恒星形成区的尘埃磁流体动力学
Dusty Magnetohydrodynamics in Star Forming Regions
摘要：
恒星的形成发生在暗分子区域，那里的氢核数密度nH超过10^4 cc，电离分数小于等于10^-7，尘埃颗粒的质量不到1%，其大小可达十分之一微米，甚至可能小至几十纳米。颗粒上的结晶对于去除气相离子是重要的，气相离子是由穿透暗区的宇宙射线产生的。中性粒子与带电粒子的碰撞对磁场与中性气体的耦合有重要贡献。因此，在研究恒星形成过程中的大尺度坍缩、波的演化和激波结构的磁流体动力学模型中，必须考虑颗粒的动力学行为。
英文摘要：
Star formation occurs in dark molecular regions where the number density of hydrogen nuclei, nH, exceeds 10^4 cc and the fractional ionization is 10^-7 or less. Dust grains with sizes ranging up to tenths of microns and perhaps down to tens of nanometers contain just under one percent of the mass. Recombination on grains is important for the removal of gas phase ions, which are produced by cosmic rays penetrating the dark regions. Collisions of neutrals with charged grains contribute significantly to the coupling of the magnetic field to the neutral gas. Consequently, the dynamics of the grains must be included in the magnetohydrodynamic models of large scale collapse, the evolution of waves and the structures of shocks important in star formation.
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