Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1

Autores
Añez López, N.; Osorio, M.; Busquet, G.; Girart, J. M.; Macías, E.; Carrasco González, C.; Curiel, S.; Estalella, R.; Fernandez Lopez, Manuel; Galván Madrid, R.; Kwon, J.; Torrelles, J. M.
Año de publicación
2020
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Recent high angular resolution (≃40 mas) ALMA observations at 1.14 mm resolve a compact (R ≃ 200 au), flattened dust structure perpendicular to the HH 80─81 jet emanating from the GGD 27-MM1 high-mass protostar, making it a robust candidate for a true accretion disk. The jet─disk system (HH 80─81/GGD 27-MM1) resembles those found in association with low- and intermediate-mass protostars. We present radiative transfer models that fit the 1.14 mm ALMA dust image of this disk, which allow us to obtain its physical parameters and predict its density and temperature structure. Our results indicate that this accretion disk is compact (R disk ≃ 170 au) and massive (≃5 M ☉), at about 20% of the stellar mass of ≃20 M ☉. We estimate the total dynamical mass of the star─disk system from the molecular line emission, finding a range between 21 and 30 M ☉, which is consistent with our model. We fit the density and temperature structures found by our model with power-law functions. These results suggest that accretion disks around massive stars are more massive and hotter than their low-mass siblings, but they still are quite stable. We also compare the temperature distribution in the GGD 27─MM1 disk with that found in low- and intermediate-mass stars and discuss possible implications for the water snow line. We have also carried out a study of the distance based on Gaia DR2 data and the population of young stellar objects in this region and from the extinction maps. We conclude that the source distance is within 1.2 and 1.4 kpc, closer than what was derived in previous studies (1.7 kpc).
Fil: Añez López, N.. Instituto de Ciencias del Espacio; España
Fil: Osorio, M.. Instituto de Astrofísica de Andalucía; España
Fil: Busquet, G.. Instituto de Ciencias del Espacio; España
Fil: Girart, J. M.. Instituto de Ciencias del Espacio; España
Fil: Macías, E.. European Southern Observatory; Chile
Fil: Carrasco González, C.. Instituto de Radioastronomía y Astrofísica; México
Fil: Curiel, S.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: Estalella, R.. Universidad de Barcelona. Facultad de Física; España
Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Galván Madrid, R.. Instituto de Radioastronomía y Astrofísica; México
Fil: Kwon, J.. University of tokyo; Japón
Fil: Torrelles, J. M.. Institut de Ciencies de l’Espai; España
Materia
STARS: FORMATION
STARS: MASSIVE
PROTOPLANETARY DISKS
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:11336/121352
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/121352
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1Añez López, N.Osorio, M.Busquet, G.Girart, J. M.Macías, E.Carrasco González, C.Curiel, S.Estalella, R.Fernandez Lopez, ManuelGalván Madrid, R.Kwon, J.Torrelles, J. M.STARS: FORMATIONSTARS: MASSIVEPROTOPLANETARY DISKShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Recent high angular resolution (≃40 mas) ALMA observations at 1.14 mm resolve a compact (R ≃ 200 au), flattened dust structure perpendicular to the HH 80─81 jet emanating from the GGD 27-MM1 high-mass protostar, making it a robust candidate for a true accretion disk. The jet─disk system (HH 80─81/GGD 27-MM1) resembles those found in association with low- and intermediate-mass protostars. We present radiative transfer models that fit the 1.14 mm ALMA dust image of this disk, which allow us to obtain its physical parameters and predict its density and temperature structure. Our results indicate that this accretion disk is compact (R disk ≃ 170 au) and massive (≃5 M ☉), at about 20% of the stellar mass of ≃20 M ☉. We estimate the total dynamical mass of the star─disk system from the molecular line emission, finding a range between 21 and 30 M ☉, which is consistent with our model. We fit the density and temperature structures found by our model with power-law functions. These results suggest that accretion disks around massive stars are more massive and hotter than their low-mass siblings, but they still are quite stable. We also compare the temperature distribution in the GGD 27─MM1 disk with that found in low- and intermediate-mass stars and discuss possible implications for the water snow line. We have also carried out a study of the distance based on Gaia DR2 data and the population of young stellar objects in this region and from the extinction maps. We conclude that the source distance is within 1.2 and 1.4 kpc, closer than what was derived in previous studies (1.7 kpc).Fil: Añez López, N.. Instituto de Ciencias del Espacio; EspañaFil: Osorio, M.. Instituto de Astrofísica de Andalucía; EspañaFil: Busquet, G.. Instituto de Ciencias del Espacio; EspañaFil: Girart, J. M.. Instituto de Ciencias del Espacio; EspañaFil: Macías, E.. European Southern Observatory; ChileFil: Carrasco González, C.. Instituto de Radioastronomía y Astrofísica; MéxicoFil: Curiel, S.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; MéxicoFil: Estalella, R.. Universidad de Barcelona. Facultad de Física; EspañaFil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Galván Madrid, R.. Instituto de Radioastronomía y Astrofísica; MéxicoFil: Kwon, J.. University of tokyo; JapónFil: Torrelles, J. M.. Institut de Ciencies de l’Espai; EspañaIOP Publishing2020-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/121352Añez López, N.; Osorio, M.; Busquet, G.; Girart, J. M.; Macías, E.; et al.; Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1; IOP Publishing; Astrophysical Journal; 888; 1; 1-2020; 1-200004-637X1538-4357CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ab5dbcinfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ab5dbcinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:46:19Zoai:ri.conicet.gov.ar:11336/121352instacron: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 11:46:20.008CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1
title Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1
spellingShingle Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1
Añez López, N.
STARS: FORMATION
STARS: MASSIVE
PROTOPLANETARY DISKS
title_short Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1
title_full Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1
title_fullStr Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1
title_full_unstemmed Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1
title_sort Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1
dc.creator.none.fl_str_mv Añez López, N.
Osorio, M.
Busquet, G.
Girart, J. M.
Macías, E.
Carrasco González, C.
Curiel, S.
Estalella, R.
Fernandez Lopez, Manuel
Galván Madrid, R.
Kwon, J.
Torrelles, J. M.
author Añez López, N.
author_facet Añez López, N.
Osorio, M.
Busquet, G.
Girart, J. M.
Macías, E.
Carrasco González, C.
Curiel, S.
Estalella, R.
Fernandez Lopez, Manuel
Galván Madrid, R.
Kwon, J.
Torrelles, J. M.
author_role author
author2 Osorio, M.
Busquet, G.
Girart, J. M.
Macías, E.
Carrasco González, C.
Curiel, S.
Estalella, R.
Fernandez Lopez, Manuel
Galván Madrid, R.
Kwon, J.
Torrelles, J. M.
author2_role author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv STARS: FORMATION
STARS: MASSIVE
PROTOPLANETARY DISKS
topic STARS: FORMATION
STARS: MASSIVE
PROTOPLANETARY DISKS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Recent high angular resolution (≃40 mas) ALMA observations at 1.14 mm resolve a compact (R ≃ 200 au), flattened dust structure perpendicular to the HH 80─81 jet emanating from the GGD 27-MM1 high-mass protostar, making it a robust candidate for a true accretion disk. The jet─disk system (HH 80─81/GGD 27-MM1) resembles those found in association with low- and intermediate-mass protostars. We present radiative transfer models that fit the 1.14 mm ALMA dust image of this disk, which allow us to obtain its physical parameters and predict its density and temperature structure. Our results indicate that this accretion disk is compact (R disk ≃ 170 au) and massive (≃5 M ☉), at about 20% of the stellar mass of ≃20 M ☉. We estimate the total dynamical mass of the star─disk system from the molecular line emission, finding a range between 21 and 30 M ☉, which is consistent with our model. We fit the density and temperature structures found by our model with power-law functions. These results suggest that accretion disks around massive stars are more massive and hotter than their low-mass siblings, but they still are quite stable. We also compare the temperature distribution in the GGD 27─MM1 disk with that found in low- and intermediate-mass stars and discuss possible implications for the water snow line. We have also carried out a study of the distance based on Gaia DR2 data and the population of young stellar objects in this region and from the extinction maps. We conclude that the source distance is within 1.2 and 1.4 kpc, closer than what was derived in previous studies (1.7 kpc).
Fil: Añez López, N.. Instituto de Ciencias del Espacio; España
Fil: Osorio, M.. Instituto de Astrofísica de Andalucía; España
Fil: Busquet, G.. Instituto de Ciencias del Espacio; España
Fil: Girart, J. M.. Instituto de Ciencias del Espacio; España
Fil: Macías, E.. European Southern Observatory; Chile
Fil: Carrasco González, C.. Instituto de Radioastronomía y Astrofísica; México
Fil: Curiel, S.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: Estalella, R.. Universidad de Barcelona. Facultad de Física; España
Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Galván Madrid, R.. Instituto de Radioastronomía y Astrofísica; México
Fil: Kwon, J.. University of tokyo; Japón
Fil: Torrelles, J. M.. Institut de Ciencies de l’Espai; España
description Recent high angular resolution (≃40 mas) ALMA observations at 1.14 mm resolve a compact (R ≃ 200 au), flattened dust structure perpendicular to the HH 80─81 jet emanating from the GGD 27-MM1 high-mass protostar, making it a robust candidate for a true accretion disk. The jet─disk system (HH 80─81/GGD 27-MM1) resembles those found in association with low- and intermediate-mass protostars. We present radiative transfer models that fit the 1.14 mm ALMA dust image of this disk, which allow us to obtain its physical parameters and predict its density and temperature structure. Our results indicate that this accretion disk is compact (R disk ≃ 170 au) and massive (≃5 M ☉), at about 20% of the stellar mass of ≃20 M ☉. We estimate the total dynamical mass of the star─disk system from the molecular line emission, finding a range between 21 and 30 M ☉, which is consistent with our model. We fit the density and temperature structures found by our model with power-law functions. These results suggest that accretion disks around massive stars are more massive and hotter than their low-mass siblings, but they still are quite stable. We also compare the temperature distribution in the GGD 27─MM1 disk with that found in low- and intermediate-mass stars and discuss possible implications for the water snow line. We have also carried out a study of the distance based on Gaia DR2 data and the population of young stellar objects in this region and from the extinction maps. We conclude that the source distance is within 1.2 and 1.4 kpc, closer than what was derived in previous studies (1.7 kpc).
publishDate 2020
dc.date.none.fl_str_mv 2020-01
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/11336/121352
Añez López, N.; Osorio, M.; Busquet, G.; Girart, J. M.; Macías, E.; et al.; Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1; IOP Publishing; Astrophysical Journal; 888; 1; 1-2020; 1-20
0004-637X
1538-4357
CONICET Digital
CONICET
url http://hdl.handle.net/11336/121352
identifier_str_mv Añez López, N.; Osorio, M.; Busquet, G.; Girart, J. M.; Macías, E.; et al.; Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1; IOP Publishing; Astrophysical Journal; 888; 1; 1-2020; 1-20
0004-637X
1538-4357
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ab5dbc
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ab5dbc
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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score 12.982451

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