AI 中文总结
利用高分辨率宇宙磁流体动力学模拟，研究星系合并中的磁场及星系团中射电遗迹的起源，以探究合并在星系和星系团演化中的作用及相关物理机制。
AI 中文摘要
长期以来，合并一直被认为是星系和星系团演化的驱动力。它们释放出巨大的引力势能，在星系和星系团中分别约为\(10^{59}\)尔格和\(10^{64}\)尔格，这些能量在强大的冲击波中耗散。特别是在星系中，强烈的潮汐效应会对残余形态产生深远影响。尽管合并建模历史悠久，但直到最近才充分认识到它们对一系列因素的敏感性，包括星系际介质的存在、沿细丝的吸积以及预先存在的磁场。以宇宙学一致的方式对这些方面进行建模需要使用高分辨率的宇宙磁流体动力学（MHD）模拟。在这项工作中，我们使用此类模拟来研究两种不同的与合并相关的现象：i）星系合并中的磁场，ii）星系团中射电遗迹的起源。
英文摘要
Mergers have long been understood to be a driver of galaxy and galaxy cluster evolution. They release tremendous amounts of gravitational potential energy - ~$10^{59}$ and ~$10^{64}$ ergs in galaxies and clusters, respectively - which is dissipated in powerful shock waves. In galaxies especially, the strong tidal effects can have profound effects on the remnant morphology. Although the modelling of mergers has a long history, it is only recently that it has been fully appreciated just how sensitive they are to a range of factors, including the existence of circumgalactic media (CGM), accretion along filaments, and pre-existing magnetic fields. Modelling these aspects in a cosmologically-consistent manner necessitates the use of high-resolution cosmological magnetohydrodynamic (MHD) simulations. In this work, we use such simulations to investigate two distinct merger-related phenomena: i) magnetic fields in galaxy mergers, and ii) the origin of radio relics in galaxy clusters.
CommentsPhD Thesis, University of Potsdam (2025), xii + 228 pages. Ch. 3-5 reprint arXiv:2011.13947, arXiv:2301.13208, and arXiv:2411.11947, resp. Ch. 6 is expanded in arXiv:2604.06302. Ch. 7 describes major revisions to the CREST and AREPO shock finder implementations; cite this work for these developments
