GMC Collisions as Triggers of Star Formation. III. Density and Magnetically Regulated Star Formation

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

doi:10.3847/1538-4357/aa6ffa

Cited by 65 publications

(63 citation statements)

References 64 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Both the studies came to the conclusion that for smaller clouds slower collisions provided a greater efficiency in forming massive stars. Wu et al (2017b) also studied the collision between molecular clouds with the added support from magnetic fields and found that the star formation rates and efficiencies are higher by a factor of ten in collision simulations.…”

Section: Introductionmentioning

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

View full text Add to dashboard Cite

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.

show abstract

Section: Introductionmentioning

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

View full text Add to dashboard Cite

show abstract

“…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%

“…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). Inoue and Fukui (2013) studied the interface layer of the colliding clouds by three-dimensional MHD simulations, and showed formation of massive molecular cores, which likely lead to form high-mass protostars gaining high mass accretion rate helped by amplified turbulence and magnetic fields via supersonic collision ( see also Inoue et al 2017).…”

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

View full text Add to dashboard Cite

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.

show abstract

“…Proper motion measurements from the final GAIA survey will be also useful to study kinematic substructures in Orion. The degree of kinematic substructure that we measure will also be compared to the results from theoretical/numerical models of star cluster formation under different scenarios (Wu et al 2017a(Wu et al , 2017b.…”

Section: Ppv Connected Structuresmentioning

confidence: 99%

IN-SYNC. V. Stellar Kinematics and Dynamics in the Orion A Molecular Cloud

Rio

Tan

Covey

et al. 2017

ApJ

Self Cite

View full text Add to dashboard Cite

The kinematics and dynamics of young stellar populations enable us to test theories of star formation. With this aim, we continue our analysis of the SDSS-III/APOGEE IN-SYNC survey, a high-resolution near-infrared spectroscopic survey of young clusters. We focus on the Orion A star-forming region, for which IN-SYNC obtained spectra of ∼2700 stars. In Paper IV we used these data to study the young stellar population. Here we study the kinematic properties through radial velocities (v r ). The young stellar population remains kinematically associated with the molecular gas, following a~-10 km s 1 gradient along the filament. However, near the center of the region, the v r distribution is slightly blueshifted and asymmetric; we suggest that this population, which is older, is slightly in the foreground. We find evidence for kinematic subclustering, detecting statistically significant groupings of colocated stars with coherent motions. These are mostly in the lower-density regions of the cloud, while the ONC radial velocities are smoothly distributed, consistent with it being an older, more dynamically evolved cluster. The velocity dispersion s v varies along the filament. The ONC appears virialized, or just slightly supervirial, consistent with an old dynamical age. Here there is also some evidence for ongoing expansion, from a v r -extinction correlation. In the southern filament, s v is ∼2-3 times larger than virial in the L1641N region, where we infer a superposition along the line of sight of stellar subpopulations, detached from the gas. In contrast, s v decreases toward L1641S, where the population is again in agreement with a virial state.

show abstract

GMC Collisions as Triggers of Star Formation. III. Density and Magnetically Regulated Star Formation

Cited by 65 publications

References 64 publications

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

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

IN-SYNC. V. Stellar Kinematics and Dynamics in the Orion A Molecular Cloud

Contact Info

Product

Resources

About