The Early Stage of Molecular Cloud Formation by Compression of Two-phase Atomic Gases
We investigate the formation of molecular clouds from atomic gas by using three-dimensional magnetohydrodynamic simulations, including non-equilibrium chemical reactions and heating/cooling processes. We consider super-Alfvénic head-on colliding flows of atomic gas possessing the two-phase structure that consists of HI clouds and surrounding warm diffuse gas. We examine how the formation of molecular clouds depends on the angle $θ$ between the upstream flow and the mean magnetic field. We find that there is a critical angle $θ_\mathrm{cr}$ above which the shock-amplified magnetic field controls the post-shock gas dynamics. If the atomic gas is compressed almost along the mean magnetic field ($θ\llθ_\mathrm{cr}$), super-Alfvénic anisotropic turbulence is maintained by the accretion of the highly inhomogeneous upstream atomic gas. As a result, a greatly extended turbulence-dominated post-shock layer is generated. Around $θ\sim θ_\mathrm{cr}$, the shock-amplified magnetic field weakens the post-shock turbulence, leading to a dense post-shock layer. For $θ\gg θ_\mathrm{cr}$, the strong magnetic pressure suppresses the formation of cold dense clouds. Efficient molecular cloud formation is expected if $θ$ is less than a few times $θ_\mathrm{cr}$. Developing an analytic model and performing a parameter survey, we obtain an analytic formula for the critical angle as a function of the mean density, collision speed, and field strength of the upstream atomic gas. The critical angle is found to be less than $\sim 15^\circ$ as long as the field strength is larger than $1~μ$G, indicating that the probability of occurrence of compression with $θ<θ_\mathrm{cr}$ is limited if shock waves come from various directions.