Theoretical Study of the Internal Structures of the Relativistic Jets

(1)我们提出了一个模型，在喷流的不均匀性导致伴随初级耀斑的光回波，这可能解释孤儿TeV耀斑观察到几个TeV的开拓者。(2)相对论喷流的表观结构复杂地依赖于喷流的横向结构和时间变化方式，因为喷流的物质速度与光的传播速度相差很小。我们发现，所观察到的X射线，光学和无线电峰之间的空间偏移可以解释由能量相关的冷却时间的加速电子在传播的发射斑点。(3)分析了相对论像差和光束对偏振结构的影响。阐明了在同动坐标系中，观测到的偏振角垂直于天平面上的磁场方向。在此基础上研究了偏振角分布的统计特性。在共动坐标系中，磁场的方向主要是横向。我们还研究了扰动螺旋场几何的偏振特性。(4)研究了无碰撞激波的电子加速过程。我们发现，相反的一维情况下，没有冲浪加速度发生的二维情况。在二维情况下，考虑了离子束存在时的等离子体不稳定性，离子双流不稳定性是最不稳定的模式。(5)考虑两种相对运动的相对论流体，计算了它们之间的能量和动量交换率，并给出了插值公式。使用它们，我们进行了数值模拟的射流的形成。

(1) We proposed a model in which inhomogeneities in the jet cause light echoes accompanying primary flares, which may explain orphan TeV flares observed for several TeV blazers.(2) Apparent structures of relativistic jets depend complicatedly on the lateral and transverse structure and on the way of time variation because the difference between the matter velocities and light propagation velocity is very small. We showed that observed spatial offsets among X-ray, optical and radio peaks can be explained by energy dependent cooling time of accelerated electrons in a propagating emitting blob.(3) Effects of the relativistic aberration and beaming on the polarization structure are analyzed. We clarified that the observed polarization angle is perpendicular to the magnetic field direction on the sky plane in the comoving frame. Based on this we studied statistical properties of the polarization angle distribution. The magnetic field turns out to be predominantly directed in the transverse direction in the comoving frame. We also studied polarization properties of perturbed helical field geometry.(4) Electron acceleration process for collisionless shocks are investigated. We showed that contrary to the one-dimensional case, no surfing acceleration occurs for two-dimensional case. Plasma instabilities in the existence of ion beams are also considered for two-dimensional case and ion two-stream instability turns out to be the most unstable mode.(5) Two relativistic fluids in a relative motion are considered and energy and momentum exchange rates between them are calculated and interpolation formulas were proposed. Using them we performed numerical simulations of the formation of jets.