三维磁流体动力学模拟中头尾射电星系的非热辐射
Non-thermal emissions from a head-tail radio galaxy in 3D magnetohydrodynamic simulations
AI总结：
本文通过三维磁流体动力学模拟研究头尾射电星系的非热辐射，发现宇宙线再加速对解释其射电性质至关重要，并探讨了同步加速器细丝的形成与长期稳定性。
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，以及这个“头尾星系”从射电到伽马射线和中微子的辐射。我们的模拟追踪了宇宙线粒子谱随能量损失和随机湍流加速的演化。我们发现再加速对于解释头尾星系观测到的射电性质至关重要，在这些星系中射电通量和谱指数没有剧烈变化。我们的模型表明，英仙座星系团中头尾星系周围的硬X射线辐射可以被硬X射线卫星（如FORCE）探测到，这将有可能约束加速效率。我们还探索了准直同步加速器细丝的起源，这些细丝是最近高质量的射电观测在一些头尾星系中发现的。连接两条尾巴的细长通量管是在早期由强回流形成的。我们发现这些细丝随风平流运动超过3亿年而未被破坏。来自通量管的射电通量远低于典型观测到的通量。然而，沿通量管的高效宇宙线扩散过程可能解决这一差异。
英文摘要：
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.
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。
