On the potential of faraday tomography to identify shock structures in supernova remnants
On the potential of faraday tomography to identify shock structures in supernova remnants
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法拉第断层扫描识别超新星遗迹中激波结构的潜力
DOI：
10.1093/mnras/stac1086
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发表时间：
2022
影响因子：
4.8
通讯作者：
Takahashi Keitaro
中科院分区：
文献类型：
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作者：
Ideguchi Shinsuke;Inoue Tsuyoshi;Akahori Takuya;Takahashi Keitaro
了解超新星遗迹（SNRs）中的磁场对于约束银河宇宙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。本文首次预测了信噪比的法拉第色散函数。在这项研究中，我们使用的三维（3D）的理想磁流体动力学（MHD）模拟的SNR扩展到一个弱，规则的磁场的结果。我们提出了本征FDFs的冲击区的信噪比为不同的视角。我们发现FDF通常是法拉第复数，这意味着传统的旋转测量研究不足以获得冲击区域磁场的信息，需要进行法拉第层析成像。我们还表明，FDF允许导出的物理深度分布的极化强度时，视线是平行于初始磁场方向。此外，我们证明，接触不连续的位置可以识别的径向轮廓的宽度的FDF的精度为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.