of physical processes in the asymptotic giant branch phase, the existence of high-field magnetic white dwarfs, and the occurrence of double white dwarf mergers. Some hydrogen-rich ultra-massive white dwarfs are pulsating stars and, as such, they offer the possibility of studying their interiors through asteroseismology. On the other hand, pulsating helium-rich ultra-massive white dwarfs could be even more attractive objects for asteroseismology if they were found, as they should be hotter and less crystallized than pulsating hydrogen-rich white dwarfs, something that would pave the way for probing their deep interiors. [Aims] We explore the pulsational properties of ultra-massive helium-rich white dwarfs with carbon-oxygen and oxygen-neon cores resulting from single stellar evolution. Our goal is to provide a theoretical basis that could eventually help to discern the core composition of ultra-massive white dwarfs and the scenario of their formation through asteroseismology, anticipating the possible future detection of pulsations in helium-rich ultra-massive white dwarfs. [Methods] We focus on three scenarios for the formation of helium-rich ultra-massive white dwarfs. First, we consider stellar models coming from two recently proposed single-star evolution scenarios for the formation of ultra-massive white dwarfs with carbon-oxygen cores that involve the rotation of the degenerate core after core helium burning and reduced mass-loss rates in massive asymptotic giant branch stars. Finally, we contemplate ultra-massive oxygen-neon core white-dwarf models resulting from standard single-star evolution. We compute the adiabatic pulsation gravity-mode periods for models in a range of effective temperatures, embracing the instability strip of average-mass pulsating helium-rich white dwarfs, and we compare the characteristics of the mode-Trapping properties for models of different formation scenarios through the analysis of the period spacing. [Results] Given that the white dwarf models coming from the three scenarios considered are characterized by distinct core chemical profiles, we find that their pulsation properties are also different, thus leading to distinctive signatures in the period-spacing and mode-Trapping properties. [Conclusions] Our results indicate that in the case of an eventual detection of pulsating ultra-massive helium-rich white dwarfs, it would be possible to derive valuable information encrypted in the core of these stars in connection with the origin of such exotic objects. This is of the utmost importance regarding recent evidence for the existence of a population of ultra-massive white dwarfs with carbon-oxygen cores. There will soon be many opportunities to detect pulsations in these stars through observations collected with ongoing space missions.
publishDate 2021
dc.date.none.fl_str_mv 2021
2022
2022
2022
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/262400
url http://hdl.handle.net/10261/262400
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/MINECO//AYA2014-59084-P
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2017-86274-P
http://doi.org/10.1051/0004-6361/202040001
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
_version_ 1869411882223271936
spelling The pulsational properties of ultra-massive DB white dwarfs with carbon-oxygen cores coming from single-star evolutionCórsico, Alejandro H.Althaus, Leandro G.Gil Pons, PilarTorres, SantiagoStars: evolutionStars: interiorsWhite dwarfsAsteroseismologyStars: oscillationsDense matter[Context] Ultra-massive white dwarfs are relevant for many reasons: Their role as type Ia supernova progenitors, the occurrence of physical processes in the asymptotic giant branch phase, the existence of high-field magnetic white dwarfs, and the occurrence of double white dwarf mergers. Some hydrogen-rich ultra-massive white dwarfs are pulsating stars and, as such, they offer the possibility of studying their interiors through asteroseismology. On the other hand, pulsating helium-rich ultra-massive white dwarfs could be even more attractive objects for asteroseismology if they were found, as they should be hotter and less crystallized than pulsating hydrogen-rich white dwarfs, something that would pave the way for probing their deep interiors. [Aims] We explore the pulsational properties of ultra-massive helium-rich white dwarfs with carbon-oxygen and oxygen-neon cores resulting from single stellar evolution. Our goal is to provide a theoretical basis that could eventually help to discern the core composition of ultra-massive white dwarfs and the scenario of their formation through asteroseismology, anticipating the possible future detection of pulsations in helium-rich ultra-massive white dwarfs. [Methods] We focus on three scenarios for the formation of helium-rich ultra-massive white dwarfs. First, we consider stellar models coming from two recently proposed single-star evolution scenarios for the formation of ultra-massive white dwarfs with carbon-oxygen cores that involve the rotation of the degenerate core after core helium burning and reduced mass-loss rates in massive asymptotic giant branch stars. Finally, we contemplate ultra-massive oxygen-neon core white-dwarf models resulting from standard single-star evolution. We compute the adiabatic pulsation gravity-mode periods for models in a range of effective temperatures, embracing the instability strip of average-mass pulsating helium-rich white dwarfs, and we compare the characteristics of the mode-Trapping properties for models of different formation scenarios through the analysis of the period spacing. [Results] Given that the white dwarf models coming from the three scenarios considered are characterized by distinct core chemical profiles, we find that their pulsation properties are also different, thus leading to distinctive signatures in the period-spacing and mode-Trapping properties. [Conclusions] Our results indicate that in the case of an eventual detection of pulsating ultra-massive helium-rich white dwarfs, it would be possible to derive valuable information encrypted in the core of these stars in connection with the origin of such exotic objects. This is of the utmost importance regarding recent evidence for the existence of a population of ultra-massive white dwarfs with carbon-oxygen cores. There will soon be many opportunities to detect pulsations in these stars through observations collected with ongoing space missions.Part of this work was supported by PIP 112-200801-00940 Grant from CONICET, by MINECO grants AYA2014-59084-P, and AYA2017-86274-P, by grant G149 from University of La Plata, and by the AGAUR grant SGR-661/201. This research has made use of NASA Astrophysics Data System.EDP SciencesMinisterio de Economía y Competitividad (España)Universidad Nacional de La PlataNASAConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2022202220212022info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/262400reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MINECO//AYA2014-59084-Pinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2017-86274-Phttp://doi.org/10.1051/0004-6361/202040001Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2624002026-05-22T06:33:51Z
score 15,811543

Similares en LA Referencia