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dc.contributor.author
Añez López, N.
dc.contributor.author
Osorio, M.
dc.contributor.author
Busquet, G.
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Girart, J. M.
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Macías, E.
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Carrasco González, C.
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Curiel, S.
dc.contributor.author
Estalella, R.
dc.contributor.author
Fernandez Lopez, Manuel
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dc.contributor.author
Galván Madrid, R.
dc.contributor.author
Kwon, J.
dc.contributor.author
Torrelles, J. M.
dc.date.available
2020-12-30T13:12:52Z
dc.date.issued
2020-01
dc.identifier.citation
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
dc.identifier.issn
0004-637X
dc.identifier.uri
http://hdl.handle.net/11336/121352
dc.description.abstract
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).
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
IOP Publishing
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
STARS: FORMATION
dc.subject
STARS: MASSIVE
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PROTOPLANETARY DISKS
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Astronomía
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Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2020-09-25T16:48:26Z
dc.identifier.eissn
1538-4357
dc.journal.volume
888
dc.journal.number
1
dc.journal.pagination
1-20
dc.journal.pais
Estados Unidos
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dc.description.fil
Fil: Añez López, N.. Instituto de Ciencias del Espacio; España
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Fil: Osorio, M.. Instituto de Astrofísica de Andalucía; España
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Fil: Busquet, G.. Instituto de Ciencias del Espacio; España
dc.description.fil
Fil: Girart, J. M.. Instituto de Ciencias del Espacio; España
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Fil: Macías, E.. European Southern Observatory; Chile
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Fil: Carrasco González, C.. Instituto de Radioastronomía y Astrofísica; México
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Fil: Curiel, S.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
dc.description.fil
Fil: Estalella, R.. Universidad de Barcelona. Facultad de Física; España
dc.description.fil
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
dc.description.fil
Fil: Galván Madrid, R.. Instituto de Radioastronomía y Astrofísica; México
dc.description.fil
Fil: Kwon, J.. University of tokyo; Japón
dc.description.fil
Fil: Torrelles, J. M.. Institut de Ciencies de l’Espai; España
dc.journal.title
Astrophysical Journal
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ab5dbc
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.3847/1538-4357/ab5dbc
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