2017/07/07 by Tsuyoshi Inoue, P. Hennebelle, Inoue, Tsuyoshi +9
Physics and Astronomy · #Astrophysics and Star Formation Studies #Astrophysics of Galaxies (astro-ph.GA) #Atomic and Molecular Physics #FOS: Physical sciences #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.1707.02035
openalex publication_date 2017/07/07 · openalex created_date 2017/08/31 · openalex updated_date 2026/07/28
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 dotMacc > 10-4 Msun/yr that is high enough to allow the formation of even O-type stars. The most massive sink particle achieves M>50 Msun in a few times 105 yr after the onset of the filament collapse.