Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs

Autores
de Gerónimo, Francisco César; Miller Bertolami, Marcelo Miguel; Battich, Tiara; Tang, Xiaodong; Catelan, Márcio; Corsico, Alejandro Hugo; Li, Yunjun; Fang, Xiao; Althaus, Leandro Gabriel
Año de publicación
2024
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Recent determinations of the total rate of the 12 C+12 C nuclear reaction show non-negligible differences with thereference reaction rate commonly used in previous stellar simulations. In addition, the current uncertainties indetermining each exit channel constitute one of the main uncertainties in shaping the inner structure of superasymptotic giant branch stars that could have a measurable impact on the properties of pulsating ultramassive whitedwarfs (WDs). We explore how new determinations of the nuclear reaction rate and its branching ratios affect theevolution of WD progenitors. We show that the current uncertainties in the branching ratios constitute the mainuncertainty factor in determining the inner composition of ultramassive WDs and their progenitors. We found thatthe use of extreme branching ratios leads to differences in the central abundances of 20Ne of at most 17%, whichare translated into differences of at most 1.3% and 0.8% in the cooling times and size of the crystallized core,respectively. However, the impact on the pulsation properties is small, less than 1 s for the asymptotic periodspacing. We found that the carbon burns partially in the interior of ultramassive WD progenitors within a particularrange of masses, leaving a hybrid CONe-core composition in their cores. The evolution of these new kinds ofpredicted objects differs substantially from the evolution of objects with pure CO cores. Differences in the size ofthe crystallized core and cooling times of up to 15% and 6%, respectively, lead to distinct patterns in the periodspacing distribution.
Fil: de Gerónimo, Francisco César. 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: Miller Bertolami, Marcelo Miguel. 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: Battich, Tiara. 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. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Tang, Xiaodong. Chinese Academy of Sciences; República de China
Fil: Catelan, Márcio. Pontificia Universidad Católica de Chile; Chile. Millennium Institute of Astrophysics; Chile
Fil: Corsico, Alejandro Hugo. 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: Li, Yunjun. China Institute of Atomic Energy; China
Fil: Fang, Xiao. Sun Yat-sen University; China
Fil: Althaus, Leandro Gabriel. 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
DA stars
Nuclear abundances
Stellar evolution
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/257176
Acceder
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network_acronym_str CONICETDig
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network_name_str CONICET Digital (CONICET)
spelling Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfsde Gerónimo, Francisco CésarMiller Bertolami, Marcelo MiguelBattich, TiaraTang, XiaodongCatelan, MárcioCorsico, Alejandro HugoLi, YunjunFang, XiaoAlthaus, Leandro GabrielDA starsNuclear abundancesStellar evolutionhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Recent determinations of the total rate of the 12 C+12 C nuclear reaction show non-negligible differences with thereference reaction rate commonly used in previous stellar simulations. In addition, the current uncertainties indetermining each exit channel constitute one of the main uncertainties in shaping the inner structure of superasymptotic giant branch stars that could have a measurable impact on the properties of pulsating ultramassive whitedwarfs (WDs). We explore how new determinations of the nuclear reaction rate and its branching ratios affect theevolution of WD progenitors. We show that the current uncertainties in the branching ratios constitute the mainuncertainty factor in determining the inner composition of ultramassive WDs and their progenitors. We found thatthe use of extreme branching ratios leads to differences in the central abundances of 20Ne of at most 17%, whichare translated into differences of at most 1.3% and 0.8% in the cooling times and size of the crystallized core,respectively. However, the impact on the pulsation properties is small, less than 1 s for the asymptotic periodspacing. We found that the carbon burns partially in the interior of ultramassive WD progenitors within a particularrange of masses, leaving a hybrid CONe-core composition in their cores. The evolution of these new kinds ofpredicted objects differs substantially from the evolution of objects with pure CO cores. Differences in the size ofthe crystallized core and cooling times of up to 15% and 6%, respectively, lead to distinct patterns in the periodspacing distribution.Fil: de Gerónimo, Francisco César. 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: Miller Bertolami, Marcelo Miguel. 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: Battich, Tiara. 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. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; AlemaniaFil: Tang, Xiaodong. Chinese Academy of Sciences; República de ChinaFil: Catelan, Márcio. Pontificia Universidad Católica de Chile; Chile. Millennium Institute of Astrophysics; ChileFil: Corsico, Alejandro Hugo. 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: Li, Yunjun. China Institute of Atomic Energy; ChinaFil: Fang, Xiao. Sun Yat-sen University; ChinaFil: Althaus, Leandro Gabriel. 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; ArgentinaIOP Publishing2024-11info: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/11336/257176de Gerónimo, Francisco César; Miller Bertolami, Marcelo Miguel; Battich, Tiara; Tang, Xiaodong; Catelan, Márcio; et al.; Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs; IOP Publishing; Astrophysical Journal; 975; 2; 11-2024; 1-100004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ad7d8einfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ad7d8einfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:01:00Zoai:ri.conicet.gov.ar:11336/257176instacron: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 10:01:01.158CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
title Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
spellingShingle Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
de Gerónimo, Francisco César
DA stars
Nuclear abundances
Stellar evolution
title_short Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
title_full Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
title_fullStr Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
title_full_unstemmed Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
title_sort Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs
dc.creator.none.fl_str_mv de Gerónimo, Francisco César
Miller Bertolami, Marcelo Miguel
Battich, Tiara
Tang, Xiaodong
Catelan, Márcio
Corsico, Alejandro Hugo
Li, Yunjun
Fang, Xiao
Althaus, Leandro Gabriel
author de Gerónimo, Francisco César
author_facet de Gerónimo, Francisco César
Miller Bertolami, Marcelo Miguel
Battich, Tiara
Tang, Xiaodong
Catelan, Márcio
Corsico, Alejandro Hugo
Li, Yunjun
Fang, Xiao
Althaus, Leandro Gabriel
author_role author
author2 Miller Bertolami, Marcelo Miguel
Battich, Tiara
Tang, Xiaodong
Catelan, Márcio
Corsico, Alejandro Hugo
Li, Yunjun
Fang, Xiao
Althaus, Leandro Gabriel
author2_role author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv DA stars
Nuclear abundances
Stellar evolution
topic DA stars
Nuclear abundances
Stellar 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 Recent determinations of the total rate of the 12 C+12 C nuclear reaction show non-negligible differences with thereference reaction rate commonly used in previous stellar simulations. In addition, the current uncertainties indetermining each exit channel constitute one of the main uncertainties in shaping the inner structure of superasymptotic giant branch stars that could have a measurable impact on the properties of pulsating ultramassive whitedwarfs (WDs). We explore how new determinations of the nuclear reaction rate and its branching ratios affect theevolution of WD progenitors. We show that the current uncertainties in the branching ratios constitute the mainuncertainty factor in determining the inner composition of ultramassive WDs and their progenitors. We found thatthe use of extreme branching ratios leads to differences in the central abundances of 20Ne of at most 17%, whichare translated into differences of at most 1.3% and 0.8% in the cooling times and size of the crystallized core,respectively. However, the impact on the pulsation properties is small, less than 1 s for the asymptotic periodspacing. We found that the carbon burns partially in the interior of ultramassive WD progenitors within a particularrange of masses, leaving a hybrid CONe-core composition in their cores. The evolution of these new kinds ofpredicted objects differs substantially from the evolution of objects with pure CO cores. Differences in the size ofthe crystallized core and cooling times of up to 15% and 6%, respectively, lead to distinct patterns in the periodspacing distribution.
Fil: de Gerónimo, Francisco César. 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: Miller Bertolami, Marcelo Miguel. 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: Battich, Tiara. 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. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Tang, Xiaodong. Chinese Academy of Sciences; República de China
Fil: Catelan, Márcio. Pontificia Universidad Católica de Chile; Chile. Millennium Institute of Astrophysics; Chile
Fil: Corsico, Alejandro Hugo. 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: Li, Yunjun. China Institute of Atomic Energy; China
Fil: Fang, Xiao. Sun Yat-sen University; China
Fil: Althaus, Leandro Gabriel. 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 Recent determinations of the total rate of the 12 C+12 C nuclear reaction show non-negligible differences with thereference reaction rate commonly used in previous stellar simulations. In addition, the current uncertainties indetermining each exit channel constitute one of the main uncertainties in shaping the inner structure of superasymptotic giant branch stars that could have a measurable impact on the properties of pulsating ultramassive whitedwarfs (WDs). We explore how new determinations of the nuclear reaction rate and its branching ratios affect theevolution of WD progenitors. We show that the current uncertainties in the branching ratios constitute the mainuncertainty factor in determining the inner composition of ultramassive WDs and their progenitors. We found thatthe use of extreme branching ratios leads to differences in the central abundances of 20Ne of at most 17%, whichare translated into differences of at most 1.3% and 0.8% in the cooling times and size of the crystallized core,respectively. However, the impact on the pulsation properties is small, less than 1 s for the asymptotic periodspacing. We found that the carbon burns partially in the interior of ultramassive WD progenitors within a particularrange of masses, leaving a hybrid CONe-core composition in their cores. The evolution of these new kinds ofpredicted objects differs substantially from the evolution of objects with pure CO cores. Differences in the size ofthe crystallized core and cooling times of up to 15% and 6%, respectively, lead to distinct patterns in the periodspacing distribution.
publishDate 2024
dc.date.none.fl_str_mv 2024-11
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/11336/257176
de Gerónimo, Francisco César; Miller Bertolami, Marcelo Miguel; Battich, Tiara; Tang, Xiaodong; Catelan, Márcio; et al.; Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs; IOP Publishing; Astrophysical Journal; 975; 2; 11-2024; 1-10
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/257176
identifier_str_mv de Gerónimo, Francisco César; Miller Bertolami, Marcelo Miguel; Battich, Tiara; Tang, Xiaodong; Catelan, Márcio; et al.; Impact of Current Uncertainties in the 12 C+ 12 C Nuclear Reaction Rate on Intermediate-mass Stars and Massive White Dwarfs; IOP Publishing; Astrophysical Journal; 975; 2; 11-2024; 1-10
0004-637X
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://iopscience.iop.org/article/10.3847/1538-4357/ad7d8e
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ad7d8e
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
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
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score 13.070432

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