Collision Between Molecular Clouds-III: The effects of cloud initial density profile on head-on collisions
arXiv:2105.04710 · doi:10.1093/mnras/stab1389
Abstract
In this third paper in our cloud-collision series, we present the results from simulations of head-on collisions with a strongly centrally-condensed initial density profile of . We investigate the impact of these density profiles on the overall evolution of the simulations: the structures formed, their dynamical evolution, and their star formation activity. We consider clouds which are globally bound and globally unbound, leading to three different scenarios -- the collision of a bound cloud with a bound cloud, the collision of two unbound clouds, or the collision of one cloud of each type. In all the simulations dense star clusters form before the collisions occur, and we find that star formation remains confined to these systems and is little affected by the collisions. If the clouds' are both initially bound, the collision forms a filamentary structure, but otherwise, this does not occur. We observe that rotating structures form around the clusters, but they also form in our non-colliding control simulations, so are not a consequence of the collisions. Dissipation of kinetic energy in these simulations is inefficient because of the substructure created in the clouds by turbulence before the collisions. As a result, although some gas is left bound in the COM frame, the star clusters formed in the simulations do not become bound to each other.
arXiv comment16 Pages, 21 Figures; Accepted by MNRAS
References in corpus (25)
- Cosmological SPH simulations: The entropy equation
- Star Formation in Disk Galaxies. I. Formation and Evolution of Giant Molecular Clouds via Gravitational Instability and Cloud Collisions
- Importance of the Initial Conditions for Star Formation - I. Cloud Evolution and Morphology
- 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
- Smoothed Particle Magnetohydrodynamics II. Variational principles and variable smoothing length terms
- Molecular Clouds Toward the Super Star Cluster NGC3603; Possible Evidence for a Cloud-Cloud Collision in Triggering the Cluster Formation
- Isolating signatures of major cloud-cloud collisions using position-velocity diagrams
- The frequency and nature of `cloud-cloud collisions' in galaxies
- Cloud-cloud collision as a trigger of the high-mass star formation; a molecular line study in RCW120
- 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
- Molecular clouds in the Trifid nebula M20; Possible evidence for a cloud-cloud collision in triggering the formation of the first generation stars
- Triggered O star formation in M20 via cloud-cloud collision: Comparisons between high-resolution CO observations and simulations
- Isolating signatures of major cloud-cloud collisions II: The lifetimes of broad bridge features
- SEREN - A new SPH code for star and planet formation simulations
- Star Formation triggered by cloud-cloud collisions
- The Gaia-ESO Survey: Kinematics of seven Galactic globular clusters
- Rotation in young massive star clusters
- The VLT-FLAMES Tarantula Survey VI: Evidence for rotation of the young massive cluster R136
- GANDALF - Graphical Astrophysics code for N-body Dynamics And Lagrangian Fluids
- Evolution of fractality and rotation in embedded star clusters
- Dynamically triggered star formation in giant molecular clouds
- The effect of photoionising feedback on star formation in isolated and colliding clouds
- Collision between Molecular Clouds I. The effect of the cloud virial ratio in head-on collisions