Cluster Shocks, Winds and Turbulence: The Dynamic Interplay Between Structure Formation, AGNs and Relativistic Plasmas

星系团是重要的宇宙学探测器，是揭示星系形成、演化和宇宙大尺度结构发展背后奥秘的关键人物。这些星系团充满了活动，因为暗物质主导的光晕的反复落入驱动了大规模的风、冲击、湍流和星系团内介质（ICM）中的熵不连续。弥漫性的热ICM包含约90%的正常星团物质，带有最近星团聚集历史的印记，通过其动力学/热力学状态提供了宇宙质量测量，传输金属和熵，转化星系恒星形成，并提供了一个实验室研究低密度介质中的基本流体和等离子体过程。由星系团范围过程和活动星系核（agn）产生的相对论性非热等离子体是理解ICM演化动力学状态的重要工具。利用这一工具需要一个丰富的观测基础，对热等离子体和非热等离子体之间相互作用的物理学有很好的理解，以及在物理和观测之间进行转换的有效方法。为此，研究人员设计了一个雄心勃勃的、协调理论和观测的项目，将利用数值模拟和望远镜系统的重大技术进步。该项目的目标包括大大提高对以下方面的理解：(1)大规模流动和湍流如何在ICM中建立并从千秒差距演变到兆秒差距；(2)磁场如何发展，然后揭示并反馈到ICM的演变；(3)相对论性宇宙射线（CRs）如何既是动态ICM的产物又是ICM的诊断；(4)AGN流出物如何与ICM物理相互作用并作为局部流动的诊断。在教育方面，该项目包括培养本科生和研究生在前沿科学和创新的数据分析和数值模拟技术的发展。调查人员还将积极参与公共教育，包括与当地天文馆、K-12科学和社区团体合作。

Clusters of galaxies are important probes of cosmology and are key players in unraveling the mysteries behind galaxy formation and evolution and the development of large scale structure in the Universe. These galaxy clusters are teeming with activity as the recurring infall of dark matter dominated halos drives large scale winds, shocks, turbulence and entropy discontinuities in the intracluster medium (ICM). The diffuse, hot ICM, comprising about 90% of the normal cluster matter, carries the imprint of the recent cluster assembly history, provides a cosmological mass metric through its dynamical/thermodynamical state, transports metals and entropy, transforms galactic star formation, and offers a laboratory into basic fluid and plasma processes in low density media. Relativistic, nonthermal plasmas produced by cluster-wide processes and active galactic nuclei (AGNs) serve as an important tool for understanding the ICM's evolving dynamical state. Exploiting this tool requires a rich observational base, a good understanding of the physics of the interactions between thermal and nonthermal plasmas, and effective ways to translate between that physics and observations. To that end, the investigators have designed an ambitious, coordinated theoretical and observational program that will leverage major technical advances in both numerical simulations and telescope systems.The aims of this project include a much improved understanding of (1) how large scale flows and turbulence are established in the ICM and evolve from kiloparsec to megaparsec scales, (2) how magnetic fields develop and then reveal and feed back to ICM evolution, (3) how relativistic cosmic rays (CRs) are both products of and diagnostics for the dynamic ICM, and (4) how AGN outflows physically interact with the ICM and serve as diagnostics of local flows.Educationally, this project includes training of undergraduate and graduate students in both cutting-edge science and the development of innovative data analysis and numerical simulation techniques. The investigators will also be active in public education, including work with the local planetarium, K-12 science and community groups.