Observational constraints for the circumstellar disk of the B star CPD-529243

Autores
Cidale, Lydia Sonia; Borges Fernandes, M.; Andruchow, Ileana; Arias, María Laura; Kraus, M.; Chesneau, O.; Kanaan, S.; Curé, M.; De Wit, W. J.; Muratore, María Florencia
Año de publicación
2012
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. The formation and evolution of gas and dust environments around B[e] supergiants are still open issues. Aims. We intend to study the geometry, kinematics and physical structure of the circumstellar environment (CE) of the B[e] supergiant CPD-52 9243 to provide further insights into the underlying mechanism causing the B[e] phenomenon. Methods. The influence of the different physical mechanisms acting on the CE (radiation pressure, rotation, bi-stability or tidal forces) is somehow reflected in the shape and kinematic properties of the gas and dust regions (flaring, Keplerian, accretion or outflowing disks). To investigate these processes we mainly used quasi-simultaneous observations taken with high spatial resolution optical long-baseline interferometry (VLTI/MIDI), near-IR spectroscopy of CO bandhead features (Gemini/Phoenix and VLT/CRIRES) and optical spectra (CASLEO/REOSC). Results. High angular resolution interferometric measurements obtained with VLTI/MIDI provide strong support for the presence of a dusty disk(ring)-like structure around CPD-52 9243, with an upper limit for its inner edge of ~8 mas (~27.5 AU, considering a distance of 3.44 kpc to the star). The disk has an inclination angle with respect to the line of sight of 46 ± 7°. The study of CO first overtone bandhead evidences a disk structure in Keplerian rotation. The optical spectrum indicates a rapid outflow in the polar direction. Conclusions. The IR emission (CO and warm dust) indicates Keplerian rotation in a circumstellar disk while the optical line transitions of various species are consistent with a polar wind. Both structures appear simultaneously and provide further evidence for the proposed paradigms of the mass-loss in supergiant B[e] stars. The presence of a detached cold CO ring around CPD-52 9243 could be due to a truncation of the inner disk caused by a companion, located possibly interior to the disk rim, clearing the center of the system. More spectroscopic and interferometric data are necessary to determine a possible binary nature of the star.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
Circumstellar matter
Stars: individual: CPD-52 9243
Stars: mass-loss
Stars: winds, outflows
Supergiants
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/84084

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/84084
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Observational constraints for the circumstellar disk of the B star CPD-529243Cidale, Lydia SoniaBorges Fernandes, M.Andruchow, IleanaArias, María LauraKraus, M.Chesneau, O.Kanaan, S.Curé, M.De Wit, W. J.Muratore, María FlorenciaCiencias AstronómicasCircumstellar matterStars: individual: CPD-52 9243Stars: mass-lossStars: winds, outflowsSupergiants<b>Context.</b> The formation and evolution of gas and dust environments around B[e] supergiants are still open issues. <b>Aims.</b> We intend to study the geometry, kinematics and physical structure of the circumstellar environment (CE) of the B[e] supergiant CPD-52 9243 to provide further insights into the underlying mechanism causing the B[e] phenomenon. <b>Methods.</b> The influence of the different physical mechanisms acting on the CE (radiation pressure, rotation, bi-stability or tidal forces) is somehow reflected in the shape and kinematic properties of the gas and dust regions (flaring, Keplerian, accretion or outflowing disks). To investigate these processes we mainly used quasi-simultaneous observations taken with high spatial resolution optical long-baseline interferometry (VLTI/MIDI), near-IR spectroscopy of CO bandhead features (Gemini/Phoenix and VLT/CRIRES) and optical spectra (CASLEO/REOSC). <b>Results.</b> High angular resolution interferometric measurements obtained with VLTI/MIDI provide strong support for the presence of a dusty disk(ring)-like structure around CPD-52 9243, with an upper limit for its inner edge of ~8 mas (~27.5 AU, considering a distance of 3.44 kpc to the star). The disk has an inclination angle with respect to the line of sight of 46 ± 7°. The study of CO first overtone bandhead evidences a disk structure in Keplerian rotation. The optical spectrum indicates a rapid outflow in the polar direction. <b>Conclusions.</b> The IR emission (CO and warm dust) indicates Keplerian rotation in a circumstellar disk while the optical line transitions of various species are consistent with a polar wind. Both structures appear simultaneously and provide further evidence for the proposed paradigms of the mass-loss in supergiant B[e] stars. The presence of a detached cold CO ring around CPD-52 9243 could be due to a truncation of the inner disk caused by a companion, located possibly interior to the disk rim, clearing the center of the system. More spectroscopic and interferometric data are necessary to determine a possible binary nature of the star.Facultad de Ciencias Astronómicas y Geofísicas2012-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/84084enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201220120info: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:UNLP2025-09-29T11:16:01Zoai:sedici.unlp.edu.ar:10915/84084Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:01.434SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Observational constraints for the circumstellar disk of the B star CPD-529243
title Observational constraints for the circumstellar disk of the B star CPD-529243
spellingShingle Observational constraints for the circumstellar disk of the B star CPD-529243
Cidale, Lydia Sonia
Ciencias Astronómicas
Circumstellar matter
Stars: individual: CPD-52 9243
Stars: mass-loss
Stars: winds, outflows
Supergiants
title_short Observational constraints for the circumstellar disk of the B star CPD-529243
title_full Observational constraints for the circumstellar disk of the B star CPD-529243
title_fullStr Observational constraints for the circumstellar disk of the B star CPD-529243
title_full_unstemmed Observational constraints for the circumstellar disk of the B star CPD-529243
title_sort Observational constraints for the circumstellar disk of the B star CPD-529243
dc.creator.none.fl_str_mv Cidale, Lydia Sonia
Borges Fernandes, M.
Andruchow, Ileana
Arias, María Laura
Kraus, M.
Chesneau, O.
Kanaan, S.
Curé, M.
De Wit, W. J.
Muratore, María Florencia
author Cidale, Lydia Sonia
author_facet Cidale, Lydia Sonia
Borges Fernandes, M.
Andruchow, Ileana
Arias, María Laura
Kraus, M.
Chesneau, O.
Kanaan, S.
Curé, M.
De Wit, W. J.
Muratore, María Florencia
author_role author
author2 Borges Fernandes, M.
Andruchow, Ileana
Arias, María Laura
Kraus, M.
Chesneau, O.
Kanaan, S.
Curé, M.
De Wit, W. J.
Muratore, María Florencia
author2_role author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Circumstellar matter
Stars: individual: CPD-52 9243
Stars: mass-loss
Stars: winds, outflows
Supergiants
topic Ciencias Astronómicas
Circumstellar matter
Stars: individual: CPD-52 9243
Stars: mass-loss
Stars: winds, outflows
Supergiants
dc.description.none.fl_txt_mv <b>Context.</b> The formation and evolution of gas and dust environments around B[e] supergiants are still open issues. <b>Aims.</b> We intend to study the geometry, kinematics and physical structure of the circumstellar environment (CE) of the B[e] supergiant CPD-52 9243 to provide further insights into the underlying mechanism causing the B[e] phenomenon. <b>Methods.</b> The influence of the different physical mechanisms acting on the CE (radiation pressure, rotation, bi-stability or tidal forces) is somehow reflected in the shape and kinematic properties of the gas and dust regions (flaring, Keplerian, accretion or outflowing disks). To investigate these processes we mainly used quasi-simultaneous observations taken with high spatial resolution optical long-baseline interferometry (VLTI/MIDI), near-IR spectroscopy of CO bandhead features (Gemini/Phoenix and VLT/CRIRES) and optical spectra (CASLEO/REOSC). <b>Results.</b> High angular resolution interferometric measurements obtained with VLTI/MIDI provide strong support for the presence of a dusty disk(ring)-like structure around CPD-52 9243, with an upper limit for its inner edge of ~8 mas (~27.5 AU, considering a distance of 3.44 kpc to the star). The disk has an inclination angle with respect to the line of sight of 46 ± 7°. The study of CO first overtone bandhead evidences a disk structure in Keplerian rotation. The optical spectrum indicates a rapid outflow in the polar direction. <b>Conclusions.</b> The IR emission (CO and warm dust) indicates Keplerian rotation in a circumstellar disk while the optical line transitions of various species are consistent with a polar wind. Both structures appear simultaneously and provide further evidence for the proposed paradigms of the mass-loss in supergiant B[e] stars. The presence of a detached cold CO ring around CPD-52 9243 could be due to a truncation of the inner disk caused by a companion, located possibly interior to the disk rim, clearing the center of the system. More spectroscopic and interferometric data are necessary to determine a possible binary nature of the star.
Facultad de Ciencias Astronómicas y Geofísicas
description <b>Context.</b> The formation and evolution of gas and dust environments around B[e] supergiants are still open issues. <b>Aims.</b> We intend to study the geometry, kinematics and physical structure of the circumstellar environment (CE) of the B[e] supergiant CPD-52 9243 to provide further insights into the underlying mechanism causing the B[e] phenomenon. <b>Methods.</b> The influence of the different physical mechanisms acting on the CE (radiation pressure, rotation, bi-stability or tidal forces) is somehow reflected in the shape and kinematic properties of the gas and dust regions (flaring, Keplerian, accretion or outflowing disks). To investigate these processes we mainly used quasi-simultaneous observations taken with high spatial resolution optical long-baseline interferometry (VLTI/MIDI), near-IR spectroscopy of CO bandhead features (Gemini/Phoenix and VLT/CRIRES) and optical spectra (CASLEO/REOSC). <b>Results.</b> High angular resolution interferometric measurements obtained with VLTI/MIDI provide strong support for the presence of a dusty disk(ring)-like structure around CPD-52 9243, with an upper limit for its inner edge of ~8 mas (~27.5 AU, considering a distance of 3.44 kpc to the star). The disk has an inclination angle with respect to the line of sight of 46 ± 7°. The study of CO first overtone bandhead evidences a disk structure in Keplerian rotation. The optical spectrum indicates a rapid outflow in the polar direction. <b>Conclusions.</b> The IR emission (CO and warm dust) indicates Keplerian rotation in a circumstellar disk while the optical line transitions of various species are consistent with a polar wind. Both structures appear simultaneously and provide further evidence for the proposed paradigms of the mass-loss in supergiant B[e] stars. The presence of a detached cold CO ring around CPD-52 9243 could be due to a truncation of the inner disk caused by a companion, located possibly interior to the disk rim, clearing the center of the system. More spectroscopic and interferometric data are necessary to determine a possible binary nature of the star.
publishDate 2012
dc.date.none.fl_str_mv 2012-12
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info:eu-repo/semantics/publishedVersion
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status_str publishedVersion
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info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201220120
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)
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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)
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