Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion

Autores
Althaus, Leandro Gabriel; Serenelli, Aldo Marcelo; Benvenuto, Omar Gustavo
Año de publicación
2001
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Conventional wisdom indicates that a millisecond pulsar is recycled during the mass transfer stage in a binary system. Usually, the companion to the pulsar is a low-mass white dwarf. If zero ages are set at the end of mass transfer, the ages of both objects should be the same. Available models characterized by dominant hydrogen burning lead to a strong discrepancy between the ages of PSR B1855]09 and its white dwarf companion. We interpret such a discrepancy as a direct consequence of ignoring element di usion in the stellar models. We show that in the frame of models in which di usion is properly accounted for, ages naturally come into a nice agreement. Consequently, we do not have to invoke any ad hoc mass loss or exotic mechanisms to account for the ages of the stars that belong to the binary system PSR B1855]09.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
astrofísica
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-nd/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/2056
Acceder
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oai_identifier_str oai:sedici.unlp.edu.ar:10915/2056
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusionAlthaus, Leandro GabrielSerenelli, Aldo MarceloBenvenuto, Omar GustavoCiencias AstronómicasastrofísicaConventional wisdom indicates that a millisecond pulsar is recycled during the mass transfer stage in a binary system. Usually, the companion to the pulsar is a low-mass white dwarf. If zero ages are set at the end of mass transfer, the ages of both objects should be the same. Available models characterized by dominant hydrogen burning lead to a strong discrepancy between the ages of PSR B1855]09 and its white dwarf companion. We interpret such a discrepancy as a direct consequence of ignoring element di usion in the stellar models. We show that in the frame of models in which di usion is properly accounted for, ages naturally come into a nice agreement. Consequently, we do not have to invoke any ad hoc mass loss or exotic mechanisms to account for the ages of the stars that belong to the binary system PSR B1855]09.Facultad de Ciencias Astronómicas y Geofísicas2001info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf1110-1117http://sedici.unlp.edu.ar/handle/10915/2056enginfo:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1086/321414/metainfo:eu-repo/semantics/altIdentifier/doi/10.1086/321414info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-nd/4.0/Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T10:48:37Zoai:sedici.unlp.edu.ar:10915/2056Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 10:48:38.923SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
title Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
spellingShingle Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
Althaus, Leandro Gabriel
Ciencias Astronómicas
astrofísica
title_short Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
title_full Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
title_fullStr Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
title_full_unstemmed Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
title_sort Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
dc.creator.none.fl_str_mv Althaus, Leandro Gabriel
Serenelli, Aldo Marcelo
Benvenuto, Omar Gustavo
author Althaus, Leandro Gabriel
author_facet Althaus, Leandro Gabriel
Serenelli, Aldo Marcelo
Benvenuto, Omar Gustavo
author_role author
author2 Serenelli, Aldo Marcelo
Benvenuto, Omar Gustavo
author2_role author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
astrofísica
topic Ciencias Astronómicas
astrofísica
dc.description.none.fl_txt_mv Conventional wisdom indicates that a millisecond pulsar is recycled during the mass transfer stage in a binary system. Usually, the companion to the pulsar is a low-mass white dwarf. If zero ages are set at the end of mass transfer, the ages of both objects should be the same. Available models characterized by dominant hydrogen burning lead to a strong discrepancy between the ages of PSR B1855]09 and its white dwarf companion. We interpret such a discrepancy as a direct consequence of ignoring element di usion in the stellar models. We show that in the frame of models in which di usion is properly accounted for, ages naturally come into a nice agreement. Consequently, we do not have to invoke any ad hoc mass loss or exotic mechanisms to account for the ages of the stars that belong to the binary system PSR B1855]09.
Facultad de Ciencias Astronómicas y Geofísicas
description Conventional wisdom indicates that a millisecond pulsar is recycled during the mass transfer stage in a binary system. Usually, the companion to the pulsar is a low-mass white dwarf. If zero ages are set at the end of mass transfer, the ages of both objects should be the same. Available models characterized by dominant hydrogen burning lead to a strong discrepancy between the ages of PSR B1855]09 and its white dwarf companion. We interpret such a discrepancy as a direct consequence of ignoring element di usion in the stellar models. We show that in the frame of models in which di usion is properly accounted for, ages naturally come into a nice agreement. Consequently, we do not have to invoke any ad hoc mass loss or exotic mechanisms to account for the ages of the stars that belong to the binary system PSR B1855]09.
publishDate 2001
dc.date.none.fl_str_mv 2001
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/10915/2056
url http://sedici.unlp.edu.ar/handle/10915/2056
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1086/321414/meta
info:eu-repo/semantics/altIdentifier/doi/10.1086/321414
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-nd/4.0/
Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-nd/4.0/
Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)
dc.format.none.fl_str_mv application/pdf
1110-1117
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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score 13.070432

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