Gas and star kinematics in cloud-cloud collisions
arXiv:2304.01255 · doi:10.1093/mnras/stad1022
Abstract
We model the collision of molecular clouds to investigate the role of the initial properties on the remnants. Our clouds collide and evolve in a background medium that is approximately ten times less dense than the clouds, and we show that this relatively dense background is dynamically important for the evolution of the collision remnants. Given the motion of the clouds and the remnants through the background, we develop, implement, and introduce dynamic boundary conditions. We investigate the effect of the initial cloud mass, velocity, internal turbulence, and impact angle. The initial velocity and its velocity components have the largest affect on the remnant. This affects the spatial extent of the remnant, which affects the number of resulting star clusters and the distribution of their masses. The less extended remnants tend to have fewer, but more massive, clusters. Unlike the clusters, the gas distributions are relatively insensitive to the initial conditions, both the distribution of the bulk gas properties and the gas clumps. In general, cloud collisions are relatively insensitive to their initial conditions when modelled hydrodynamically in a dynamically important background medium.
arXiv comment22 pages, 23 figures. Accepted for publication in MNRAS
References in corpus (66)
- Toward Understanding Massive Star Formation
- The Formation of Massive Stars from Turbulent Cores
- Modelling Accretion in Protobinary Systems
- Density, Velocity, and Magnetic Field Structure in Turbulent Molecular Cloud Models
- The Formation of a Star Cluster: Predicting the Properties of Stars and Brown Dwarfs
- The Star Formation Rate of Turbulent Magnetized Clouds: Comparing Theory, Simulations, and Observations
- SPLASH: An interactive visualisation tool for Smoothed Particle Hydrodynamics simulations
- Competitive accretion in embedded stellar cluster
- Stellar, brown dwarf and multiple star properties from a radiation hydrodynamical simulation of star cluster formation
- Filamentary structure of star-forming complexes
- The Universality of Turbulence in Galactic Molecular Clouds
- Phantom: A smoothed particle hydrodynamics and magnetohydrodynamics code for astrophysics
- On the Star Formation Efficiency of Turbulent Magnetized Clouds
- Molecular Cloud Evolution II. From cloud formation to the early stages of star formation in decaying conditions
- Global collapse of molecular clouds as a formation mechanism for the most massive stars
- An Origin of Supersonic Motions in Interstellar Clouds
- On the diversity and statistical properties of protostellar discs
- Simulating the formation of molecular clouds. I. Slow formation by gravitational collapse from static initial conditions
- Star Formation in Disk Galaxies. I. Formation and Evolution of Giant Molecular Clouds via Gravitational Instability and Cloud Collisions
- The PdBI Arcsecond Whirlpool Survey (PAWS): Environmental Dependence of Giant Molecular Cloud Properties in M51
- Formation of Massive Molecular Cloud Cores by Cloud-cloud Collision
- The Origin of Massive Stars: The Inertial-Inflow Model
- Do cloud-cloud collisions trigger high-mass star formation? I. Small cloud collisions
- Molecular clouds towards RCW 49 and Westerlund 2; Evidence for cluster formation triggered by cloud-cloud collision
- Unifying low and high mass star formation through density amplified hubs of filaments
- Molecular Clouds Toward the Super Star Cluster NGC3603; Possible Evidence for a Cloud-Cloud Collision in Triggering the Cluster Formation
- Molecular Cloud Evolution IV: Magnetic Fields, Ambipolar Diffusion, and the Star Formation Efficiency
- On the convergence of the critical cooling timescale for the fragmentation of self-gravitating discs
- Isolating signatures of major cloud-cloud collisions using position-velocity diagrams
- Conditions for Circumstellar Disk Formation: Effects of Initial Conditions and Sink Treatment
- Cloud-cloud collisions and triggered star formation
- The frequency and nature of `cloud-cloud collisions' in galaxies
- The two molecular clouds in RCW 38; evidence for formation of the youngest super star cluster in the Milky Way triggered by cloud-cloud collision
- Temperature and Density Distribution in the Molecular Gas Toward Westerlund 2: Further Evidence for Physical Association
- Star Formation in Disk Galaxies. II. The Effect of Star Formation and Photoelectric Heating on the Formation and Evolution of Giant Molecular Clouds
- A new look at the molecular gas in M42 and M43; possible evidence for cloud-cloud collision which triggered formation of the OB stars in the Orion Nebula Cluster
- Isolating signatures of major cloud-cloud collisions II: The lifetimes of broad bridge features
- The Physical Properties of Large-Scale Galactic Filaments
- Formation of the Young Massive Cluster R136 triggered by Tidally-driven Colliding HI Flows
- Tracing the formation of molecular clouds via [CII], [CI] and CO emission
- Forming spectroscopic massive proto-binaries by disk fragmentation
- Star Formation triggered by cloud-cloud collisions
- There is no magnetic braking catastrophe: Low-mass star cluster and protostellar disc formation with non-ideal magnetohydrodynamics
- What can simulated molecular clouds tell us about real molecular clouds?
- An ALMA study of hub-filament systems I. On the clump mass concentration within the most massive cores
- Formation of the young compact cluster GM 24 triggered by a cloud-cloud collision
- ALMA view of G0.253+0.016: Can cloud-cloud collision form the cloud?
- The formation of massive stellar clusters in converging galactic flows with photoionisation
- Cloud formation in colliding flows: influence of the choice of cooling function
- The role of collision speed, cloud density, and turbulence in the formation of young massive clusters via cloud-cloud collisions
- A comparison between grid and particle methods on the small-scale dynamo in magnetised supersonic turbulence
- ALMA CO Observations of a Giant Molecular Cloud in M33: Evidence for High-Mass Star Formation Triggered by Cloud-Cloud Collisions
- Massive core/star formation triggered by cloud-cloud collision: Effect of magnetic field
- Molecular cloud formation in high-shear, magnetized colliding flows
- The Effects of Inhomogeneities within Colliding Flows on the Formation and Evolution of Molecular Clouds
- Origin of multiple nuclei in ultraluminous infrared galaxies
- Molecular line signatures of cloud-cloud collisions
- Cloud-cloud collision as origin of the G31.41+0.31 massive protocluster
- The properties of clusters, and the orientation of magnetic fields relative to filaments, in magnetohydrodynamic simulations of colliding clouds
- High-mass star formation in Orion possibly triggered by cloud-cloud collision III, NGC2068 and NGC2071
- Collision between Molecular Clouds I. The effect of the cloud virial ratio in head-on collisions
- MHD simulations of dense core collision
- A kinematic analysis of the CO clouds toward a reflection nebula NGC 2023 observed with the Nobeyama 45 m telescope; Further evidence for a cloud-cloud collision in the Orion region
- Star formation in Galactic flows
- Property of Young Massive Clusters in a Galaxy-Galaxy Merger Remnant
- Collision Between Molecular Clouds-III: The effects of cloud initial density profile on head-on collisions