在具有活动星系核喷流的星系团模拟中连接湍流速度和磁场
Connecting turbulent velocities and magnetic fields in galaxy cluster simulations with active galactic nuclei jets
摘要：
对星系团中热气体速度场的研究有助于揭示小尺度上的微观物理细节和活动星系核反馈的本质。同样地，法拉第旋转测量（RM）追踪的磁场也揭示了它们对气体动力学以及宇宙射线产生和传输的影响。通过对孤立的英仙座星系团中活动星系核喷流膨胀叶的产生、演化和破裂过程的非辐射磁流体动力学模拟，研究了大尺度气体运动学和磁场之间的内在联系。特别是，我们连接集群速度测量与模拟RM地图，以突出其潜在的物理连接，这开辟了在两个不同的观测湍流水平进行比较的可能性。对于单射流爆发，我们发现只有一个局部的速度场的影响，即相关的速度色散的增加是不是体积填充。此外，在具有预先存在的湍流的设置中，这种速度分散的增加在很大程度上被隐藏。我们使用模拟X射线观测表明，在弧分分辨率，速度色散，因此占主导地位的现有的大规模湍流，只有最低限度地改变了射流的存在。中心气体的速度结构上升的recently上升的叶，我们发现快速，相干流出低速色散。我们的研究结果强调，投影速度分布显示复杂的结构，这对观测的解释构成了挑战。
英文摘要：
The study of velocity fields of the hot gas in galaxy clusters can help to unravel details of microphysics on small-scales and to decipher the nature of feedback by active galactic nuclei (AGN). Likewise, magnetic fields as traced by Faraday rotation measurements (RMs) inform about their impact on gas dynamics as well as on cosmic ray production and transport. We investigate the inherent relationship between large-scale gas kinematics and magnetic fields through non-radiative magnetohydrodynamical simulations of the creation, evolution and disruption of AGN jet-inflated lobes in an isolated Perseus-like galaxy cluster, with and without pre-existing turbulence. In particular, we connect cluster velocity measurements with mock RM maps to highlight their underlying physical connection, which opens up the possibility of comparing turbulence levels in two different observables. For single jet outbursts, we find only a local impact on the velocity field, i.e. the associated increase in velocity dispersion is not volume-filling. Furthermore, in a setup with pre-existing turbulence, this increase in velocity dispersion is largely hidden. We use mock X-ray observations to show that at arcmin resolution, the velocity dispersion is therefore dominated by existing large-scale turbulence and is only minimally altered by the presence of a jet. For the velocity structure of central gas uplifted by buoyantly rising lobes, we find fast, coherent outflows with low velocity dispersion. Our results highlight that projected velocity distributions show complex structures which pose challenges for the interpretation of observations.
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