H II区象鼻和球状体的辐射磁流体动力学模型
Radiation-MHD models of elephant trunks and globules in H II regions
摘要：
我们研究的形成和致密气体，被称为象鼻，在H II区域的边界，电离辐射的阴影形成的致密团块的支柱的演变。磁场对这一过程的影响进行了研究，使用三维辐射磁流体力学模拟。对于一个模拟，其中一个初始均匀的磁场强度|B| =50 μ G的定向垂直于辐射传播方向，该领域被扫到与支柱在其动力学演化过程中对齐，在协议的“创造之柱”在M16，和一些彗星球状体的观测。当用18uG的较弱场重新运行模拟时，该效应显著增强。具有|B| =160 μ G的较强场足以完全防止这种演变，也显著影响光电离过程。使用更大的模拟域可以看出，Mackey & Lim（2010）研究的柱体形成模型最终在远离恒星的致密气体缺乏的情况下演化为彗星结构。
英文摘要：
We study the formation and evolution of pillars of dense gas, known as elephant trunks, at the boundaries of H II regions, formed by shadowing of ionising radiation by dense clumps. The effects of magnetic fields on this process are investigated using 3D radiation-magnetohydrodynamics simulations. For a simulation in which an initially uniform magnetic field of strength |B|=50 uG is oriented perpendicular to the radiation propagation direction, the field is swept into alignment with the pillar during its dynamical evolution, in agreement with observations of the "Pillars of Creation" in M16, and of some cometary globules. This effect is significantly enhanced when the simulation is re-run with a weaker field of 18 uG. A stronger field with |B|=160 uG is sufficient to prevent this evolution completely, also significantly affecting the photoionisation process. Using a larger simulation domain it is seen that the pillar formation models studied in Mackey & Lim (2010) ultimately evolve to cometary structures in the absence of dense gas further from the star.
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