GMC Collisions as Triggers of Star Formation. II. 3D Turbulent, Magnetized Simulations

Wu, Benjamin; Tan, Jonathan C.; Nakamura, Fúmitaka; Loo, S. Van; Christie, Duncan; Collins, David C.

doi:10.3847/1538-4357/835/2/137

Cited by 68 publications

(67 citation statements)

References 76 publications

(115 reference statements)

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“…Applying relative orientation analysis to synthetic polarization observations of numerical simulations, indicates that the slope and intercept of the relative orientation parameter, may encode information about the geometry of the flows that created the cloud (Soler and Hennebelle, 2017;Wu et al, 2017), or the magnetic field strength (Soler et al, 2013;Chen et al, 2016;Wu et al, 2017).…”

Section: Correlations Between Cloud Structure and Magnetic Field Oriementioning

confidence: 99%

Submillimeter and Far-Infrared Polarimetric Observations of Magnetic Fields in Star-Forming Regions

Pattle

Fissel

2019

Front. Astron. Space Sci.

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Observations of star-forming regions by the current and upcoming generation of submillimeter polarimeters will shed new light on the evolution of magnetic fields over the cloud-to-core size scales involved in the early stages of the star formation process. Recent wide-area and high-sensitivity polarization observations have drawn attention to the challenges of modeling magnetic field structure of star forming regions, due to variations in dust polarization properties in the interstellar medium. However, these observations also for the first time provide sufficient information to begin to break the degeneracy between polarization efficiency variations and depolarization due to magnetic field sub-beam structure, and thus to accurately infer magnetic field properties in the star-forming interstellar medium. In this article we discuss submillimeter and far-infrared polarization observations of star-forming regions made with single-dish instruments. We summarize past, present and forthcoming single-dish instrumentation, and discuss techniques which have been developed or proposed to interpret polarization observations, both in order to infer the morphology and strength of the magnetic field, and in order to determine the environments in which dust polarization observations reliably trace the magnetic field. We review recent polarimetric observations of molecular clouds, filaments, and starless and protostellar cores, and discuss how the application of the full range of modern analysis techniques to recent observations will advance our understanding of the role played by the magnetic field in the early stages of star formation.

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Section: Correlations Between Cloud Structure and Magnetic Field Oriementioning

confidence: 99%

Submillimeter and Far-Infrared Polarimetric Observations of Magnetic Fields in Star-Forming Regions

Pattle

Fissel

2019

Front. Astron. Space Sci.

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“…Magnetic fields, which are neglected in these simulations, are likely to influence cloud-cloud collisions in several ways, and other authors have begun to investigate this complex issue. In particular Wu et al (2017a) use ideal-MHD AMR simulations to investigate the influence of the orientation of an initially-smooth magnetic field relative to the collision axis. They find, not surprisingly, that the further the field is from being parallel to the collision axis, the less high-density gas is generated early in the collision.…”

Section: Discussionmentioning

confidence: 99%

Collision between molecular clouds – I. The effect of the cloud virial ratio in head-on collisions

Tanvir

Dale

2020

Monthly Notices of the Royal Astronomical Society

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In a series of papers we investigate the effect of collisions between turbulent molecular clouds on their structure, evolution and star formation activity. In this paper we look into the role of the clouds' initial virial ratios. Three different scenarios were examined: both clouds initially bound, one cloud bound and one unbound, and both clouds initially unbound. Models in which one or both clouds are bound generate filamentary structures aligned along the collision axis and discernible in position-position and position-velocity space. If neither cloud is bound, no filaments result. Unlike in previous simulations of collisions between smooth clouds, owing to the substructure created in the clouds by turbulence before the collisions, dissipation of kinetic energy by the collision is very inefficient and in none of our simulations is sufficient bulk kinetic energy lost to render the clouds bound. Simulations where both clouds are bound created twice as much stellar mass than the bound-unbound model, and both these scenarios produced much more stellar mass than the simulation in which both clouds are unbound. Each simulation was also compared with a control run in which the clouds do not collide. We find the bound-bound collision increases the overall star formation efficiency by a factor of approximately two relative to the control, but that the bound-unbound collision produces a much smaller increase, and the collision has very little effect on the unbound-unbound cloud collision.

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“…Balfour et al (2015Balfour et al ( , 2017) also presented numerical simulation of head-on and non-head-on a cloud-cloud collision. In addition, the magneto-hydrodynamical simulations (MHD) simulation of giant molecular cloud (GMC) collision was carried out by several authors (e.g., Wu et al 2015Wu et al , 2017aWu et al , 2017bChristie et al 2017;Bisbas et al 2017;. They showed GMC collision enhanced star formation rate and efficiency (Wu et al 2017b).…”

Section: Cloud-cloud Collisions As a Trigger Of High-mass Star Formationmentioning

confidence: 99%

FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45 m telescope (FUGIN): Molecular clouds toward W 33; possible evidence for a cloud–cloud collision triggering O star formation

Kohno

Torii

Tachihara

et al. 2018

Publications of the Astronomical Society of Japan

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We observed molecular clouds in the W33 high-mass star-forming region associated with compact and extended H II regions using the NANTEN2 telescope as well as the Nobeyama 45-m telescope in the J =1-0 transitions of 12 CO, 13 CO, and C 18 O as a part of the FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45-m telescope (FUGIN) legacy survey. We detected three velocity components at 35 km s −1 , 45 km s −1 , and 58 km s −1 . The 35 km s −1 and 58 km s −1 clouds are likely to be physically associated with W33 because of the enhanced 12 CO J = 3-2 to J =1-0 intensity ratio as R 3−2/1−0 > 1.0 due to the ultraviolet irradiation by OB stars, and morphological correspondence between the distributions of molecular gas and the infrared and radio continuum emissions excited by high-mass stars. The two clouds show complementary distributions around W33. The velocity separation is too large to be gravitationally bound, and yet not explained by expanding motion by stellar feedback. c 2014. Astronomical Society of Japan. 2Publications of the Astronomical Society of Japan, (2014), Vol. 00, No. 0 Therefore, we discuss that a cloud-cloud collision scenario likely explains the high-mass star formation in W33.

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GMC Collisions as Triggers of Star Formation. II. 3D Turbulent, Magnetized Simulations

Cited by 68 publications

References 76 publications

Submillimeter and Far-Infrared Polarimetric Observations of Magnetic Fields in Star-Forming Regions

Submillimeter and Far-Infrared Polarimetric Observations of Magnetic Fields in Star-Forming Regions

Collision between molecular clouds – I. The effect of the cloud virial ratio in head-on collisions

FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45 m telescope (FUGIN): Molecular clouds toward W 33; possible evidence for a cloud–cloud collision triggering O star formation

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