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

Sanhueza, Patricio; Girart, J. M.; Padovani, M.; Galli, Daniele; Hull, Charles L. H.; Zhang, Qizhou; Cortés, Paulo C.; Stephens, Ian; Fernández-López, Manuel; Jackson, James M.; Frau, P.; Koch, Patrick M.; Wu, Benjamin; Zapata, Luis A.; Olguin, Fernando A.; Lu, Xing; Silva, Andréa; Tang, Ya-Wen; Sakai, Takeshi; Guzmán, Andrés E.; Tatematsu, Ken’ichi; Nakamura, Fúmitaka; Chen, Huei-Ru Vivien

doi:10.3847/2041-8213/ac081c

Cited by 63 publications

(64 citation statements)

References 52 publications

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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%

“…The magnetic field model of Sanhueza et al (2021) assumes an hourglass poloidal field with an added toroidal component; but our magnetic spiral model is dominated by toroidal features. However, choosing the basic large- scale field model is a choice which will bias the estimate with its assumptions.…”

Section: Iras 18089-1732mentioning

confidence: 99%

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Magnetic Spirals in Accretion Flows Originated from Misaligned Magnetic Field

Wang,

Väisälä,

Shang

et al. 2022

Preprint

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Misalignment between rotation and magnetic field has been suggested to be one type of physical mechanisms which can easen the effects of magnetic braking during collapse of cloud cores leading to formation of protostellar disks. However, its essential factors are poorly understood. Therefore, we perform a more detailed analysis of the physics involved. We analyze existing simulation data to measure the system torques, mass accretion rates and Toomre Q parameters. We also examine the presence of shocks in the system. While advective torques are generally the strongest, we find that magnetic and gravitational torques can play substantial roles in how angular momentum is transferred during the disk formation process. Magnetic torques can shape the accretion flows, creating two-armed magnetized inflow spirals aligned with the magnetic field. We find evidence of an accretion shock that is aligned according to the spiral structure of the system. Inclusion of ambipolar diffusion as explored in this work has shown a slight influence in the small scale structures but not in the main morphology. We discuss potential candidate systems where some of these phenomena could be present.

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Section: Focused On Finding Potential Observable Features)mentioning

confidence: 89%

Section: Iras 18089-1732mentioning

confidence: 89%

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Magnetic Spirals in Accretion Flows Originated from Misaligned Magnetic Field

Wang,

Väisälä,

Shang

et al. 2022

Preprint

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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%

The ALMA Survey of 70 $μ$m Dark High-mass Clumps in Early Stages (ASHES). IV. Star formation signatures in G023.477

Morii,

Sanhueza,

Nakamura

et al. 2021

Preprint

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With a mass of ∼1000 M and a surface density of ∼0.5 g cm −2 , G023.477+0.114 also known as IRDC 18310-4 is an infrared dark cloud (IRDC) that has the potential to form high-mass stars and has been recognized as a promising prestellar clump candidate. To characterize the early stages of high-mass star formation, we have observed G023.477+0.114 as part of the ALMA Survey of 70 µm Dark Highmass Clumps in Early Stages (ASHES). We have conducted ∼1. 2 resolution observations with the Atacama Large Millimeter/submillimeter Array (ALMA) at 1.3 mm in dust continuum and molecular line emission. We identified 11 cores, whose masses range from 1.1 M to 19.0 M . Ignoring magnetic fields, the virial parameters of the cores are below unity, implying that the cores are gravitationally bound. However, when magnetic fields are included, the prestellar cores are close to virial equilibrium, while the protostellar cores remain sub-virialized. Star formation activity has already started in this clump. Four collimated outflows are detected in CO and SiO. H 2 CO and CH 3 OH emission coincide with the high-velocity components seen in the CO and SiO emission. The outflows are randomly oriented for the natal filament and the magnetic field. The position-velocity diagrams suggest that episodic mass ejection has already begun even in this very early phase of protostellar formation. The masses of the identified cores are comparable to the expected maximum stellar mass that this IRDC could form (8-19 M ). We explore two possibilities on how IRDC G023.477+0.114 could eventually form high-mass stars in the context of theoretical scenarios.

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“…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%

The Magnetic Field in the Milky Way Filamentary Bone G47

Stephens,

Myers,

Zucker

et al. 2022

Preprint

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Star formation primarily occurs in filaments where magnetic fields are expected to be dynamically important. The largest and densest filaments trace spiral structure within galaxies. Over a dozen of these dense (∼10 4 cm −3 ) and long (>10 pc) filaments have been found within the Milky Way, and they are often referred to as "bones." Until now, none of these bones have had their magnetic field resolved and mapped in their entirety. We introduce the SOFIA legacy project FIELDMAPS which has begun mapping ∼10 of these Milky Way bones using the HAWC+ instrument at 214 µm and 18. 2 resolution. Here we present a first result from this survey on the ∼60 pc long bone G47. Contrary to some studies of dense filaments in the Galactic plane, we find that the magnetic field is often not perpendicular to the spine (i.e., the center-line of the bone). Fields tend to be perpendicular in the densest areas of active star formation and more parallel or random in other areas. The average field is neither parallel or perpendicular to the Galactic plane nor the bone. The magnetic field strengths along the spine typically vary from ∼20 to ∼100 µG. Magnetic fields tend to be strong enough to suppress collapse along much of the bone, but for areas that are most active in star formation, the fields are notably less able to resist gravitational collapse. * Hubble Fellow are used to trace spiral structure within the Milky Way (e.g,. Reid et al. 2014). Observations from Spitzer revealed that some of these star-forming clouds are dense (∼10 4 cm −3 ), high-mass, and exceptionally elongated (e.g., over 80 pc × 0.5 pc for the Nessie filament; Jackson et al. 2010;Goodman et al. 2014). These filamentary structures are called bones because they delineate the

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

Cited by 63 publications

References 52 publications

Magnetic Spirals in Accretion Flows Originated from Misaligned Magnetic Field

Magnetic Spirals in Accretion Flows Originated from Misaligned Magnetic Field

The ALMA Survey of 70 $μ$m Dark High-mass Clumps in Early Stages (ASHES). IV. Star formation signatures in G023.477

The Magnetic Field in the Milky Way Filamentary Bone G47

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