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To understand the formation of a magnetically dominated molecular cloud outof an atomic cloud, we follow the dynamical evolution of the cloud with atime-dependent axisymmetric magnetohydrodynamic code. A thermally stable warmatomic cloud is initially in static equilibrium with the surrounding hotionised gas. A shock propagating through the hot medium interacts with thecloud. As a fast-mode shock propagates through the cloud, the gas behind itbecomes thermally unstable. The $\beta$ value of the gas also becomes muchsmaller than the initial value of order unity. These conditions are ideal formagnetohydrodynamic waves to produce high-density clumps embedded in a rarefiedwarm medium. A slow-mode shock follows the fast-mode shock. Behind this shock adense shell forms, which subsequently fragments. This is a primary region forthe formation of massive stars. Our simulations show that only weak andmoderate-strength shocks can form cold clouds which have properties typical ofgiant molecular clouds.

Shock-triggered formation of magnetically-dominated clouds