标题： MHD湍流模拟在宇宙结构背景中 显示英文标题

标题： MHD Turbulence Simulation in a Cosmic Structure Context

摘要： 星系团和宇宙丝状结构的气体介质构成了宇宙中大部分的重子物质，它是非常动态的。 它也可能具有湍流特性，尽管湍流特性尚不清楚。 气体非常稀薄，基本上是完全电离的等离子体。 观测证据表明，星系间介质（ICMs）在某种程度上是磁化的。 ICM种子磁场有几个可能的来源；观测到的磁场很可能是ICM中湍流的结果。 我们正在进行一项模拟研究，旨在理解在这种情况下非常微弱的初始磁场如何在驱动湍流中演化。 我们发现，磁场最终会演变为与湍流中的旋涡、无散度动能达到平衡水平。 随着这种演变，磁场结构的拓扑从纤维状形式转变为带状结构，在这种结构中，磁场方向与涡旋结构层叠在一起。 显示英文摘要

摘要： The gaseous media of galaxy clusters and cosmic filaments, which constitute most of the baryonic matter in the universe, is highly dynamic. It is also probably turbulent, although the turbulence properties are poorly known. The gas is highly rarefied, essentially fully ionized plasma. Observational evidence suggests intracluster media (ICMs) are magnetized at some level. There are several possible origins for ICM seed fields; the observed fields are likely the result of turbulence in the ICM. We are engaged in a simulation study designed to understand in this context how very weak initial magnetic fields evolve in driven turbulence. We find that the magnetic fields eventually evolve towards equipartition levels with the vortical, solenoidal kinetic energy in the turbulence. As they do so the topology of the field structures transition from filamentary forms into ribbon-like structures in which the field orientations are laminated with vorticity structures.