The Formation of Massive Molecular Filaments and Massive Stars Triggered by a MHD Shock Wave
The Formation of Massive Molecular Filaments and Massive Stars Triggered by a MHD Shock Wave
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MHD 冲击波引发的大质量分子丝和大质量恒星的形成
DOI：
10.1093/pasj/psx089
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发表时间：
2018
影响因子：
2.3
通讯作者：
Shu-ichiro
中科院分区：
文献类型：
--
作者：
Inoue;Tsuyoshi; Hennebelle;Patrick; Fukui;Yasuo; Matsumoto;Tomoaki; Iwasaki;Kazunari; Inutsuka;Shu-ichiro
最近的观测表明，强烈的分子云碰撞可以触发大质量星星/星团的形成。碰撞引起的最重要的物理过程是冲击压缩。本文采用等温磁流体动力学方法，在考虑自引力的情况下，数值研究了激波对分子云演化的影响。自适应网格加密和下沉粒子技术被用来跟踪冲击云的长期演变。我们发现，湍流不均匀分子云的激波压缩产生了大量的细丝，这些细丝垂直于背景磁场，正如我们在以前的论文中指出的那样。大质量的暗条表现出沿着暗条的整体坍缩，并向位于坍缩中心的汇粒子提供能量。我们观察到一个很高的吸积率yr-1，高到足以形成O型恒星。在暗条坍缩开始后的105年内，最大质量的汇粒子有几次超过M> 50 min。
Recent observations suggest an that intensive molecular cloud collision can trigger massive star/cluster formation. The most important physical process caused by the collision is a shock compression. In this paper, the influence of a shock wave on the evolution of a molecular cloud is studied numerically by using isothermal magnetohydrodynamics simulations with the effect of self-gravity. Adaptive mesh refinement and sink particle techniques are used to follow the long-time evolution of the shocked cloud. We find that the shock compression of a turbulent inhomogeneous molecular cloud creates massive filaments, which lie perpendicularly to the background magnetic field, as we have pointed out in a previous paper. The massive filament shows global collapse along the filament, which feeds a sink particle located at the collapse center. We observe a high accretion rateyr−1that is high enough to allow the formation of even O-type stars. The most massive sink particle achievesM> 50Min a few times 105yr after the onset of the filament collapse.