Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.

Autores
Kraus, M.; Cidale, Lydia Sonia; Arias, María Laura; Maravelias, G.; Nickeler, D.; Torres, Andrea Fabiana; Borges Fernandes, M.; Aret, A.; Cure, M.; Vallverdú, R.; Barba, Rodolfo Hector
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. B[e] supergiants are evolved massive stars, enshrouded in a dense wind and surrounded by a molecular and dusty disk. Themechanisms that drive phases of enhanced mass loss and mass ejections, responsible for the shaping of the circumstellar material ofthese objects, are still unclear.Aims. We aim to improve our knowledge on the structure and dynamics of the circumstellar disk of the Large Magellanic Cloud B[e]supergiant LHA 120-S 73.Methods. High-resolution optical and near-infrared spectroscopic data were obtained over a period of 16 and 7 years, respectively.The spectra cover the diagnostic emission lines from [Ca ii] and [O i], as well as the CO bands. These features trace the disk atdifferent distances from the star. We analyzed the kinematics of the individual emission regions by modeling their emission profiles.A low-resolution mid-infrared spectrum was obtained as well, which provides information on the composition of the dusty disk.Results. All diagnostic emission features display double-peaked line profiles, which we interpret as due to Keplerian rotation. We findthat the profile of each forbidden line contains contributions from two spatially clearly distinct rings. In total, we find that LHA 120-S 73 is surrounded by at least four individual rings of material with alternating densities (or by a disk with strongly non-monotonicradial density distribution). Moreover, we find that the molecular ring must have gaps or at least strong density inhomogeneities,or in other words, a clumpy structure. The optical spectra additionally display a broad emission feature at 6160?6180 Å, which weinterpret as molecular emission from TiO. The mid-infrared spectrum displays features of oxygen- and carbon-rich grain species,which indicates a long-lived, stable dusty disk.We cannot confirm the previously reported high value for the stellar rotation velocity. He i λ 5876 is the only clearly detectable pureatmospheric absorption line in our data. Its line profile is strongly variable in both width and shape and resembles of those seen innon-radially pulsating stars. A proper determination of the real underlying stellar rotation velocity is hence not possible.Conclusions. The existence of multiple stable and clumpy rings of alternating density recalls ring structures around planets. Althoughthere is currently insufficient observational evidence, it is tempting to propose a scenario with one (or more) minor bodies or planetsrevolving around LHA 120-S 73 and stabilizing the ring system, in analogy to the shepherd moons in planetary systems.
Fil: Kraus, M.. Astronomický ústav; República Checa
Fil: Cidale, Lydia Sonia. 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: Arias, María Laura. 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. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Maravelias, G.. Astronomický ústav; República Checa
Fil: Nickeler, D.. Astronomický ústav; República Checa
Fil: Torres, Andrea Fabiana. 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: Borges Fernandes, M.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Aret, A.. Tartu Observatory; Estonia
Fil: Cure, M.. Universidad de Valparaíso; Chile
Fil: Vallverdú, R.. 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: Barba, Rodolfo Hector. Universidad de La Serena; Chile
Materia
Circumstellar matter
Infrared stars
Massive stars
LHA 120-S 73 (estrella)
Early type stars
Supergiant 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:11336/37945

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network_name_str CONICET Digital (CONICET)
spelling Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.Kraus, M.Cidale, Lydia SoniaArias, María LauraMaravelias, G.Nickeler, D.Torres, Andrea FabianaBorges Fernandes, M.Aret, A.Cure, M.Vallverdú, R.Barba, Rodolfo HectorCircumstellar matterInfrared starsMassive starsLHA 120-S 73 (estrella)Early type starsSupergiant starshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. B[e] supergiants are evolved massive stars, enshrouded in a dense wind and surrounded by a molecular and dusty disk. Themechanisms that drive phases of enhanced mass loss and mass ejections, responsible for the shaping of the circumstellar material ofthese objects, are still unclear.Aims. We aim to improve our knowledge on the structure and dynamics of the circumstellar disk of the Large Magellanic Cloud B[e]supergiant LHA 120-S 73.Methods. High-resolution optical and near-infrared spectroscopic data were obtained over a period of 16 and 7 years, respectively.The spectra cover the diagnostic emission lines from [Ca ii] and [O i], as well as the CO bands. These features trace the disk atdifferent distances from the star. We analyzed the kinematics of the individual emission regions by modeling their emission profiles.A low-resolution mid-infrared spectrum was obtained as well, which provides information on the composition of the dusty disk.Results. All diagnostic emission features display double-peaked line profiles, which we interpret as due to Keplerian rotation. We findthat the profile of each forbidden line contains contributions from two spatially clearly distinct rings. In total, we find that LHA 120-S 73 is surrounded by at least four individual rings of material with alternating densities (or by a disk with strongly non-monotonicradial density distribution). Moreover, we find that the molecular ring must have gaps or at least strong density inhomogeneities,or in other words, a clumpy structure. The optical spectra additionally display a broad emission feature at 6160?6180 Å, which weinterpret as molecular emission from TiO. The mid-infrared spectrum displays features of oxygen- and carbon-rich grain species,which indicates a long-lived, stable dusty disk.We cannot confirm the previously reported high value for the stellar rotation velocity. He i λ 5876 is the only clearly detectable pureatmospheric absorption line in our data. Its line profile is strongly variable in both width and shape and resembles of those seen innon-radially pulsating stars. A proper determination of the real underlying stellar rotation velocity is hence not possible.Conclusions. The existence of multiple stable and clumpy rings of alternating density recalls ring structures around planets. Althoughthere is currently insufficient observational evidence, it is tempting to propose a scenario with one (or more) minor bodies or planetsrevolving around LHA 120-S 73 and stabilizing the ring system, in analogy to the shepherd moons in planetary systems.Fil: Kraus, M.. Astronomický ústav; República ChecaFil: Cidale, Lydia Sonia. 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: Arias, María Laura. 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. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Maravelias, G.. Astronomický ústav; República ChecaFil: Nickeler, D.. Astronomický ústav; República ChecaFil: Torres, Andrea Fabiana. 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: Borges Fernandes, M.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Aret, A.. Tartu Observatory; EstoniaFil: Cure, M.. Universidad de Valparaíso; ChileFil: Vallverdú, R.. 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: Barba, Rodolfo Hector. Universidad de La Serena; ChileEDP Sciences2016-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/37945Kraus, M.; Cidale, Lydia Sonia; Arias, María Laura; Maravelias, G.; Nickeler, D.; et al.; Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.; EDP Sciences; Astronomy and Astrophysics; 593; 7-2016; 1-130004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628493info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2016/09/aa28493-16/aa28493-16.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 Técnicas2025-09-29T10:01:55Zoai:ri.conicet.gov.ar:11336/37945instacron: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 10:01:55.295CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.
title Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.
spellingShingle Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.
Kraus, M.
Circumstellar matter
Infrared stars
Massive stars
LHA 120-S 73 (estrella)
Early type stars
Supergiant stars
title_short Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.
title_full Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.
title_fullStr Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.
title_full_unstemmed Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.
title_sort Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.
dc.creator.none.fl_str_mv Kraus, M.
Cidale, Lydia Sonia
Arias, María Laura
Maravelias, G.
Nickeler, D.
Torres, Andrea Fabiana
Borges Fernandes, M.
Aret, A.
Cure, M.
Vallverdú, R.
Barba, Rodolfo Hector
author Kraus, M.
author_facet Kraus, M.
Cidale, Lydia Sonia
Arias, María Laura
Maravelias, G.
Nickeler, D.
Torres, Andrea Fabiana
Borges Fernandes, M.
Aret, A.
Cure, M.
Vallverdú, R.
Barba, Rodolfo Hector
author_role author
author2 Cidale, Lydia Sonia
Arias, María Laura
Maravelias, G.
Nickeler, D.
Torres, Andrea Fabiana
Borges Fernandes, M.
Aret, A.
Cure, M.
Vallverdú, R.
Barba, Rodolfo Hector
author2_role author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Circumstellar matter
Infrared stars
Massive stars
LHA 120-S 73 (estrella)
Early type stars
Supergiant stars
topic Circumstellar matter
Infrared stars
Massive stars
LHA 120-S 73 (estrella)
Early type stars
Supergiant stars
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. B[e] supergiants are evolved massive stars, enshrouded in a dense wind and surrounded by a molecular and dusty disk. Themechanisms that drive phases of enhanced mass loss and mass ejections, responsible for the shaping of the circumstellar material ofthese objects, are still unclear.Aims. We aim to improve our knowledge on the structure and dynamics of the circumstellar disk of the Large Magellanic Cloud B[e]supergiant LHA 120-S 73.Methods. High-resolution optical and near-infrared spectroscopic data were obtained over a period of 16 and 7 years, respectively.The spectra cover the diagnostic emission lines from [Ca ii] and [O i], as well as the CO bands. These features trace the disk atdifferent distances from the star. We analyzed the kinematics of the individual emission regions by modeling their emission profiles.A low-resolution mid-infrared spectrum was obtained as well, which provides information on the composition of the dusty disk.Results. All diagnostic emission features display double-peaked line profiles, which we interpret as due to Keplerian rotation. We findthat the profile of each forbidden line contains contributions from two spatially clearly distinct rings. In total, we find that LHA 120-S 73 is surrounded by at least four individual rings of material with alternating densities (or by a disk with strongly non-monotonicradial density distribution). Moreover, we find that the molecular ring must have gaps or at least strong density inhomogeneities,or in other words, a clumpy structure. The optical spectra additionally display a broad emission feature at 6160?6180 Å, which weinterpret as molecular emission from TiO. The mid-infrared spectrum displays features of oxygen- and carbon-rich grain species,which indicates a long-lived, stable dusty disk.We cannot confirm the previously reported high value for the stellar rotation velocity. He i λ 5876 is the only clearly detectable pureatmospheric absorption line in our data. Its line profile is strongly variable in both width and shape and resembles of those seen innon-radially pulsating stars. A proper determination of the real underlying stellar rotation velocity is hence not possible.Conclusions. The existence of multiple stable and clumpy rings of alternating density recalls ring structures around planets. Althoughthere is currently insufficient observational evidence, it is tempting to propose a scenario with one (or more) minor bodies or planetsrevolving around LHA 120-S 73 and stabilizing the ring system, in analogy to the shepherd moons in planetary systems.
Fil: Kraus, M.. Astronomický ústav; República Checa
Fil: Cidale, Lydia Sonia. 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: Arias, María Laura. 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. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Maravelias, G.. Astronomický ústav; República Checa
Fil: Nickeler, D.. Astronomický ústav; República Checa
Fil: Torres, Andrea Fabiana. 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: Borges Fernandes, M.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Aret, A.. Tartu Observatory; Estonia
Fil: Cure, M.. Universidad de Valparaíso; Chile
Fil: Vallverdú, R.. 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: Barba, Rodolfo Hector. Universidad de La Serena; Chile
description Context. B[e] supergiants are evolved massive stars, enshrouded in a dense wind and surrounded by a molecular and dusty disk. Themechanisms that drive phases of enhanced mass loss and mass ejections, responsible for the shaping of the circumstellar material ofthese objects, are still unclear.Aims. We aim to improve our knowledge on the structure and dynamics of the circumstellar disk of the Large Magellanic Cloud B[e]supergiant LHA 120-S 73.Methods. High-resolution optical and near-infrared spectroscopic data were obtained over a period of 16 and 7 years, respectively.The spectra cover the diagnostic emission lines from [Ca ii] and [O i], as well as the CO bands. These features trace the disk atdifferent distances from the star. We analyzed the kinematics of the individual emission regions by modeling their emission profiles.A low-resolution mid-infrared spectrum was obtained as well, which provides information on the composition of the dusty disk.Results. All diagnostic emission features display double-peaked line profiles, which we interpret as due to Keplerian rotation. We findthat the profile of each forbidden line contains contributions from two spatially clearly distinct rings. In total, we find that LHA 120-S 73 is surrounded by at least four individual rings of material with alternating densities (or by a disk with strongly non-monotonicradial density distribution). Moreover, we find that the molecular ring must have gaps or at least strong density inhomogeneities,or in other words, a clumpy structure. The optical spectra additionally display a broad emission feature at 6160?6180 Å, which weinterpret as molecular emission from TiO. The mid-infrared spectrum displays features of oxygen- and carbon-rich grain species,which indicates a long-lived, stable dusty disk.We cannot confirm the previously reported high value for the stellar rotation velocity. He i λ 5876 is the only clearly detectable pureatmospheric absorption line in our data. Its line profile is strongly variable in both width and shape and resembles of those seen innon-radially pulsating stars. A proper determination of the real underlying stellar rotation velocity is hence not possible.Conclusions. The existence of multiple stable and clumpy rings of alternating density recalls ring structures around planets. Althoughthere is currently insufficient observational evidence, it is tempting to propose a scenario with one (or more) minor bodies or planetsrevolving around LHA 120-S 73 and stabilizing the ring system, in analogy to the shepherd moons in planetary systems.
publishDate 2016
dc.date.none.fl_str_mv 2016-07
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/11336/37945
Kraus, M.; Cidale, Lydia Sonia; Arias, María Laura; Maravelias, G.; Nickeler, D.; et al.; Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.; EDP Sciences; Astronomy and Astrophysics; 593; 7-2016; 1-13
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/37945
identifier_str_mv Kraus, M.; Cidale, Lydia Sonia; Arias, María Laura; Maravelias, G.; Nickeler, D.; et al.; Inhomogeneous molecular ring around the B[e] supergiant LHA 120-S 73.; EDP Sciences; Astronomy and Astrophysics; 593; 7-2016; 1-13
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
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dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
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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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