Multi point analysis of coronal mass ejection flux ropes using combined data from Solar Orbiter, BepiColombo and Wind
Multi point analysis of coronal mass ejection flux ropes using combined data from Solar Orbiter, BepiColombo and Wind
复制标题
使用太阳轨道飞行器、BepiColombo 和 Wind 的组合数据对日冕物质抛射通量绳进行多点分析
DOI：
10.1051/0004-6361/202140919
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发表时间：
2021
影响因子：
6.5
通讯作者：
Wolfgang Baumjohann
中科院分区：
文献类型：
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作者：
A. Weiss;C. Moestl;E. Davies;T. Amerstorfer;M. Bauer;J. Hinterreiter;M. Reiss;R. Bailey;T. Horbury;H. O’Brien;V. Evans;V. Angelini;D. Heiner;I. Richter;H. Auster;W. Magnes;D. Fischer;Wolfgang Baumjohann
最近发射的太阳轨道飞行器和贝皮科伦坡号打开了一个短暂的窗口，这两个航天器位于一个星座中，可以对任何面向地球的日冕物质抛射进行详细采样。幸运的是，太阳轨道飞行器于 2020 年 4 月 19 日和 5 月 28 日对 ICME 进行了原位探测，发生了两起这样的事件。大约一天后，BepiColombo 和 Wind 也对这两起事件进行了原位观测。我们尝试使用经验磁通绳模型同时重建所有三个航天器的现场磁场测量。这使我们能够在更大、更全球的范围内测试磁通绳模型的有效性，并允许对不同航天器组合的分析进行交叉验证。最后，我们还可以将现场建模的结果与 STEREO-A 日光层成像仪获得的远程观测结果进行比较。我们利用 3D 冠状绳弹射模型来模拟 ICME 演化。我们采用了先前开发的 ABC-SMC 拟合算法来应用于多点场景。我们表明，我们能够使用我们的模型结合磁通绳拟合算法同时重建三个不同航天器位置的磁通绳特征。对于 4 月 19 日的 ICME，我们的方法非常有效。另一方面，5 月 28 日的 ICME 显示了我们方法的局限性。不幸的是，对这些事件使用多点观测似乎并没有解决固有问题，例如由于航天器位置的特定星座而估计磁场扭曲或磁通绳纵横比。由于我们的通用方法可用于任何基于快进模拟的模型，因此我们为使用更先进的 ICME 模型的未来研究提供了蓝图。
The recent launch of Solar Orbiter and BepiColombo opened a brief window in which these two spacecraft were positioned in a constellation that allows for the detailed sampling of any Earth-directed CMEs. Fortunately, two such events occurred with in situ detections of an ICME by Solar Orbiter on the 19th of April and the 28th of May 2020. These two events were subsequently also observed in situ by BepiColombo and Wind around a day later. We attempt to reconstruct the observed in situ magnetic field measurements for all three spacecraft simultaneously using an empirical magnetic flux rope model. This allows us to test the validity of our flux rope model on a larger and more global scale and allows for cross-validation of the analysis with different spacecraft combinations. Finally, we can also compare the results from the in situ modeling to remote observations obtained from the STEREO-A heliospheric imagers. We make use of the 3D coronal rope ejection model in order to simulate the ICME evolution. We adapt a previously developed ABC-SMC fitting algorithm for the application to multi point scenarios. We show that we are able to generally reconstruct the flux ropes signatures at three different spacecraft positions simultaneously using our model in combination with the flux rope fitting algorithm. For the well-behaved 19th of April ICME our approach works very well. The 28th of May ICME, on the other hand, shows the limitations of our approach. Unfortunately, the usage of multi-point observations for these events does not appear to solve inherent issues, such as the estimation of the magnetic field twist or flux rope aspect-ratios due to the specific constellation of the spacecraft positions. As our general approach can be used for any fast forward simulation-based model we give a blueprint for future studies using more advanced ICME models.