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dc.contributor.author
Sanhueza, Patricio
dc.contributor.author
Girart, Josep Miquel
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Padovani, Marco
dc.contributor.author
Galli, Daniele
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Hull, Charles L. H.
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Zhang, Qizhou
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Cortes, Paulo
dc.contributor.author
Stephens, Ian
dc.contributor.author
Fernandez Lopez, Manuel
dc.contributor.author
Jackson, James M.
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Frau, Pau
dc.contributor.author
Kock, Patrick M.
dc.contributor.author
Wu, Benjamin
dc.contributor.author
Zapata, Luis A.
dc.contributor.author
Olguin, Fernando
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Lu, Xing
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Silva, Andrea
dc.contributor.author
Tang, Ya Wen
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Sakai, Takeshi
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Guzmán, Andrés E.
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Tatematsu, Ken'Ichi
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Nakamura, Fumitaka
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Chen, Huei Ru Vivien
dc.date.available
2021-11-05T13:33:31Z
dc.date.issued
2021-07
dc.identifier.citation
Sanhueza, Patricio; Girart, Josep Miquel; Padovani, Marco; Galli, Daniele; Hull, Charles L. H.; et al.; Gravity-driven Magnetic Field at ∼1000 au Scales in High-mass Star Formation; American Astronomical Society; Astrophysical Journal Letters; 915; 1; 7-2021; 1-12
dc.identifier.issn
2041-8205
dc.identifier.uri
http://hdl.handle.net/11336/146109
dc.description.abstract
A full understanding of high-mass star formation requires the study of one of the most elusive components of the energy balance in the interstellar medium: magnetic fields. We report Atacama Large Millimeter/submillimeter Array (ALMA) 1.2 mm, high-resolution (700 au) dust polarization and molecular line observations of the rotating hot molecular core embedded in the high-mass star-forming region IRAS 18089-1732. The dust continuum emission and magnetic field morphology present spiral-like features resembling a whirlpool. The velocity field traced by the H13CO+ (J = 3-2) transition line reveals a complex structure with spiral filaments that are likely infalling and rotating, dragging the field with them. We have modeled the magnetic field and find that the best model corresponds to a weakly magnetized core with a mass-to-magnetic-flux ratio (λ) of 8.38. The modeled magnetic field is dominated by a poloidal component, but with an important contribution from the toroidal component that has a magnitude of 30% of the poloidal component. Using the Davis-Chandrasekhar-Fermi method, we estimate a magnetic field strength of 3.5 mG. At the spatial scales accessible to ALMA, an analysis of the energy balance of the system indicates that gravity overwhelms turbulence, rotation, and the magnetic field. We show that high-mass star formation can occur in weakly magnetized environments, with gravity taking the dominant role.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
American Astronomical Society
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Young stellar objects
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Magnetic fields
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Massive stars
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Star-forming regions
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Astronomía
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Ciencias Físicas
dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
dc.title
Gravity-driven Magnetic Field at ∼1000 au Scales in High-mass Star Formation
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2021-11-04T13:18:18Z
dc.identifier.eissn
2041-8213
dc.journal.volume
915
dc.journal.number
1
dc.journal.pagination
1-12
dc.journal.pais
Estados Unidos
dc.description.fil
Fil: Sanhueza, Patricio. National Astronomical Observatory Of Japan; Japón
dc.description.fil
Fil: Girart, Josep Miquel. Instituto de Estudios Espaciales de Cataluña; España
dc.description.fil
Fil: Padovani, Marco. Osservatorio Astrofisico Di Arcetri; Italia
dc.description.fil
Fil: Galli, Daniele. Osservatorio Astrofisico Di Arcetri; Italia
dc.description.fil
Fil: Hull, Charles L. H.. Atacama Large Millimeter-submillimeter Array; Chile
dc.description.fil
Fil: Zhang, Qizhou. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
dc.description.fil
Fil: Cortes, Paulo. National Radio Astronomy Observatory; Estados Unidos
dc.description.fil
Fil: Stephens, Ian. Worcester State University; Estados Unidos
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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: Jackson, James M.. NASA Ames Research Center; Estados Unidos
dc.description.fil
Fil: Frau, Pau. Csic. Instituto de Ciencias del Espacio; España
dc.description.fil
Fil: Kock, Patrick M.. Academia Sinica; China
dc.description.fil
Fil: Wu, Benjamin. National Astronomical Observatory Of Japan; Japón
dc.description.fil
Fil: Zapata, Luis A.. Instituto de Radioastronomía y Astrofísica; México
dc.description.fil
Fil: Olguin, Fernando. National Tsing Hua University; China
dc.description.fil
Fil: Lu, Xing. National Astronomical Observatory Of Japan; Japón
dc.description.fil
Fil: Silva, Andrea. National Astronomical Observatory Of Japan; Japón
dc.description.fil
Fil: Tang, Ya Wen. Academia Sinica; China
dc.description.fil
Fil: Sakai, Takeshi. The University Of Electro-communications; Japón
dc.description.fil
Fil: Guzmán, Andrés E.. National Astronomical Observatory Of Japan; Japón
dc.description.fil
Fil: Tatematsu, Ken'Ichi. National Astronomical Observatory Of Japan; Japón
dc.description.fil
Fil: Nakamura, Fumitaka. National Astronomical Observatory Of Japan; Japón
dc.description.fil
Fil: Chen, Huei Ru Vivien. National Tsing Hua University; China
dc.journal.title
Astrophysical Journal Letters
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.3847/2041-8213/ac081c
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/2041-8213/ac081c
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