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dc.contributor.author
Sanhueza, Patricio  
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Girart, Josep Miquel  
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Padovani, Marco  
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Galli, Daniele  
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Hull, Charles L. H.  
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Zhang, Qizhou  
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Cortes, Paulo  
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Stephens, Ian  
dc.contributor.author
Fernandez Lopez, Manuel  
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Jackson, James M.  
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Frau, Pau  
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Kock, Patrick M.  
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Wu, Benjamin  
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Zapata, Luis A.  
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Olguin, Fernando  
dc.contributor.author
Lu, Xing  
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Silva, Andrea  
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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  
dc.subject.classification
Astronomía  
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Ciencias Físicas  
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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  
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Fil: Girart, Josep Miquel. Instituto de Estudios Espaciales de Cataluña; España  
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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  
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Fil: Zhang, Qizhou. Harvard-Smithsonian Center for Astrophysics; Estados Unidos  
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Fil: Cortes, Paulo. National Radio Astronomy Observatory; Estados Unidos  
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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  
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Fil: Frau, Pau. Csic. Instituto de Ciencias del Espacio; España  
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Fil: Kock, Patrick M.. Academia Sinica; China  
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Fil: Wu, Benjamin. National Astronomical Observatory Of Japan; Japón  
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Fil: Zapata, Luis A.. Instituto de Radioastronomía y Astrofísica; México  
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Fil: Olguin, Fernando. National Tsing Hua University; China  
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Fil: Lu, Xing. National Astronomical Observatory Of Japan; Japón  
dc.description.fil
Fil: Silva, Andrea. National Astronomical Observatory Of Japan; Japón  
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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  
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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