Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) stars

Autores
Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel
Año de publicación
2006
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. We present full evolutionary calculations appropriate to post-AGB PG 1159 stars for a wide range of stellar masses. Methods. We take into account the complete evolutionary stages of PG 1159 progenitors starting from the Zero Age Main Sequence. We consider the two kinds of Born Again Scenarios, the very late thermal pulse (VLTP) and the late thermal pulse (LTP), that give rise to hydrogen-deficient compositions. The location of our PG 1159 tracks in the effective temperature-gravity diagram and their comparison with previous calculations as well as the resulting surface compositions are discussed. Results. Our results reinforce the idea that the different abundances of 14N observed at the surface of those PG 1159 stars with undetected hydrogen is an indication that the progenitors of these stars would have evolved through a VLTP episode, where most of the hydrogen content of the remnant is burnt, or LTP, where hydrogen is not burnt but instead diluted to very low surface abundances. We derive new values for spectroscopical masses based on these models. We discuss the correlation between the presence of planetary nebulae and the 14N abundance as another indicator that 14N-rich objects should come from a VLTP episode while 14N-deficient ones should be the result of a LTP. Finally, we discuss an evolutionary scenario that could explain the existence of PG 1159 stars with unusually high helium abundances and a possible evolutionary connection between these stars and the low mass O(He) stars. © ESO 2006.
Fil: Miller Bertolami, Marcelo Miguel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Althaus, Leandro Gabriel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Materia
AGB stars
Post AGB stars
Interior stars
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/39214
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/39214
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) starsMiller Bertolami, Marcelo MiguelAlthaus, Leandro GabrielAGB starsPost AGB starsInterior starshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. We present full evolutionary calculations appropriate to post-AGB PG 1159 stars for a wide range of stellar masses. Methods. We take into account the complete evolutionary stages of PG 1159 progenitors starting from the Zero Age Main Sequence. We consider the two kinds of Born Again Scenarios, the very late thermal pulse (VLTP) and the late thermal pulse (LTP), that give rise to hydrogen-deficient compositions. The location of our PG 1159 tracks in the effective temperature-gravity diagram and their comparison with previous calculations as well as the resulting surface compositions are discussed. Results. Our results reinforce the idea that the different abundances of 14N observed at the surface of those PG 1159 stars with undetected hydrogen is an indication that the progenitors of these stars would have evolved through a VLTP episode, where most of the hydrogen content of the remnant is burnt, or LTP, where hydrogen is not burnt but instead diluted to very low surface abundances. We derive new values for spectroscopical masses based on these models. We discuss the correlation between the presence of planetary nebulae and the 14N abundance as another indicator that 14N-rich objects should come from a VLTP episode while 14N-deficient ones should be the result of a LTP. Finally, we discuss an evolutionary scenario that could explain the existence of PG 1159 stars with unusually high helium abundances and a possible evolutionary connection between these stars and the low mass O(He) stars. © ESO 2006.Fil: Miller Bertolami, Marcelo Miguel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Althaus, Leandro Gabriel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaEDP Sciences2006-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/39214Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel; Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) stars; EDP Sciences; Astronomy and Astrophysics; 454; 3; 8-2006; 845-8540004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20054723info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2006/30/aa4723-05/aa4723-05.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:54:52Zoai:ri.conicet.gov.ar:11336/39214instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-22 11:54:53.022CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) stars
title Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) stars
spellingShingle Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) stars
Miller Bertolami, Marcelo Miguel
AGB stars
Post AGB stars
Interior stars
title_short Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) stars
title_full Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) stars
title_fullStr Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) stars
title_full_unstemmed Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) stars
title_sort Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) stars
dc.creator.none.fl_str_mv Miller Bertolami, Marcelo Miguel
Althaus, Leandro Gabriel
author Miller Bertolami, Marcelo Miguel
author_facet Miller Bertolami, Marcelo Miguel
Althaus, Leandro Gabriel
author_role author
author2 Althaus, Leandro Gabriel
author2_role author
dc.subject.none.fl_str_mv AGB stars
Post AGB stars
Interior stars
topic AGB stars
Post AGB stars
Interior stars
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Aims. We present full evolutionary calculations appropriate to post-AGB PG 1159 stars for a wide range of stellar masses. Methods. We take into account the complete evolutionary stages of PG 1159 progenitors starting from the Zero Age Main Sequence. We consider the two kinds of Born Again Scenarios, the very late thermal pulse (VLTP) and the late thermal pulse (LTP), that give rise to hydrogen-deficient compositions. The location of our PG 1159 tracks in the effective temperature-gravity diagram and their comparison with previous calculations as well as the resulting surface compositions are discussed. Results. Our results reinforce the idea that the different abundances of 14N observed at the surface of those PG 1159 stars with undetected hydrogen is an indication that the progenitors of these stars would have evolved through a VLTP episode, where most of the hydrogen content of the remnant is burnt, or LTP, where hydrogen is not burnt but instead diluted to very low surface abundances. We derive new values for spectroscopical masses based on these models. We discuss the correlation between the presence of planetary nebulae and the 14N abundance as another indicator that 14N-rich objects should come from a VLTP episode while 14N-deficient ones should be the result of a LTP. Finally, we discuss an evolutionary scenario that could explain the existence of PG 1159 stars with unusually high helium abundances and a possible evolutionary connection between these stars and the low mass O(He) stars. © ESO 2006.
Fil: Miller Bertolami, Marcelo Miguel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Althaus, Leandro Gabriel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
description Aims. We present full evolutionary calculations appropriate to post-AGB PG 1159 stars for a wide range of stellar masses. Methods. We take into account the complete evolutionary stages of PG 1159 progenitors starting from the Zero Age Main Sequence. We consider the two kinds of Born Again Scenarios, the very late thermal pulse (VLTP) and the late thermal pulse (LTP), that give rise to hydrogen-deficient compositions. The location of our PG 1159 tracks in the effective temperature-gravity diagram and their comparison with previous calculations as well as the resulting surface compositions are discussed. Results. Our results reinforce the idea that the different abundances of 14N observed at the surface of those PG 1159 stars with undetected hydrogen is an indication that the progenitors of these stars would have evolved through a VLTP episode, where most of the hydrogen content of the remnant is burnt, or LTP, where hydrogen is not burnt but instead diluted to very low surface abundances. We derive new values for spectroscopical masses based on these models. We discuss the correlation between the presence of planetary nebulae and the 14N abundance as another indicator that 14N-rich objects should come from a VLTP episode while 14N-deficient ones should be the result of a LTP. Finally, we discuss an evolutionary scenario that could explain the existence of PG 1159 stars with unusually high helium abundances and a possible evolutionary connection between these stars and the low mass O(He) stars. © ESO 2006.
publishDate 2006
dc.date.none.fl_str_mv 2006-08
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
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://hdl.handle.net/11336/39214
Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel; Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) stars; EDP Sciences; Astronomy and Astrophysics; 454; 3; 8-2006; 845-854
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/39214
identifier_str_mv Miller Bertolami, Marcelo Miguel; Althaus, Leandro Gabriel; Full evolutionary models for PG 1159 stars. Implications for the helium-rich O(He) stars; EDP Sciences; Astronomy and Astrophysics; 454; 3; 8-2006; 845-854
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20054723
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2006/30/aa4723-05/aa4723-05.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 12.982451

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