The large field-of-view of the Sun Watcher using Active Pixel System detector and Image Processing (SWAP) instrument onboard the PRoject for Onboard Autonomy 2 (PROBA2) spacecraft provides a unique opportunity to study extended coronal structures observed in the EUV in conjunction with global coronal magnetic field simulations. A global non-potential magnetic field model is used to simulate the evolution of the global corona from 1 September 2014 to 31 March 2015, driven by newly emerging bipolar active regions determined from Helioseismic and Magnetic Imager (HMI) magnetograms. We compare the large-scale structure of the simulated magnetic field with structures seen off-limb in SWAP EUV observations. In particular, we investigate how successful the model is in reproducing regions of closed and open structures, the scale of structures, and compare the evolution of a coronal fan observed over several rotations. The model is found to accurately reproduce observed large-scale, off-limb structures. When discrepancies do arise they mainly occur off the east solar limb due to active regions emerging on the far side of the Sun, which cannot be incorporated into the model until they are observed on the Earth-facing side. When such “late” active region emergences are incorporated into the model, we find that the simulated corona self-corrects within a few days, so that simulated structures off the west limb more closely match what is observed. Where the model is less successful, we consider how this may be addressed, through model developments or additional observational products. Electronic Supplementary Material The online version of this article (10.1007/s11207-020-01668-2) contains supplementary material, which is available to authorized users.

中文翻译：

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使用 SWAP 和数据驱动的非势日冕磁场模型研究中日冕


太阳观察者的大视场使用星载自主项目 2 (PROBA2) 航天器上的主动像素系统探测器和图像处理 (SWAP) 仪器，为研究在 EUV 中观察到的扩展日冕结构提供了独特的机会全球日冕磁场模拟。全球非势磁场模型用于模拟2014年9月1日至2015年3月31日期间全球日冕的演变，该演变是由日震和磁成像仪（HMI）磁图确定的新出现的双极活动区域驱动的。我们将模拟磁场的大尺度结构与 SWAP EUV 观测中在肢体之外看到的结构进行了比较。特别是，我们研究了该模型在再现封闭和开放结构区域、结构规模方面的成功程度，并比较了在几次旋转中观察到的日冕扇的演化。该模型被发现可以准确地再现观察到的大型离肢结构。当差异确实出现时，它们主要发生在东太阳边缘，因为太阳远端出现了活跃区域，只有在面向地球的一侧观察到这些区域才能将其纳入模型中。当这种“晚期”活动区域的出现被纳入模型时，我们发现模拟的日冕会在几天内进行自我修正，从而使西肢外的模拟结构更接近于观察到的情况。如果模型不太成功，我们会考虑如何通过模型开发或其他观测产品来解决这个问题。电子补充材料 本文的在线版本 (10.1007/s11207-020-01668-2) 包含补充材料，可供授权用户使用。