Westerlund 2星团分子云形成的磁流体动力学模拟：喷流与星团星际介质的相互作用
Magnetohydrodynamic Simulations of the Formation of Molecular Clouds toward the Stellar Cluster Westerlund 2: Interaction of a Jet with Clumpy Interstellar Medium
摘要：
利用三维磁流体动力学（MHD）数值模拟方法研究了NANTEN 2和Mopra望远镜观测到的Westerlund 2星团附近CO云的形成机制。这些分子云显示出一种特殊的形状，由TeV射线源HESS J1023-575一侧的弧形云和另一侧的云（喷流云）的线性分布组成。我们认为，这些云是由喷流与星际中性氢（HI）团块的相互作用形成的。通过研究由激波压缩和冷却形成的稠密冷云的形状与HI团簇填充因子的关系，发现HI团簇的密度分布决定了喷流-云相互作用形成的分子云的形状，当填充因子较大时，形成弧形云。另一方面，当填充因子较小时，分子云与射流对齐。在填充因子较小的模型中，射流传播较快。
英文摘要：
The formation mechanism of CO clouds observed with NANTEN2 and Mopra telescope toward the stellar cluster Westerlund 2 is studied by three-dimensional magnetohydrodynamic (MHD) simulations taking into account the interstellar cooling. These molecular clouds show a peculiar shape composing of an arc-shaped cloud in one side of a TeV-ray source HESS J1023-575 and a linear distribution of clouds (jet clouds) in another side. We propose that these clouds are formed by the interaction of a jet with interstellar neutral hydrogen (HI) clumps. By studying the dependence of the shape of dense cold clouds formed by shock compression and cooling on the filling factor of HI clumps, we found that the density distribution of HI clumps determines the shape of molecular clouds formed by the jet-cloud interaction; arc-clouds are formed when the filling factor is large. On the other hand, when the filling factor is small, molecular clouds align with the jet. The jet propagates faster in models with small filling factors.
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