A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds
- Autores
- Walborn, Nolan Revere; Morrell, Nidia Irene; Howarth, Ian D.; Crowther, Paul A.; Lennon, Daniel J.; Massey, Philip; Arias, Julia Ines
- Año de publicación
- 2004
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- From a survey of the 3400 Å region in the earliest O-type spectra, we have found that two of the four O2 giants observed in the Large Magellanic Cloud have O IV lines there that are stronger than the N IV lines, while the other two have the opposite. A Small Magellanic Cloud counterpart also has N IV stronger than O IV. Inspection of the blue spectra of these stars shows that the former pair have weaker N lines in all ionization states (III, IV, and V) present as well as lines of C IV λ4658, while the latter three have stronger N lines and greater He/H. Space ultraviolet observations of two of the N-strong stars show N V wind profiles substantially stronger than those of C IV, while in the N-weak stars the C IV features are equal to or stronger than the N V. The N-strong stars are now reclassified as ON2 III(f*), newly defining that category. These characteristics strongly suggest a larger fraction of processed material in the atmospheres of the ON2 stars, which we confirm by modeling the optical spectra. In the context of current models, it is in turn implied that the ON2 stars are in a more advanced evolutionary state than the others, and/or that they had higher initial rotational velocities. The recent formulation of the effects of rotation on massive stellar evolution introduces an additional fundamental parameter, which the CNO abundances are in principle able to constrain. We present some illustrative comparisons with current Geneva evolutionary models for rotating massive stars. It is possible that these very hot, nitrogen-rich objects are products of homogeneous evolution. Our results will provide motivation for further physical modeling of the atmospheres and evolutionary histories of the most massive hot stars.
Fil: Walborn, Nolan Revere. Space Telescope Science Institute; Estados Unidos
Fil: Morrell, Nidia Irene. Las campanas observatory; Chile
Fil: Howarth, Ian D.. University College London; Estados Unidos
Fil: Crowther, Paul A.. University of Sheffield; Reino Unido
Fil: Lennon, Daniel J.. Isaac Newton Group of Telescopes; España
Fil: Massey, Philip. Lowell Observatory; Estados Unidos
Fil: Arias, Julia Ines. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina - Materia
-
Magellanic Clouds
Abundances
Early type stars
Evolution of stars
Fundamental parameters - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/37076
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A CNO Dichotomy among O2 Giant Spectra in the Magellanic CloudsWalborn, Nolan RevereMorrell, Nidia IreneHowarth, Ian D.Crowther, Paul A.Lennon, Daniel J.Massey, PhilipArias, Julia InesMagellanic CloudsAbundancesEarly type starsEvolution of starsFundamental parametershttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1From a survey of the 3400 Å region in the earliest O-type spectra, we have found that two of the four O2 giants observed in the Large Magellanic Cloud have O IV lines there that are stronger than the N IV lines, while the other two have the opposite. A Small Magellanic Cloud counterpart also has N IV stronger than O IV. Inspection of the blue spectra of these stars shows that the former pair have weaker N lines in all ionization states (III, IV, and V) present as well as lines of C IV λ4658, while the latter three have stronger N lines and greater He/H. Space ultraviolet observations of two of the N-strong stars show N V wind profiles substantially stronger than those of C IV, while in the N-weak stars the C IV features are equal to or stronger than the N V. The N-strong stars are now reclassified as ON2 III(f*), newly defining that category. These characteristics strongly suggest a larger fraction of processed material in the atmospheres of the ON2 stars, which we confirm by modeling the optical spectra. In the context of current models, it is in turn implied that the ON2 stars are in a more advanced evolutionary state than the others, and/or that they had higher initial rotational velocities. The recent formulation of the effects of rotation on massive stellar evolution introduces an additional fundamental parameter, which the CNO abundances are in principle able to constrain. We present some illustrative comparisons with current Geneva evolutionary models for rotating massive stars. It is possible that these very hot, nitrogen-rich objects are products of homogeneous evolution. Our results will provide motivation for further physical modeling of the atmospheres and evolutionary histories of the most massive hot stars.Fil: Walborn, Nolan Revere. Space Telescope Science Institute; Estados UnidosFil: Morrell, Nidia Irene. Las campanas observatory; ChileFil: Howarth, Ian D.. University College London; Estados UnidosFil: Crowther, Paul A.. University of Sheffield; Reino UnidoFil: Lennon, Daniel J.. Isaac Newton Group of Telescopes; EspañaFil: Massey, Philip. Lowell Observatory; Estados UnidosFil: Arias, Julia Ines. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaIOP Publishing2004-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/37076Walborn, Nolan Revere; Morrell, Nidia Irene; Howarth, Ian D.; Crowther, Paul A.; Lennon, Daniel J.; et al.; A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds; IOP Publishing; Astrophysical Journal; 608; 2; 6-2004; 1028-10380004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1086/420761info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1086/420761/metainfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:34:01Zoai:ri.conicet.gov.ar:11336/37076instacron: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:34982025-09-29 09:34:01.526CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds |
title |
A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds |
spellingShingle |
A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds Walborn, Nolan Revere Magellanic Clouds Abundances Early type stars Evolution of stars Fundamental parameters |
title_short |
A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds |
title_full |
A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds |
title_fullStr |
A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds |
title_full_unstemmed |
A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds |
title_sort |
A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds |
dc.creator.none.fl_str_mv |
Walborn, Nolan Revere Morrell, Nidia Irene Howarth, Ian D. Crowther, Paul A. Lennon, Daniel J. Massey, Philip Arias, Julia Ines |
author |
Walborn, Nolan Revere |
author_facet |
Walborn, Nolan Revere Morrell, Nidia Irene Howarth, Ian D. Crowther, Paul A. Lennon, Daniel J. Massey, Philip Arias, Julia Ines |
author_role |
author |
author2 |
Morrell, Nidia Irene Howarth, Ian D. Crowther, Paul A. Lennon, Daniel J. Massey, Philip Arias, Julia Ines |
author2_role |
author author author author author author |
dc.subject.none.fl_str_mv |
Magellanic Clouds Abundances Early type stars Evolution of stars Fundamental parameters |
topic |
Magellanic Clouds Abundances Early type stars Evolution of stars Fundamental parameters |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
From a survey of the 3400 Å region in the earliest O-type spectra, we have found that two of the four O2 giants observed in the Large Magellanic Cloud have O IV lines there that are stronger than the N IV lines, while the other two have the opposite. A Small Magellanic Cloud counterpart also has N IV stronger than O IV. Inspection of the blue spectra of these stars shows that the former pair have weaker N lines in all ionization states (III, IV, and V) present as well as lines of C IV λ4658, while the latter three have stronger N lines and greater He/H. Space ultraviolet observations of two of the N-strong stars show N V wind profiles substantially stronger than those of C IV, while in the N-weak stars the C IV features are equal to or stronger than the N V. The N-strong stars are now reclassified as ON2 III(f*), newly defining that category. These characteristics strongly suggest a larger fraction of processed material in the atmospheres of the ON2 stars, which we confirm by modeling the optical spectra. In the context of current models, it is in turn implied that the ON2 stars are in a more advanced evolutionary state than the others, and/or that they had higher initial rotational velocities. The recent formulation of the effects of rotation on massive stellar evolution introduces an additional fundamental parameter, which the CNO abundances are in principle able to constrain. We present some illustrative comparisons with current Geneva evolutionary models for rotating massive stars. It is possible that these very hot, nitrogen-rich objects are products of homogeneous evolution. Our results will provide motivation for further physical modeling of the atmospheres and evolutionary histories of the most massive hot stars. Fil: Walborn, Nolan Revere. Space Telescope Science Institute; Estados Unidos Fil: Morrell, Nidia Irene. Las campanas observatory; Chile Fil: Howarth, Ian D.. University College London; Estados Unidos Fil: Crowther, Paul A.. University of Sheffield; Reino Unido Fil: Lennon, Daniel J.. Isaac Newton Group of Telescopes; España Fil: Massey, Philip. Lowell Observatory; Estados Unidos Fil: Arias, Julia Ines. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina |
description |
From a survey of the 3400 Å region in the earliest O-type spectra, we have found that two of the four O2 giants observed in the Large Magellanic Cloud have O IV lines there that are stronger than the N IV lines, while the other two have the opposite. A Small Magellanic Cloud counterpart also has N IV stronger than O IV. Inspection of the blue spectra of these stars shows that the former pair have weaker N lines in all ionization states (III, IV, and V) present as well as lines of C IV λ4658, while the latter three have stronger N lines and greater He/H. Space ultraviolet observations of two of the N-strong stars show N V wind profiles substantially stronger than those of C IV, while in the N-weak stars the C IV features are equal to or stronger than the N V. The N-strong stars are now reclassified as ON2 III(f*), newly defining that category. These characteristics strongly suggest a larger fraction of processed material in the atmospheres of the ON2 stars, which we confirm by modeling the optical spectra. In the context of current models, it is in turn implied that the ON2 stars are in a more advanced evolutionary state than the others, and/or that they had higher initial rotational velocities. The recent formulation of the effects of rotation on massive stellar evolution introduces an additional fundamental parameter, which the CNO abundances are in principle able to constrain. We present some illustrative comparisons with current Geneva evolutionary models for rotating massive stars. It is possible that these very hot, nitrogen-rich objects are products of homogeneous evolution. Our results will provide motivation for further physical modeling of the atmospheres and evolutionary histories of the most massive hot stars. |
publishDate |
2004 |
dc.date.none.fl_str_mv |
2004-06 |
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/11336/37076 Walborn, Nolan Revere; Morrell, Nidia Irene; Howarth, Ian D.; Crowther, Paul A.; Lennon, Daniel J.; et al.; A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds; IOP Publishing; Astrophysical Journal; 608; 2; 6-2004; 1028-1038 0004-637X CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/37076 |
identifier_str_mv |
Walborn, Nolan Revere; Morrell, Nidia Irene; Howarth, Ian D.; Crowther, Paul A.; Lennon, Daniel J.; et al.; A CNO Dichotomy among O2 Giant Spectra in the Magellanic Clouds; IOP Publishing; Astrophysical Journal; 608; 2; 6-2004; 1028-1038 0004-637X CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1086/420761 info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1086/420761/meta |
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 |
dc.publisher.none.fl_str_mv |
IOP Publishing |
publisher.none.fl_str_mv |
IOP Publishing |
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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1844613050397622272 |
score |
13.070432 |