New models for the evolution of central stars of planetary nebulae: faster and brighter

Autores
Miller Bertolami, Marcelo Miguel
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The post-asymptotic giant branch (AGB) phase is arguably one of the least understood phases of the evolution of low- and intermediate- mass stars. The recent post-AGB evolutionary sequences computed by Miller Bertolami (2016) are at least three to ten times faster than those previously published by Vassiliadis & Wood (1994) and Blöcker (1995) which have been used in a large number of studies. This is true for the whole mass and metallicity range. The new models are also ~0.1-0.3 dex brighter than the previous models with similar remnant masses. In this short article we comment on the main reasons behind these differences, and discuss possible implications for other studies of post-AGB stars or planetary nebulae.
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
planetary nebulae: general
stars: AGB and post-AGB
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:10915/85972
Acceder
id SEDICI_d7cc3992f4b5586b66ed7b3a6a2b211d
oai_identifier_str oai:sedici.unlp.edu.ar:10915/85972
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling New models for the evolution of central stars of planetary nebulae: faster and brighterMiller Bertolami, Marcelo MiguelCiencias Astronómicasplanetary nebulae: generalstars: AGB and post-AGBThe post-asymptotic giant branch (AGB) phase is arguably one of the least understood phases of the evolution of low- and intermediate- mass stars. The recent post-AGB evolutionary sequences computed by Miller Bertolami (2016) are at least three to ten times faster than those previously published by Vassiliadis & Wood (1994) and Blöcker (1995) which have been used in a large number of studies. This is true for the whole mass and metallicity range. The new models are also ~0.1-0.3 dex brighter than the previous models with similar remnant masses. In this short article we comment on the main reasons behind these differences, and discuss possible implications for other studies of post-AGB stars or planetary nebulae.Instituto de Astrofísica de La Plata2016info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf179-183http://sedici.unlp.edu.ar/handle/10915/85972enginfo:eu-repo/semantics/altIdentifier/issn/1743-9213info:eu-repo/semantics/altIdentifier/doi/10.1017/S1743921317001533info: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:UNLP2025-10-22T16:57:33Zoai:sedici.unlp.edu.ar:10915/85972Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-10-22 16:57:33.405SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv New models for the evolution of central stars of planetary nebulae: faster and brighter
title New models for the evolution of central stars of planetary nebulae: faster and brighter
spellingShingle New models for the evolution of central stars of planetary nebulae: faster and brighter
Miller Bertolami, Marcelo Miguel
Ciencias Astronómicas
planetary nebulae: general
stars: AGB and post-AGB
title_short New models for the evolution of central stars of planetary nebulae: faster and brighter
title_full New models for the evolution of central stars of planetary nebulae: faster and brighter
title_fullStr New models for the evolution of central stars of planetary nebulae: faster and brighter
title_full_unstemmed New models for the evolution of central stars of planetary nebulae: faster and brighter
title_sort New models for the evolution of central stars of planetary nebulae: faster and brighter
dc.creator.none.fl_str_mv Miller Bertolami, Marcelo Miguel
author Miller Bertolami, Marcelo Miguel
author_facet Miller Bertolami, Marcelo Miguel
author_role author
dc.subject.none.fl_str_mv Ciencias Astronómicas
planetary nebulae: general
stars: AGB and post-AGB
topic Ciencias Astronómicas
planetary nebulae: general
stars: AGB and post-AGB
dc.description.none.fl_txt_mv The post-asymptotic giant branch (AGB) phase is arguably one of the least understood phases of the evolution of low- and intermediate- mass stars. The recent post-AGB evolutionary sequences computed by Miller Bertolami (2016) are at least three to ten times faster than those previously published by Vassiliadis & Wood (1994) and Blöcker (1995) which have been used in a large number of studies. This is true for the whole mass and metallicity range. The new models are also ~0.1-0.3 dex brighter than the previous models with similar remnant masses. In this short article we comment on the main reasons behind these differences, and discuss possible implications for other studies of post-AGB stars or planetary nebulae.
Instituto de Astrofísica de La Plata
description The post-asymptotic giant branch (AGB) phase is arguably one of the least understood phases of the evolution of low- and intermediate- mass stars. The recent post-AGB evolutionary sequences computed by Miller Bertolami (2016) are at least three to ten times faster than those previously published by Vassiliadis & Wood (1994) and Blöcker (1995) which have been used in a large number of studies. This is true for the whole mass and metallicity range. The new models are also ~0.1-0.3 dex brighter than the previous models with similar remnant masses. In this short article we comment on the main reasons behind these differences, and discuss possible implications for other studies of post-AGB stars or planetary nebulae.
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/10915/85972
url http://sedici.unlp.edu.ar/handle/10915/85972
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/1743-9213
info:eu-repo/semantics/altIdentifier/doi/10.1017/S1743921317001533
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
179-183
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
_version_ 1846783189918416896
score 12.982451

Publicaciones similares