GMC Collisions as Triggers of Star Formation. VI. Collision-Induced Turbulence
arXiv:1711.01325 · doi:10.1093/pasj/psx140
Abstract
We investigate collisions between giant molecular clouds (GMCs) as potential generators of their internal turbulence. Using magnetohydrodynamic (MHD) simulations of self-gravitating, magnetized, turbulent, GMCs, we compare kinematic and dynamic properties of dense gas structures formed when such clouds collide compared to those that form in non-colliding clouds as self-gravity overwhelms decaying turbulence. We explore the nature of turbulence in these structures via distribution functions of density, velocity dispersions, virial parameters, and momentum injection. We find that the dense clumps formed from GMC collisions have higher effective Mach number, greater overall velocity dispersions, sustain near-virial equilibrium states for longer times, and are the conduit for injection of turbulent momentum into high density gas at high rates.
12 pages, 7 figures, Accepted for publication in PASJ
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- Investigating the Upper Scorpius OB association with HERMES. I. The spectroscopic sample and 6D kinematics
- Interactions of a shock with a molecular cloud at various stages of its evolution due to thermal instability and gravity
- Searching for further evidence for cloud-cloud collisions in L1188
- A possible far-ultraviolet flux-dependent core mass function in NGC 6357
- An X-ray View of Two Infrared Dark Clouds G034.43+00.24 and G035.39-00.33