Distortion of Magnetic Fields in BHR 71

Kandori, Ryo; Tamura, Motohide; Saito, Masao; Tomisaka, Kohji; Matsumoto, Toshiro; Tazaki, Ryo; Nagata, T.; Kusakabe, Nobuhiko; Kwon, Jungmi; Nagayama, Takahiro; Tatematsu, Ken’ichi

doi:10.3847/1538-4357/ab7b68

Cited by 9 publications

(4 citation statements)

References 58 publications

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“…This leads to the formation of filamentary structures perpendicular to the magnetic field (or perpendicular to the plane of the paper in Figure 14). This mechanism of dense-filament formation was discovered by Inoue & Fukui (2013) and Vaidya et al 2013; see also Arzoumanian et al 2018 andKandori et al 2020 for observational supports). We emphasize that the filaments formed by this mechanism lie perpendicular to the magnetic field, at least when they are first created.…”

Section: Structure Formation In the Interface Layersupporting

confidence: 57%

Cloud-cloud collisions and triggered star formation

Fukui,

Habe,

Inoue

et al. 2020

Preprint

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Star formation is a fundamental process for galactic evolution. One issue over the last several decades has been determining whether star formation is induced by external triggers or is self-regulated in a closed system. The role of an external trigger, which can effectively collect mass in a small volume, has attracted particular attention in connection with the formation of massive stellar clusters, which in the extreme may lead to starbursts. Recent observations have revealed massive cluster formation triggered by cloud-cloud collisions in nearby interacting galaxies, including the Magellanic system and the Antennae Galaxies as well as almost all well-known high-mass star-forming regions such as RCW 120, M20, M42, NGC 6334, etc., in the Milky Way. Theoretical efforts are laying the foundation for the mass compression that causes massive cluster/star formation. Here, we review the recent progress on cloud-cloud collisions and triggered star-cluster formation and discuss the future prospects for this area of research.

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Section: Structure Formation In the Interface Layersupporting

confidence: 57%

Cloud-cloud collisions and triggered star formation

Fukui,

Habe,

Inoue

et al. 2020

Preprint

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“…The morphology of the B-fields is affected by gravity (resulting in a well-known hour-glass shape; Ewertowski & Basu 2013), and regulated by the supersonic gas motion as proposed by Inoue & Fukui (2013). The latter seems to be frequently observed, e.g., deformation of B-field geometry in M16 (Pattle et al 2018), Orion-A (Tahani et al 2019), Musca filament (Bonne et al 2020a(Bonne et al , 2020b, and BHR 71 bipolar outflow system (Kandori et al 2020). Using simulations, Abe et al (2021) demonstrated that a shock with a velocity of ∼7 km s −1 is able to wrap the B-fields.…”

Section: Introductionmentioning

confidence: 98%

SOFIA Observations of 30 Doradus. II. Magnetic Fields and Large-scale Gas Kinematics

Tram

Bonne

et al. 2023

ApJ

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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 (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.

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“…Although lower-mass, BHR 71 appears to be somewhat analogous to CB 54. However, Kandori et al (2020) mapped the magnetic field in BHR 71 using SIRPOL NIR polarimetry at the IRSF, finding the field to be significantly distorted from the mean plane-of-sky field direction in the region. They ascribe this distortion to an interaction between the globule and a large-scale shock (cf.…”

Section: Comparison With Other Regionsmentioning

confidence: 99%

Magnetic fields and outflows in the large Bok globule CB 54

Pattle,

Lai,

Sadavoy

et al. 2022

Preprint

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We have observed the large Bok globule CB 54 in 850𝜇m polarised light using the POL-2 polarimeter on the James Clerk Maxwell Telescope (JCMT). We find that the magnetic field in the periphery of the globule shows significant, ordered deviation from the mean field direction in the globule centre. This deviation appears to correspond with the extended but relatively weak 12 CO outflow emanating from the Class 0 sources at the centre of the globule. Energetics analysis suggests that if the outflow is reshaping the magnetic field in the globule's periphery, then we can place an upper limit of < 27 𝜇G on the magnetic field strength in the globule's periphery. Comparison with archival Planck and CARMA measurements shows that the field in the centre of the globule is consistent over several orders of magnitude in size scale, and oriented parallel to the density structure in the region in projection. We thus hypothesise that while non-thermal motions in the region may be sub-Alfvénic, the magnetic field is subdominant to gravity over a wide range of size scales. Our results suggest that even a relatively weak outflow may be able to significantly reshape magnetic fields in star-forming regions on scales > 0.1 pc.

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Distortion of Magnetic Fields in BHR 71

Cited by 9 publications

References 58 publications

Cloud-cloud collisions and triggered star formation

Cloud-cloud collisions and triggered star formation

SOFIA Observations of 30 Doradus. II. Magnetic Fields and Large-scale Gas Kinematics

Magnetic fields and outflows in the large Bok globule CB 54

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