Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections
Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections
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DOI：
10.1007/s11214-020-00757-9
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发表时间：
2020-10
影响因子：
10.3
通讯作者：
S. Patsourakos;A. Vourlidas;T. Török;B. Kliem;S. Antiochos;V. Archontis;G. Aulanier;Xin Cheng
中科院分区：
文献类型：
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作者：
S. Patsourakos;A. Vourlidas;T. Török;B. Kliem;S. Antiochos;V. Archontis;G. Aulanier;Xin Cheng
对日冕物质抛射（CME）爆发前磁场结构的本质有一个清楚的认识是理解和最终预测太阳爆发所必需的。只有两种看似不同的磁结构被认为是可行的，即剪切磁弧（SMA）和磁通绳（MFR）。它们可以通过三种物理机制形成（通量出现，通量抵消，螺旋度凝结）。然而，对于CME的罪魁祸首究竟是SMA还是MFR，人们已经争论了30年。我们成立了一个国际空间科学研究所（ISSI）团队来处理和解决这个问题，并在这里报告结果。我们回顾了建模和观测领域的现状，确定了开放和封闭的问题，编制了SMA和MFR观测值列表，以针对观测值进行测试，并概述了研究活动，以缩小我们目前的理解差距。我们认为，多视点多热日冕观测和多高度矢量磁场测量相结合是最终解决这一问题的最佳途径。我们使用MHD模拟和合成日冕图像来证明这种方法，我们的主要结论是，用SMA和MFR来区分喷发前的结构似乎是人为的。如果喷发前的构造处于从SMA到MFR不断演变的混合状态，则观测和建模都可以保持一致。因此，一个给定的配置的“占主导地位”的性质将在很大程度上取决于它的进化阶段（SMA一样的早期，MFR一样的喷发）。
A clear understanding of the nature of the pre-eruptive magnetic field configurations of Coronal Mass Ejections (CMEs) is required for understanding and eventually predicting solar eruptions. Only two, but seemingly disparate, magnetic configurations are considered viable; namely, sheared magnetic arcades (SMA) and magnetic flux ropes (MFR). They can form via three physical mechanisms (flux emergence, flux cancellation, helicity condensation). Whether the CME culprit is an SMA or an MFR, however, has been strongly debated for thirty years. We formed an International Space Science Institute (ISSI) team to address and resolve this issue and report the outcome here. We review the status of the field across modeling and observations, identify the open and closed issues, compile lists of SMA and MFR observables to be tested against observations and outline research activities to close the gaps in our current understanding. We propose that the combination of multi-viewpoint multi-thermal coronal observations and multi-height vector magnetic field measurements is the optimal approach for resolving the issue conclusively. We demonstrate the approach using MHD simulations and synthetic coronal images.Our key conclusion is that the differentiation of pre-eruptive configurations in terms of SMAs and MFRs seems artificial. Both observations and modeling can be made consistent if the pre-eruptive configuration exists in a hybrid state that is continuously evolving from an SMA to an MFR. Thus, the ‘dominant’ nature of a given configuration will largely depend on its evolutionary stage (SMA-like early-on, MFR-like near the eruption).