标题： 非热辐射来自三维磁流体动力学模拟中的头尾射电星系 显示英文标题

标题： Non-thermal emissions from a head-tail radio galaxy in 3D magnetohydrodynamic simulations

摘要： 我们展示了星系团中喷流-风相互作用的磁流体动力学模拟，以及由此产生的“头部-尾部星系”从射电到伽马射线和中微子的辐射。 我们的模拟跟踪了宇宙射线（CR）粒子能谱的能量损失和随机湍流加速过程。 我们发现，再加速对于解释头部-尾部星系的观测射电特性是至关重要的，在这些星系中，射电流量和光谱指数不会剧烈变化。 我们的模型表明，通过硬X射线卫星（如FORCE）可以在Perseus星系团中的头部-尾部星系周围探测到硬X射线辐射，这可能会限制加速效率。 我们还探讨了成束的同步辐射丝状结构的起源，这些结构最近通过高质量的射电观测在一些头部-尾部星系中被发现。 在早期阶段，由强回流形成的细长通量管连接两个尾部。 我们发现这些丝状物在3亿多年内随着风移动而没有被破坏。 通量管的射电流量远低于典型的观测流量。 然而，沿通量管的高效宇宙射线扩散过程可能解决这一差异。 显示英文摘要

摘要： We present magnetohydrodynamic simulations of a jet-wind interaction in a galaxy cluster and the radio to gamma-ray and the neutrino emissions from this "head-tail galaxy". Our simulation follows the evolution of cosmic-ray (CR) particle spectra with energy losses and the stochastic turbulence acceleration. We find that the reacceleration is essential to explain the observed radio properties of head-tail galaxies, in which the radio flux and spectral index do not drastically change. Our models suggest that hard X-ray emissions can be detected around the head-tail galaxy in the Perseus cluster by the hard X-ray satellites, such as FORCE, and it will potentially constrain the acceleration efficiency. We also explore the origin of the collimated synchrotron threads, which are found in some head-tail galaxies by recent high-quality radio observations. Thin and elongated flux tubes, connecting the two tails, are formed by strong backflows at an early phase. We find that these threads advect with the wind for over 300 Myr without disrupting. The radio flux from the flux tubes is much lower than the typical observed flux. An efficient CR diffusion process along the flux tubes, however, may solve this discrepancy.