庞大而精致。II。高空间分辨率大质量星系团湍流运动的统计特性
Massive and Refined. II. The statistical properties of turbulent motions in massive galaxy clusters with high spatial resolution
摘要：
我们使用自适应网格细化程序ENZO（例如Norman et al.2007），研究了一组20个大动态范围模拟的星系团在团内介质中的混沌运动特性。所采用的设置使我们能够研究的光谱和空间特性的湍流运动在星系团与前所未有的细节，实现了最大的雷诺数的顺序R=500-1000的最大涡。研究了团内介质中这些运动的能量与宿主系统动力学状态之间的相关性，以及湍流运动的统计特性及其随时间的演化，支持了主要的并合事件是团内大部分湍流动能注入的原因。湍流被发现占20- 30%的热能在合并集群，而它占5%的松弛集群。提供了我们模拟的星系团中湍流和运动的能量与最近用XMM-牛顿（Sanders et al.2010）推导的真实附近星系团中的上限的比较。当对相同空间尺度的湍流运动进行比较时，模拟结果的数据在目前观测所允许的范围内。最后，我们评论的可能性，湍流可能会加速相对论粒子导致形成的巨型射电晕的湍流（合并）集群。基于我们的模拟，我们确认以前的半分析研究表明，湍流集群的分数是一致的集群托管无线电晕。
英文摘要：
We study the properties of chaotic motions in the intra cluster medium using a set of 20 galaxy clusters simulated with large dynamical range, using the Adaptive Mesh Refinement code ENZO (e.g. Norman et al.2007). The adopted setup allows us to study the spectral and spatial properties of turbulent motions in galaxy clusters with unprecedented detail, achieving an maximum available Reynolds number of the order of R=500-1000 for the largest eddies. The correlations between the energy of these motions in the Intra Cluster Medium and the dynamical state of the host systems are studied, and the statistical properties of turbulent motions and their evolution with time support that major merger events are responsible for the injection of the bulk of turbulent kinetic energy inside cluster. Turbulence is found to account for a 20-30 per cent of the thermal energy in merging clusters, while it accounts for a 5 per cent in relaxed clusters. A comparison of the energies of turbulence and motions in our simulated clusters with present upper-limits in real nearby clusters, recently derived with XMM-Newton (Sanders et al.2010), is provided. When the same spatial scales of turbulent motions are compared, the data from simulations result well within the range presently allowed by observations. Finally, we comment on the possibility that turbulence may accelerate relativistic particles leading to the formation of giant radio halos in turbulent (merging) clusters. Based on our simulations we confirm previous semi-analytical studies that suggest that the fraction of turbulent clusters is consistent with that of clusters hosting radio halos.
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