The effect of <SUP>22</SUP>Ne diffusion in the evolution and pulsational properties of white dwarfs with solar metallicity progenitors

Autores
Camisassa, María Eugenia; Althaus, Leandro Gabriel; Córsico, Alejandro Hugo; Vinyoles, N.; Serenelli, Aldo Marcelo; Isern, J.; Miller Bertolami, Marcelo Miguel; García Berro, E.
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Because of the large neutron excess of 22Ne, sedimentation of this isotope occurs rapidly in the interior of white dwarfs. This process releases an additional amount of energy, thus delaying the cooling times of the white dwarf. This influences the ages of different stellar populations derived using white dwarf cosmochronology. Furthermore, the overabundance of 22Ne in the inner regions of the star modifies the Brunt-Väisälä frequency, thus altering the pulsational properties of these stars. In this work we discuss the impact of 22Ne sedimentation in white dwarfs resulting from solar metallicity progenitors (Z = 0.02). We performed evolutionary calculations of white dwarfs with masses of 0.528, 0.576, 0.657, and 0.833 derived from full evolutionary computations of their progenitor stars, starting at the zero-Age main sequence all the way through the central hydrogen and helium burning, the thermally pulsing asymptotic giant branch (AGB), and post-AGB phases. Our computations show that at low luminosities (), 22Ne sedimentation delays the cooling of white dwarfs with solar metallicity progenitors by about 1 Gyr. Additionally, we studied the consequences of 22Ne sedimentation on the pulsational properties of ZZ Ceti white dwarfs. We find that 22Ne sedimentation induces differences in the periods of these stars larger than the present observational uncertainties, particularly in more massive white dwarfs.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
asteroseismology
dense matter
diffusion
stars: evolution
stars: interiors
white dwarfs
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/86799

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network_name_str SEDICI (UNLP)
spelling The effect of <SUP>22</SUP>Ne diffusion in the evolution and pulsational properties of white dwarfs with solar metallicity progenitorsCamisassa, María EugeniaAlthaus, Leandro GabrielCórsico, Alejandro HugoVinyoles, N.Serenelli, Aldo MarceloIsern, J.Miller Bertolami, Marcelo MiguelGarcía Berro, E.Ciencias Astronómicasasteroseismologydense matterdiffusionstars: evolutionstars: interiorswhite dwarfsBecause of the large neutron excess of 22Ne, sedimentation of this isotope occurs rapidly in the interior of white dwarfs. This process releases an additional amount of energy, thus delaying the cooling times of the white dwarf. This influences the ages of different stellar populations derived using white dwarf cosmochronology. Furthermore, the overabundance of 22Ne in the inner regions of the star modifies the Brunt-Väisälä frequency, thus altering the pulsational properties of these stars. In this work we discuss the impact of 22Ne sedimentation in white dwarfs resulting from solar metallicity progenitors (Z = 0.02). We performed evolutionary calculations of white dwarfs with masses of 0.528, 0.576, 0.657, and 0.833 derived from full evolutionary computations of their progenitor stars, starting at the zero-Age main sequence all the way through the central hydrogen and helium burning, the thermally pulsing asymptotic giant branch (AGB), and post-AGB phases. Our computations show that at low luminosities (), 22Ne sedimentation delays the cooling of white dwarfs with solar metallicity progenitors by about 1 Gyr. Additionally, we studied the consequences of 22Ne sedimentation on the pulsational properties of ZZ Ceti white dwarfs. We find that 22Ne sedimentation induces differences in the periods of these stars larger than the present observational uncertainties, particularly in more massive white dwarfs.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2016info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/86799enginfo:eu-repo/semantics/altIdentifier/issn/0004-637Xinfo:eu-repo/semantics/altIdentifier/doi/10.3847/0004-637X/823/2/158info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:45Zoai:sedici.unlp.edu.ar:10915/86799Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:45.53SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv The effect of <SUP>22</SUP>Ne diffusion in the evolution and pulsational properties of white dwarfs with solar metallicity progenitors
title The effect of <SUP>22</SUP>Ne diffusion in the evolution and pulsational properties of white dwarfs with solar metallicity progenitors
spellingShingle The effect of <SUP>22</SUP>Ne diffusion in the evolution and pulsational properties of white dwarfs with solar metallicity progenitors
Camisassa, María Eugenia
Ciencias Astronómicas
asteroseismology
dense matter
diffusion
stars: evolution
stars: interiors
white dwarfs
title_short The effect of <SUP>22</SUP>Ne diffusion in the evolution and pulsational properties of white dwarfs with solar metallicity progenitors
title_full The effect of <SUP>22</SUP>Ne diffusion in the evolution and pulsational properties of white dwarfs with solar metallicity progenitors
title_fullStr The effect of <SUP>22</SUP>Ne diffusion in the evolution and pulsational properties of white dwarfs with solar metallicity progenitors
title_full_unstemmed The effect of <SUP>22</SUP>Ne diffusion in the evolution and pulsational properties of white dwarfs with solar metallicity progenitors
title_sort The effect of <SUP>22</SUP>Ne diffusion in the evolution and pulsational properties of white dwarfs with solar metallicity progenitors
dc.creator.none.fl_str_mv Camisassa, María Eugenia
Althaus, Leandro Gabriel
Córsico, Alejandro Hugo
Vinyoles, N.
Serenelli, Aldo Marcelo
Isern, J.
Miller Bertolami, Marcelo Miguel
García Berro, E.
author Camisassa, María Eugenia
author_facet Camisassa, María Eugenia
Althaus, Leandro Gabriel
Córsico, Alejandro Hugo
Vinyoles, N.
Serenelli, Aldo Marcelo
Isern, J.
Miller Bertolami, Marcelo Miguel
García Berro, E.
author_role author
author2 Althaus, Leandro Gabriel
Córsico, Alejandro Hugo
Vinyoles, N.
Serenelli, Aldo Marcelo
Isern, J.
Miller Bertolami, Marcelo Miguel
García Berro, E.
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
asteroseismology
dense matter
diffusion
stars: evolution
stars: interiors
white dwarfs
topic Ciencias Astronómicas
asteroseismology
dense matter
diffusion
stars: evolution
stars: interiors
white dwarfs
dc.description.none.fl_txt_mv Because of the large neutron excess of 22Ne, sedimentation of this isotope occurs rapidly in the interior of white dwarfs. This process releases an additional amount of energy, thus delaying the cooling times of the white dwarf. This influences the ages of different stellar populations derived using white dwarf cosmochronology. Furthermore, the overabundance of 22Ne in the inner regions of the star modifies the Brunt-Väisälä frequency, thus altering the pulsational properties of these stars. In this work we discuss the impact of 22Ne sedimentation in white dwarfs resulting from solar metallicity progenitors (Z = 0.02). We performed evolutionary calculations of white dwarfs with masses of 0.528, 0.576, 0.657, and 0.833 derived from full evolutionary computations of their progenitor stars, starting at the zero-Age main sequence all the way through the central hydrogen and helium burning, the thermally pulsing asymptotic giant branch (AGB), and post-AGB phases. Our computations show that at low luminosities (), 22Ne sedimentation delays the cooling of white dwarfs with solar metallicity progenitors by about 1 Gyr. Additionally, we studied the consequences of 22Ne sedimentation on the pulsational properties of ZZ Ceti white dwarfs. We find that 22Ne sedimentation induces differences in the periods of these stars larger than the present observational uncertainties, particularly in more massive white dwarfs.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
description Because of the large neutron excess of 22Ne, sedimentation of this isotope occurs rapidly in the interior of white dwarfs. This process releases an additional amount of energy, thus delaying the cooling times of the white dwarf. This influences the ages of different stellar populations derived using white dwarf cosmochronology. Furthermore, the overabundance of 22Ne in the inner regions of the star modifies the Brunt-Väisälä frequency, thus altering the pulsational properties of these stars. In this work we discuss the impact of 22Ne sedimentation in white dwarfs resulting from solar metallicity progenitors (Z = 0.02). We performed evolutionary calculations of white dwarfs with masses of 0.528, 0.576, 0.657, and 0.833 derived from full evolutionary computations of their progenitor stars, starting at the zero-Age main sequence all the way through the central hydrogen and helium burning, the thermally pulsing asymptotic giant branch (AGB), and post-AGB phases. Our computations show that at low luminosities (), 22Ne sedimentation delays the cooling of white dwarfs with solar metallicity progenitors by about 1 Gyr. Additionally, we studied the consequences of 22Ne sedimentation on the pulsational properties of ZZ Ceti white dwarfs. We find that 22Ne sedimentation induces differences in the periods of these stars larger than the present observational uncertainties, particularly in more massive white dwarfs.
publishDate 2016
dc.date.none.fl_str_mv 2016
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/10915/86799
url http://sedici.unlp.edu.ar/handle/10915/86799
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-637X
info:eu-repo/semantics/altIdentifier/doi/10.3847/0004-637X/823/2/158
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
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
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