Combining STEREO heliospheric imagers and Solar Orbiter to investigate the evolution of the 2022 March 10 CME
Combining STEREO heliospheric imagers and Solar Orbiter to investigate the evolution of the 2022 March 10 CME
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结合 STEREO 日光层成像仪和太阳轨道飞行器来研究 2022 年 3 月 10 日日冕物质抛射的演变
DOI：
10.1051/0004-6361/202347561
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发表时间：
2024
影响因子：
6.5
通讯作者：
Galvin, A. B.
中科院分区：
文献类型：
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作者：
Zhuang, B.;Lugaz, N.;Al-Haddad, N.;Scolini, C.;Farrugia, C. J.;Regnault, F.;Davies, E. E.;Yu, W.;Winslow, R. M.;Galvin, A. B.
日冕物质抛射（CME）是从日冕喷发到行星际空间的磁化等离子体的大尺度结构。2020年发射的太阳轨道器（SolO）能够在日光层最内层对CME进行现场测量，在这样的距离上，CME可以在日光层成像仪（HI）的内视场内进行远程观测。因此，它提供了机会，调查的对应关系的日冕物质抛射子结构在现场测量和远程观察。我们研究了一个CME，它开始于2022年3月10日，由SolO在0.44 Au进行原位测量。目的结合广角成像仪对CME的远程观测和最内层日光层的原位测量，使我们能够比较通过两种技术得出的CME属性，验证估计，并更好地理解CME的演变，特别是大小和径向膨胀，在0.5 Au.MethodsWe比较了不同的CME子结构的演变观察到的图像从HIs上的Ahead日地关系天文台（STEREO-A）和CME的签名测量SolO原位。CME在其后缘具有密度增强的远程和原位观测，这验证了使用密度增强的签名后CME准确地识别CME后缘。我们还估计和比较的径向尺寸和径向扩张速度的不同的子结构在这两个observation.ResultsThe远程图像中的CME的前，后边缘的演变是一致的原位CME测量。径向膨胀（即，径向尺寸和径向膨胀速度）与SolO同时获得的原位估计结果一致。然而，我们没有发现这样的磁喷出物区域内的CME，因为它是很难识别的磁喷出物的边缘在远程图像。
ContextCoronal mass ejections (CMEs) are large-scale structures of magnetized plasma that erupt from the corona into interplanetary space. The launch of Solar Orbiter (SolO) in 2020 enables in situ measurements of CMEs in the innermost heliosphere, at such distances where CMEs can be observed remotely within the inner field of view of heliospheric imagers (HIs). It thus provides the opportunity for investigations into the correspondence of the CME substructures measured in situ and observed remotely. We studied a CME that started on 2022 March 10 and was measured in situ by SolO at ∼0.44 au.AimsCombining remote observations of CMEs from wide-angle imagers and in situ measurements in the innermost heliosphere allows us to compare CME properties derived through both techniques, validate the estimates, and better understand CME evolution, specifically the size and radial expansion, within 0.5 au.MethodsWe compared the evolution of different CME substructures observed in images from the HIs on board the Ahead Solar Terrestrial Relations Observatory (STEREO-A) and the CME signatures measured in situ by SolO. The CME is found to possess a density enhancement at its rear edge in both remote and in situ observations, which validates the use of the signature of density enhancement following the CMEs to accurately identify the CME rear edge. We also estimated and compared the radial size and radial expansion speed of different substructures in both observations.ResultsThe evolution of the CME front and rear edges in remote images is consistent with the in situ CME measurements. The radial expansion (i.e., radial size and radial expansion speed) of the whole CME structure consisting of the magnetic ejecta and the sheath is consistent with the in situ estimates obtained at the same time from SolO. However, we do not find such consistencies for the magnetic ejecta region inside the CME because it is difficult to identify the magnetic ejecta edges in the remote images.