2021
DOI: 10.3847/2041-8213/ac081c
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Gravity-driven Magnetic Field at ∼1000 au Scales in High-mass Star Formation

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 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 H … Show more

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Cited by 63 publications
(64 citation statements)
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“…With recently observed streamers into the Class 0 object Per-emb-2 (Pineda et al 2020), the arc seen by Grant et al (2021) in [MGM2012] 512, and the field configuration in HH211 (Lee et al 2019), there are observational possibilities to examine spiralling inflows. Sanhueza et al (2021) have also been able to demonstrate streamers in massive star formation environment of IRAS 18089-1732. Spiral behaviour can also happen in a disk plane, like in HH 111 VLA 1 as observed by Lee et al (2020).…”
Section: Focused On Finding Potential Observable Features)mentioning
confidence: 89%
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“…With recently observed streamers into the Class 0 object Per-emb-2 (Pineda et al 2020), the arc seen by Grant et al (2021) in [MGM2012] 512, and the field configuration in HH211 (Lee et al 2019), there are observational possibilities to examine spiralling inflows. Sanhueza et al (2021) have also been able to demonstrate streamers in massive star formation environment of IRAS 18089-1732. Spiral behaviour can also happen in a disk plane, like in HH 111 VLA 1 as observed by Lee et al (2020).…”
Section: Focused On Finding Potential Observable Features)mentioning
confidence: 89%
“…These would be values between our models I and H, though those are not directly comparable, as our models do not examine massive star formation, and the basis for computing values of λ is different. Sanhueza et al (2021) show that IRAS 18089-1732 consist on one spiral streamer and two inflow filaments. Based on polarization estimates, the magnetic field is following the spiral geometry of the streamers/filaments and it is substantially toroidal.…”
Section: Iras 18089-1732mentioning
confidence: 89%
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“…At the core scale, no strong correlation between outflow axis and magnetic field has been reported in both low-mass (e.g., Hull et al 2014;Hull & Zhang 2019) and highmass star-forming regions (Zhang et al 2014;Baug et al 2020). This lack of correlation implies that the role of magnetic fields is less important than both gravity and angular momentum from the core to disk scales (e.g., Sanhueza et al 2021). A random distribution of outflow-filament orientation has also been found in both low-mass and high-mass star-forming regions (Tatematsu et al 2016;Stephens et al 2017;Baug et al 2020).…”
Section: Position Angle Of Outflowsmentioning
confidence: 99%
“…Moreover, the B-fields may provide some support against collapse. One much smaller scales (1000 -10000 au), YSOs themselves can have diverse magnetic field morphologies such as spiral-like, hourglass, and radial (e.g., as seen in the MAGMAR survey; Cortes et al 2021;Fernández-López et al 2021;Sanhueza et al 2021). Focusing on the large-scale observations of filaments, it is important to establish if fields are universally perpendicular to the spines of the main filament and whether the B-field strength is sufficient to help support the filament from collapse.…”
Section: Introductionmentioning
confidence: 99%