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
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/85972
Ver los metadatos del registro completo
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:UNLP2025-09-29T11:16:44Zoai: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:13292025-09-29 11:16:44.635SEDICI (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_ |
1844616039995801600 |
score |
13.070432 |