论文标题
关于Faraday层析成像的潜力，可以鉴定超新星残留物中的冲击结构
On the Potential of Faraday Tomography to Identify Shock Structures in Supernova Remnants
论文作者
论文摘要
关于超新星残留物（SNR）中磁场的知识对于约束银河宇宙射线加速模型至关重要。它还可以间接提供有关星际磁场的信息。在本文中，我们首次预测SNR的Faraday分散函数（FDF）。在这项研究中，我们使用三维（3D）理想的磁性水力动力学（MHD）模拟的SNR的结果，该模拟扩展为弱的规则磁场。我们介绍了SNR的震惊区域的内在FDF，以了解不同的视角。我们发现FDF通常是Faraday复合物，这意味着常规旋转测量研究不足以获得有关冲击区域中磁场的信息，而Faraday层析成像是必要的。我们还表明，当视线与初始磁场方向平行时，FDF允许得出极化强度的物理深度分布。此外，我们证明，可以从FDF宽度的径向剖面识别触点不连续性的位置，其精度为0.1-0.2 PC。
Knowledge about the magnetic fields in supernova remnants (SNRs) is of paramount importance for constraining Galactic cosmic ray acceleration models. It could also indirectly provide information on the interstellar magnetic fields. In this paper, we predict the Faraday dispersion functions (FDFs) of SNRs for the first time. For this study, we use the results of three dimensional (3D) ideal magnetohydrodynamic (MHD) simulations of SNRs expanding into a weak, regular magnetic field. We present the intrinsic FDFs of the shocked region of SNRs for different viewing angles. We find that the FDFs are generally Faraday complex, which implies that conventional rotation measure study is not sufficient to obtain the information on the magnetic fields in the shocked region and Faraday tomography is necessary. We also show that the FDF allows to derive the physical-depth distribution of polarization intensity when the line of sight is parallel to the initial magnetic field orientation. Furthermore, we demonstrate that the location of contact discontinuity can be identified from the radial profile of the width of the FDF with the accuracy of 0.1-0.2 pc.
