Molecular emission from GG Carinae's circumbinary disk

Autores
Kraus, M.; Oksala, M. E.; Nickeler, D. H.; Muratore, M. F.; Borges Fernandes, M.; Aret, A.; Cidale, Lydia Sonia; de Wit, W. J.
Año de publicación
2013
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The appearance of the B[e] phenomenon in evolved massive stars such as B[e] supergiants is still a mystery. While these stars are generally found to have disks that are cool and dense enough for efficient molecule and dust condensation, the origin of the disk material is still unclear. We aim at studying the kinematics and origin of the disk in the eccentric binary system GG Car, whose primary component is proposed to be a B[e] supergiant. Based on medium- and high-resolution near-infrared spectra we analyzed the CO-band emission detected from GG Car. The complete CO-band structure delivers information on the density and temperature of the emitting region, and the detectable 13CO bands allow us to constrain the evolutionary phase. In addition, the kinematics of the CO gas can be extracted from the shape of the first 12CO band head. We find that the CO gas is located in a ring surrounding the eccentric binary system, and its kinematics agrees with Keplerian rotation with a velocity, projected to the line of sight, of (80pm 1) km/s. The CO ring has a column density of (5pm 3)x10^21 cm^-2 and a temperature of 3200pm 500 K. In addition, the material is chemically enriched in 13CO, which agrees with the primary component being slightly evolved off the main sequence. We discuss two possible scenarios for the origin of the circumbinary disk: (i) non-conservative Roche lobe overflow, and (ii) the possibility that the progenitor of the primary component could have been a classical Be star. Neither can be firmly excluded, but for Roche lobe overflow to occur, a combination of stellar and orbital parameter extremawould be required.
Fil: Kraus, M.. Astronomický ústav; República Checa
Fil: Oksala, M. E.. Astronomický ústav; República Checa
Fil: Nickeler, D. H.. Astronomický ústav; República Checa
Fil: Muratore, M. F.. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Borges Fernandes, M.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Aret, A.. Tartu Observatory; Estonia
Fil: Cidale, Lydia Sonia. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: de Wit, W. J.. European Southern Observatory; Chile
Materia
Emission lines
Early type stars
Supergiants
Circumstellar matter
GG CAR (estrella)
B stars
Nivel de accesibilidad
acceso abierto
Condiciones de uso
Atribución-NoComercial-CompartirIgual 2.5 Argentina (CC 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:11336/8290
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/8290
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Molecular emission from GG Carinae's circumbinary diskKraus, M.Oksala, M. E.Nickeler, D. H.Muratore, M. F.Borges Fernandes, M.Aret, A.Cidale, Lydia Soniade Wit, W. J.Emission linesEarly type starsSupergiantsCircumstellar matterGG CAR (estrella)B starshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The appearance of the B[e] phenomenon in evolved massive stars such as B[e] supergiants is still a mystery. While these stars are generally found to have disks that are cool and dense enough for efficient molecule and dust condensation, the origin of the disk material is still unclear. We aim at studying the kinematics and origin of the disk in the eccentric binary system GG Car, whose primary component is proposed to be a B[e] supergiant. Based on medium- and high-resolution near-infrared spectra we analyzed the CO-band emission detected from GG Car. The complete CO-band structure delivers information on the density and temperature of the emitting region, and the detectable 13CO bands allow us to constrain the evolutionary phase. In addition, the kinematics of the CO gas can be extracted from the shape of the first 12CO band head. We find that the CO gas is located in a ring surrounding the eccentric binary system, and its kinematics agrees with Keplerian rotation with a velocity, projected to the line of sight, of (80pm 1) km/s. The CO ring has a column density of (5pm 3)x10^21 cm^-2 and a temperature of 3200pm 500 K. In addition, the material is chemically enriched in 13CO, which agrees with the primary component being slightly evolved off the main sequence. We discuss two possible scenarios for the origin of the circumbinary disk: (i) non-conservative Roche lobe overflow, and (ii) the possibility that the progenitor of the primary component could have been a classical Be star. Neither can be firmly excluded, but for Roche lobe overflow to occur, a combination of stellar and orbital parameter extremawould be required.Fil: Kraus, M.. Astronomický ústav; República ChecaFil: Oksala, M. E.. Astronomický ústav; República ChecaFil: Nickeler, D. H.. Astronomický ústav; República ChecaFil: Muratore, M. F.. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Borges Fernandes, M.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Aret, A.. Tartu Observatory; EstoniaFil: Cidale, Lydia Sonia. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: de Wit, W. J.. European Southern Observatory; ChileEdp Sciences2013-01info: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/11336/8290Kraus, M.; Oksala, M. E.; Nickeler, D. H.; Muratore, M. F.; Borges Fernandes, M.; et al.; Molecular emission from GG Carinae's circumbinary disk; Edp Sciences; Astronomy And Astrophysics; 549; A28; 1-2013; 1-80004-6361enginfo:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2013A%26A...549A..28Kinfo:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2013/01/aa20442-12/aa20442-12.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201220442info:eu-repo/semantics/openAccessAtribución-NoComercial-CompartirIgual 2.5 Argentina (CC BY-NC-SA 2.5 AR)https://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-11-12T09:51:01Zoai:ri.conicet.gov.ar:11336/8290instacron: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:34982025-11-12 09:51:01.78CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Molecular emission from GG Carinae's circumbinary disk
title Molecular emission from GG Carinae's circumbinary disk
spellingShingle Molecular emission from GG Carinae's circumbinary disk
Kraus, M.
Emission lines
Early type stars
Supergiants
Circumstellar matter
GG CAR (estrella)
B stars
title_short Molecular emission from GG Carinae's circumbinary disk
title_full Molecular emission from GG Carinae's circumbinary disk
title_fullStr Molecular emission from GG Carinae's circumbinary disk
title_full_unstemmed Molecular emission from GG Carinae's circumbinary disk
title_sort Molecular emission from GG Carinae's circumbinary disk
dc.creator.none.fl_str_mv Kraus, M.
Oksala, M. E.
Nickeler, D. H.
Muratore, M. F.
Borges Fernandes, M.
Aret, A.
Cidale, Lydia Sonia
de Wit, W. J.
author Kraus, M.
author_facet Kraus, M.
Oksala, M. E.
Nickeler, D. H.
Muratore, M. F.
Borges Fernandes, M.
Aret, A.
Cidale, Lydia Sonia
de Wit, W. J.
author_role author
author2 Oksala, M. E.
Nickeler, D. H.
Muratore, M. F.
Borges Fernandes, M.
Aret, A.
Cidale, Lydia Sonia
de Wit, W. J.
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Emission lines
Early type stars
Supergiants
Circumstellar matter
GG CAR (estrella)
B stars
topic Emission lines
Early type stars
Supergiants
Circumstellar matter
GG CAR (estrella)
B 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 The appearance of the B[e] phenomenon in evolved massive stars such as B[e] supergiants is still a mystery. While these stars are generally found to have disks that are cool and dense enough for efficient molecule and dust condensation, the origin of the disk material is still unclear. We aim at studying the kinematics and origin of the disk in the eccentric binary system GG Car, whose primary component is proposed to be a B[e] supergiant. Based on medium- and high-resolution near-infrared spectra we analyzed the CO-band emission detected from GG Car. The complete CO-band structure delivers information on the density and temperature of the emitting region, and the detectable 13CO bands allow us to constrain the evolutionary phase. In addition, the kinematics of the CO gas can be extracted from the shape of the first 12CO band head. We find that the CO gas is located in a ring surrounding the eccentric binary system, and its kinematics agrees with Keplerian rotation with a velocity, projected to the line of sight, of (80pm 1) km/s. The CO ring has a column density of (5pm 3)x10^21 cm^-2 and a temperature of 3200pm 500 K. In addition, the material is chemically enriched in 13CO, which agrees with the primary component being slightly evolved off the main sequence. We discuss two possible scenarios for the origin of the circumbinary disk: (i) non-conservative Roche lobe overflow, and (ii) the possibility that the progenitor of the primary component could have been a classical Be star. Neither can be firmly excluded, but for Roche lobe overflow to occur, a combination of stellar and orbital parameter extremawould be required.
Fil: Kraus, M.. Astronomický ústav; República Checa
Fil: Oksala, M. E.. Astronomický ústav; República Checa
Fil: Nickeler, D. H.. Astronomický ústav; República Checa
Fil: Muratore, M. F.. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Borges Fernandes, M.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Aret, A.. Tartu Observatory; Estonia
Fil: Cidale, Lydia Sonia. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: de Wit, W. J.. European Southern Observatory; Chile
description The appearance of the B[e] phenomenon in evolved massive stars such as B[e] supergiants is still a mystery. While these stars are generally found to have disks that are cool and dense enough for efficient molecule and dust condensation, the origin of the disk material is still unclear. We aim at studying the kinematics and origin of the disk in the eccentric binary system GG Car, whose primary component is proposed to be a B[e] supergiant. Based on medium- and high-resolution near-infrared spectra we analyzed the CO-band emission detected from GG Car. The complete CO-band structure delivers information on the density and temperature of the emitting region, and the detectable 13CO bands allow us to constrain the evolutionary phase. In addition, the kinematics of the CO gas can be extracted from the shape of the first 12CO band head. We find that the CO gas is located in a ring surrounding the eccentric binary system, and its kinematics agrees with Keplerian rotation with a velocity, projected to the line of sight, of (80pm 1) km/s. The CO ring has a column density of (5pm 3)x10^21 cm^-2 and a temperature of 3200pm 500 K. In addition, the material is chemically enriched in 13CO, which agrees with the primary component being slightly evolved off the main sequence. We discuss two possible scenarios for the origin of the circumbinary disk: (i) non-conservative Roche lobe overflow, and (ii) the possibility that the progenitor of the primary component could have been a classical Be star. Neither can be firmly excluded, but for Roche lobe overflow to occur, a combination of stellar and orbital parameter extremawould be required.
publishDate 2013
dc.date.none.fl_str_mv 2013-01
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/11336/8290
Kraus, M.; Oksala, M. E.; Nickeler, D. H.; Muratore, M. F.; Borges Fernandes, M.; et al.; Molecular emission from GG Carinae's circumbinary disk; Edp Sciences; Astronomy And Astrophysics; 549; A28; 1-2013; 1-8
0004-6361
url http://hdl.handle.net/11336/8290
identifier_str_mv Kraus, M.; Oksala, M. E.; Nickeler, D. H.; Muratore, M. F.; Borges Fernandes, M.; et al.; Molecular emission from GG Carinae's circumbinary disk; Edp Sciences; Astronomy And Astrophysics; 549; A28; 1-2013; 1-8
0004-6361
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2013A%26A...549A..28K
info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2013/01/aa20442-12/aa20442-12.html
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201220442
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
Atribución-NoComercial-CompartirIgual 2.5 Argentina (CC BY-NC-SA 2.5 AR)
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv Atribución-NoComercial-CompartirIgual 2.5 Argentina (CC BY-NC-SA 2.5 AR)
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 13.25334

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