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
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/86799
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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 |
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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) |
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http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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