A solar storm observed from the Sun to Venus using the STEREO, Venus Express, and MESSENGER spacecraft
A solar storm observed from the Sun to Venus using the STEREO, Venus Express, and MESSENGER spacecraft
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DOI：
10.1029/2008ja014034
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发表时间：
2009-07
影响因子：
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通讯作者：
A. Rouillard;J. Davies;R. Forsyth;N. Savani;N. Sheeley;A. Thernisien;Tielong Zhang;R. A. Howard;B. Anderson;C. Carr;S. Tsang;M. Lockwood;C. Davis;R. Harrison;D. Bewsher;M. Fränz;S. Crothers;C. Eyles;Daniel S. Brown;I. Whittaker;M. Hapgood;A. Coates;G. Jones;M. Grande;R. Frahm;J. Winningham
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文献类型：
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作者：
A. Rouillard;J. Davies;R. Forsyth;N. Savani;N. Sheeley;A. Thernisien;Tielong Zhang;R. A. Howard;B. Anderson;C. Carr;S. Tsang;M. Lockwood;C. Davis;R. Harrison;D. Bewsher;M. Fränz;S. Crothers;C. Eyles;Daniel S. Brown;I. Whittaker;M. Hapgood;A. Coates;G. Jones;M. Grande;R. Frahm;J. Winningham
STEREO-A航天器上的SECCHI光学成像仪器套件用于跟踪2007年5月期间从太阳向日光层传播的太阳风暴，该风暴由若干日冕物质抛射和其他日冕环组成。利用STEREO-A（HI-1/2A）上的SECCHI日球成像仪（HI）的观测资料，确定了最大行星际日冕物质抛射（ICME）的三维传播路径。通过SECCHI图像跟踪了CME的两个部分，一个明亮的环和一个位于事件后部的V形特征。我们表明，这两种结构可能是位于一个单一的磁通绳的电子散射光的视线整合的结果。除了被HI成像外，CME还被金星快车和信使号航天器上的等离子体和磁场实验同时观测。正如预期的那样，成像的环和V形结构束缚了现场观察到的磁通绳。SECCHI图像显示，领先的环状结构比V形结构传播得更快，并且在磁通绳通过期间发生了原位CME速度的降低。我们将其解释为磁绳向外穿过行星际介质时不断径向膨胀的结果。直接从SECCHI-HI图像中获得的径向膨胀速度约为30 km/s，与现场观测到的两个结构的速度差异一致。本文表明，磁绳的位置可以确定从白色光图像，这可能有重要的空间天气应用。
The suite of SECCHI optical imaging instruments on the STEREO-A spacecraft is used to track a solar storm, consisting of several coronal mass ejections (CMEs) and other coronal loops, as it propagates from the Sun into the heliosphere during May 2007. The 3-D propagation path of the largest interplanetary CME (ICME) is determined from the observations made by the SECCHI Heliospheric Imager (HI) on STEREO-A (HI-1/2A). Two parts of the CME are tracked through the SECCHI images, a bright loop and a V-shaped feature located at the rear of the event. We show that these two structures could be the result of line-of-sight integration of the light scattered by electrons located on a single flux rope. In addition to being imaged by HI, the CME is observed simultaneously by the plasma and magnetic field experiments on the Venus Express and MESSENGER spacecraft. The imaged loop and V-shaped structure bound, as expected, the flux rope observed in situ. The SECCHI images reveal that the leading loop-like structure propagated faster than the V-shaped structure, and a decrease in in situ CME speed occurred during the passage of the flux rope. We interpret this as the result of the continuous radial expansion of the flux rope as it progressed outward through the interplanetary medium. An expansion speed in the radial direction of similar to 30 km s(-1) is obtained directly from the SECCHI-HI images and is in agreement with the difference in speed of the two structures observed in situ. This paper shows that the flux rope location can be determined from white light images, which could have important space weather applications.