The 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 parsec-scale 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 (
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Abstract B -fields) of 30 Doradus inferred from the far-infrared polarimetric observations by SOFIA/HAWC+ at 89, 154, and 214μ m. TheB -field morphology is complex, showing bending structures around R136. In addition, we use high spectral and angular resolution [Cii ] observations from SOFIA/GREAT and CO(2-1) from APEX. The kinematic structure of the region correlates with theB -field morphology and shows evidence of multiple expanding-shells. OurB -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 350μ G at 89, 154, and 214μ m, 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 theB -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 [Cii ] and CO(2-1) is likely to confirm these suggestions. -
Chuss, David T. ; Andersson, B-G ; Bally, John ; Dotson, Jessie L. ; Darren Dowell, C. ; Guerra, Jordan A. ; Harper, Doyal A. ; Houde, Martin ; Jay Jones, Terry ; Lazarian, A. ; et al ( , The Astrophysical Journal)