团簇内介质中cosmic-ray电子的生命周期
Life cycle of cosmic-ray electrons in the intracluster medium
摘要：
模拟了中心射电星系注入小星系团介质中的相对论电子的演化过程，研究了初始喷流功率对射电等离子体扩散和辐射特性的影响。通过将被动示踪粒子耦合到自适应网格宇宙学MHD模拟中，我们研究了宇宙射线电子如何作为输入喷流功率的函数分散。我们还研究了后者如何影响的热和非热性质的集群内介质，与差异可辨别的$\sim$陀螺仪开始后的射流。我们发展了宇宙射线电子的能谱，受到同步加速器和逆康普顿发射以及通过冲击波和湍流再加速的能量增益为主的能量损失。我们发现，在没有重大合并的情况下，宇宙射线电子经历的再加速量不足以产生长寿命的可检测的无线电发射。然而，对于所有的模拟，再加速过程的作用是至关重要的，以保持一个显着的和体积填充水库的化石电子（$γ\sim 10^3$）的几个陀螺后，第一次注入射流。这对解释最近发现的星系团的辐射和其他射电现象很重要。
英文摘要：
We simulate the evolution of relativistic electrons injected into the medium of a small galaxy cluster by a central radio galaxy, studying how the initial jet power affects the dispersal and the emission properties of radio plasma. By coupling passive tracer particles to adaptive-mesh cosmological MHD simulations, we study how cosmic-ray electrons are dispersed as a function of the input jet power. We also investigate how the latter affects the thermal and non-thermal properties of the intracluster medium, with differences discernible up to $\sim$ Gyr after the start of the jet. We evolved the energy spectra of cosmic-ray electrons, subject to energy losses that are dominated by synchrotron and inverse Compton emission as well as energy gains via re-acceleration by shock waves and turbulence. We find that in the absence of major mergers the amount of re-acceleration experienced by cosmic-ray electrons is not enough to produce long-lived detectable radio emissions. However, for all simulations the role of re-acceleration processes is crucial to maintain a significant and volume-filling reservoir of fossil electrons ($γ\sim 10^3$) for several Gyrs after the first injection by jets. This is important to possibly explain recent discoveries of cluster-wide emission and other radio phenomena in galaxy clusters.
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