The Formation of Massive Molecular Filaments and Massive Stars Triggered by a MHD Shock Wave
arXiv:1707.02035
Abstract
Recent observations suggest that intensive molecular cloud collision can trigger massive star/cluster formation. The most important physical process caused by the collision is a shock compression. In this paper, the influence of a shock wave on the evolution of a molecular cloud is studied numerically by using isothermal magnetohydrodynamics (MHD) simulations with the effect of self-gravity. Adaptive-mesh-refinement and sink particle techniques are used to follow long-time evolution of the shocked cloud. We find that the shock compression of turbulent inhomogeneous molecular cloud creates massive filaments, which lie perpendicularly to the background magnetic field as we have pointed out in a previous paper. The massive filament shows global collapse along the filament, which feeds a sink particle located at the collapse center. We observe high accretion rate dot{M}_acc > 10^{-4} M_sun/yr that is high enough to allow the formation of even O-type stars. The most massive sink particle achieves M>50 M_sun in a few times 10^5 yr after the onset of the filament collapse.
arXiv comment10 pages, 10 figures, submitted to the PASJ special issue (cloud collision)
References in corpus (5)
- GMC Collisions as Triggers of Star Formation. III. Density and Magnetically Regulated Star Formation
- Formation of the young compact cluster GM 24 triggered by a cloud-cloud collision
- High-mass star formation in Orion B triggered by cloud-cloud collision: Merging molecular clouds in NGC 2024
- Does feedback help or hinder star formation? The effect of photoionisation on star formation in Giant Molecular Clouds
- A new view of the giant molecular cloud M16 (Eagle Nebula) in 12CO J=1-0 and 2-1 transitions with NANTEN2