Gravity-driven Magnetic Field at ∼1000 au Scales in High-mass Star Formation

@article{Sanhueza2021GravitydrivenMF,
  title={Gravity-driven Magnetic Field at ∼1000 au Scales in High-mass Star Formation},
  author={Patricio Sanhueza and Josep Miquel. Girart and Marco Padovani and Daniele Galli and Charles L. H. Hull and Qizhou Zhang and Paulo C. Cort{\'e}s and Ian W. Stephens and Manuel Fern{\'a}ndez-L{\'o}pez and James M. Jackson and Pau Frau and Patrick M. Koch and Benjamin Wu and Luis A. Zapata and Fernando A. Olguin and Xing Lu and Andrea Silva and Ya-Wen Tang and Takeshi Sakai and Andr{\'e}s E. Guzm{\'a}n and Ken’ichi Tatematsu and Fumitaka Nakamura and Huei-Ru Vivien Chen},
  journal={The Astrophysical Journal Letters},
  year={2021},
  volume={915}
}
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… 
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References

SHOWING 1-10 OF 54 REFERENCES
A new probe of magnetic fields during high-mass star formation Zeeman splitting of 6.7 GHz methanol masers
Context. The role of magnetic fields during high-mass star formation is a matter of fierce debate, yet only a few direct probes of magnetic field strengths are available. Aims. The magnetic field is
Magnetic Fields in Massive Star-forming Regions (MagMaR). I. Linear Polarized Imaging of the Ultracompact H ii Region G5.89–0.39
We report 1.2 mm polarized continuum emission observations carried out with the Atacama Large Millimeter/submillimeter Array toward the high-mass star formation region G5.89–0.39. The observations
Digging into the Interior of Hot Cores with ALMA (DIHCA). I. Dissecting the High-mass Star-forming Core G335.579-0.292 MM1
We observed the high-mass star-forming region G335.579–0.292 with the Atacama Large Millimeter/submillimeter Array (ALMA) at 226 GHz with an angular resolution of 0.″3 (∼1000 au resolution at the
Multidirectional Mass Accretion and Collimated Outflows on Scales of 100–2000 au in Early Stages of High-mass Protostars
We observed the W51 high-mass star-forming complex with the Atacama Large Millimeter/submillimeter Array’s longest-baseline configurations, achieving an angular resolution of ∼20 mas, corresponding
The Explosion in Orion-KL as Seen by Mosaicking the Magnetic Field with ALMA
We present the first linear-polarization mosaicked observations performed by the Atacama Large Millimeter/submillimeter Array (ALMA). We mapped the Orion-KLeinmann-Low (Orion-KL) nebula using
Gravity and Rotation Drag the Magnetic Field in High-mass Star Formation
The formation of hot stars out of the cold interstellar medium lies at the heart of astrophysical research. Understanding the importance of magnetic fields during star formation remains a major
Characterizing the Accuracy of ALMA Linear-polarization Mosaics
We characterize the accuracy of linear-polarization mosaics made using the Atacama Large Millimeter/submillimeter Array (ALMA). First, we observed the bright, highly linearly polarized blazar 3C 279
Role and Mechanisms of Angular Momentum Transport During the Formation and Early Evolution of Stars-EES2012
  • 2013
Magnetic Fields in the Infrared Dark Cloud G34.43+0.24
We present the B-fields mapped in IRDC G34.43+0.24 using 850 μm polarized dust emission observed with the POL-2 instrument at the James Clerk Maxwell telescope. We examine the magnetic field
ALMA resolves the hourglass magnetic field in G31.41+0.31
Context. Submillimeter Array (SMA) 870 μm polarization observations of the hot molecular core G31.41+0.31 revealed one of the clearest examples up to date of an hourglass-shaped magnetic field
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