将AGN气泡转化为具有晃动的射电遗迹：用真实物理模拟CR输运
Turning AGN bubbles into radio relics with sloshing: modeling CR transport with realistic physics
摘要：
射电遗迹是位于星系团外围的弧形同步辐射源，由$μ$ G磁场中的宇宙射线电子产生，被认为是由合并激波锋（重新）加速的。然而，并不是所有的遗迹都出现在与X射线中看到的冲击相同的位置。在以前的工作中，我们建议，一些遗迹的形状可能会导致从预先存在的宇宙射线电子的空间分布，并测试了这一假设，使用模拟发射AGN喷流到一个集群大气与晃动气体运动产生的先前的合并事件。我们发现，这些运动可以将活动星系核气泡中富含宇宙射线的物质输送到大半径，并在切向方向拉伸它，产生类似于射电遗迹的非对称形状。在这项工作中，我们通过将宇宙射线建模为经历扩散和阿尔文损失的单独流体来改进我们对宇宙射线的物理描述。我们发现，包括这个额外的宇宙射线物理显着减少了这些额外的功能的外观，表明我们原来的假设是敏感的宇宙射线物理在集群内介质的建模。
英文摘要：
Radio relics are arc-like synchrotron sources at the periphery of galaxy clusters, produced by cosmic-ray electrons in a $μ$G magnetic field which are believed to have been (re-)accelerated by merger shock fronts. However, not all relics appear at the same location as shocks as seen in the X-ray. In a previous work, we suggested that the shape of some relics may result from the pre-existing spatial distribution of cosmic-ray electrons, and tested this hypothesis using simulations by launching AGN jets into a cluster atmosphere with sloshing gas motions generated by a previous merger event. We showed that these motions could transport the cosmic ray-enriched material of the AGN bubbles to large radii and stretch it in a tangential direction, producing a filamentary shape resembling a radio relic. In this work, we improve our physical description for the cosmic rays by modeling them as a separate fluid which undergoes diffusion and Alfvén losses. We find that including this additional cosmic ray physics significantly diminishes the appearance of these filamentary features, showing that our original hypothesis is sensitive to the modeling of cosmic ray physics in the intracluster medium.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
