Three Dimensional Structure of Relativistic Jet Formation
Three Dimensional Structure of Relativistic Jet Formation
复制标题
相对论性射流形成的三维结构
DOI：
10.1093/mnras/sts519
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发表时间：
2012
影响因子：
4.8
通讯作者：
O. Porth
中科院分区：
文献类型：
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作者：
O. Porth
利用高分辨率自适应网格加密模拟，我们研究了旋转磁层中相对论喷流的形成。在这里，我们专注于非轴对称模式的发展，由于内部和外部扰动的射流。这些扰动要么来自于随流动注入的扰动，要么来自于团状外部介质。在螺旋场几何形状的加速射流，m=1至m=5模式进行了分析，并发现饱和的高度\sim 20内盘半径。我们还讨论了一种方法来控制人工放大的m = 4噪声的carnival模拟几何。强扰动由于不均匀的环境介质导致流动配置与增加的磁间距，从而表明一个自稳定的射流形成机制。
Using high resolution adaptive mesh refinement simulations in 3D, we investigate the formation of relativistic jets from rotating magnetospheres. Here, we focus on the development of non-axisymmetric modes due to internal and external perturbations to the jet. These originate either from injection of perturbations with the flow or from a clumpy external medium. In the helical field geometry of the accelerating jet, the m=1 to m=5 modes are analyzed and found to saturate at a height of \sim 20 inner disk radii. We also discuss a means to control artificial amplification of m = 4 noise in the cartesian simulation geometry. Strong perturbations due to an in-homogeneous ambient medium lead to flow configurations with increased magnetic pitch and thus indicate a self-stabilization of the jet formation mechanism.