AM06-19-009 星間分子雲分裂の三次元磁気流体力学数値シミュレーション(宇宙流体(2),一般講演)

概要

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We study the self-gravitational instability of a magnetized gaseous layer by performing a 3-dimensional magneto-hydrodynamic (MHD) numerical simulation with ambipolar diffusion. When the strength of the magnetic field is weaker than the critical value, the gaseous layer is fragmented by the instability in a free-fall time of the cloud. On the other hand, when the magnetic field is stronger than the critical value, the gaseous layer is gravitationally stable because magnetic field prevents the contraction of the cloud. However, because the molecular cloud contains a lot of neutrals as well as some ions, ambipolar diffusion occurs in the cloud. Due to this effect, the gravitational instability develops gradually over the diffusion time. We confirm that the infall velocity is subsonic when the magnetic field is stronger than the critical value. We also find that the cores have a higher β than the surroundings for the strong field case, and vice versa.
日本流体力学会の論文
2006-09-05