Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/8187
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dc.contributor.authorTram, Le Ngoc-
dc.contributor.authorBonne, Lars-
dc.contributor.authorHu, Yue-
dc.contributor.authorLopez-Rodriguez, Enrique-
dc.contributor.authorGuerra, Jordan A-
dc.contributor.authorLesaffre, Pierre-
dc.contributor.authorGusdorf, Antoine-
dc.contributor.authorHoang, Thiem-
dc.contributor.authorLee, Min-Young-
dc.contributor.authorLazarian, Alex-
dc.contributor.authorAndersson, B-G-
dc.contributor.authorCoude, Simon-
dc.contributor.authorArchana Soam-
dc.contributor.authorVacca, William D-
dc.contributor.authorLee, Hyeseung-
dc.contributor.authorGordon, Michael-
dc.date.accessioned2023-04-26T08:43:17Z-
dc.date.available2023-04-26T08:43:17Z-
dc.date.issued2023-03-20-
dc.identifier.citationThe Astrophysical Journal, Vol. 946, No.1, 8en_US
dc.identifier.issn1538-4357-
dc.identifier.urihttp://hdl.handle.net/2248/8187-
dc.descriptionOpen Accessen_US
dc.descriptionOriginal content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.-
dc.description.abstractThe heart of the Large Magellanic Cloud, 30 Doradus, is a complex region with a clear core-halo structure. Feedback from the stellar cluster R136 has been shown to be the main source of energy creating multiple parsecscale expanding-shells in the outer region, and carving a nebula core in the proximity of the ionization source. We present the morphology and strength of the magnetic fields (B-fields) of 30 Doradus inferred from the far-infrared polarimetric observations by SOFIA/HAWC+ at 89, 154, and 214 μm. The B-field morphology is complex, showing bending structures around R136. In addition, we use high spectral and angular resolution [C II] observations from SOFIA/GREAT and CO(2-1) from APEX. The kinematic structure of the region correlates with the B-field morphology and shows evidence of multiple expanding-shells. Our B-field strength maps, estimated using the Davis–Chandrasekhar–Fermi method and structure-function, show variations across the cloud within a maximum of 600, 450, and 350 μG at 89, 154, and 214 μm, respectively. We estimated that the majority of the 30 Doradus clouds are subcritical and sub-Alfvénic. The probability distribution function of the gas density shows that the turbulence is mainly compressively driven, while the plasma beta parameter indicates supersonic turbulence. We show that the B-field is sufficient to hold the cloud structure integrity under feedback from R136. We suggest that supersonic compressive turbulence enables the local gravitational collapse and triggers a new generation of stars to form. The velocity gradient technique using [C II] and CO(2-1) is likely to confirm these suggestions.en_US
dc.language.isoenen_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.urihttps://doi.org/10.3847/1538-4357/acaab0-
dc.rights© 2023. The Author(s).-
dc.subjectInterstellar dusten_US
dc.subjectInterstellar dust extinctionen_US
dc.subjectStar formationen_US
dc.subjectInterstellar magnetic fieldsen_US
dc.subjectMagnetic fieldsen_US
dc.subjectInterstellar dynamicsen_US
dc.subjectStarlight polarizationen_US
dc.subjectLarge magellanic clouden_US
dc.titleSOFIA Observations of 30 Doradus. II. Magnetic Fields and Large-scale Gas Kinematicsen_US
dc.typeArticleen_US
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