An Erupting Filament and Associated CME Observed by Hinode, STEREO and SOHO
An Erupting Filament and Associated CME Observed by Hinode, STEREO and SOHO
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Hinode、STEREO 和 SOHO 观测到的喷发细丝和相关 CME
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发表时间：
2010
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通讯作者：
A. Bemporad
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作者：
K. Reeves;A. Bemporad
2007年5月启动了一次多航天器活动，用Hinode、STEREO和SOHO仪器（Hinode HOP 7）观测离边日冕。在这次活动中，5月9日，NOAA 10953在西翼发生了一次暗条喷发和一次日冕物质抛射（CME）。暗条爆发开始于13：40 UT左右，并导致4SW纬度的CME。值得注意的是，这一事件是由STEREO（EUVI和COR 1）和Hinode/EIS和SOHO/Urea光谱仪观测到的。我们提出了所有这些工具的结果。来自Stereo/EUVI A和B的He ii λ304谱线的高节奏数据被用于研究细丝的3-D膨胀。一个缓慢的上升阶段，在此期间的灯丝向南移动，其次是一个脉冲阶段，在此期间的灯丝似乎改变方向，然后有助于向西扩展的CME在STEREO/COR 1。Hinode/EIS用2”狭缝扫描灯丝爆发的区域。EIS谱显示出显着的非热增宽线在不同温度下发射的灯丝喷发的位置。日冕物质抛射也可以用SOHO/Umos仪器观测到：摄谱仪狭缝的中心位于1.7太阳半径，南纬5SW，记录到O VI λλ1032−1037和Si xii λ520谱线强度的突然增加。我们讨论了这个有趣的喷发事件的整体形态，并提供了一个初步的温度和密度结构的评估。
A multi-spacecraft campaign was set up in May 2007 to observe the off-limb corona with Hinode, STEREO and SOHO instruments (Hinode HOP 7). During this campaign, a filament eruption and a coronal mass ejection (CME) occurred on May 9 from NOAA 10953 at the West limb. The filament eruption starts around 13:40 UT and results in a CME at 4SW latitude. Remarkably, the event was observed by STEREO (EUVI and COR1) and by the Hinode/EIS and SOHO/UVCS spectrometers. We present results from all these instruments. High-cadence data from Stereo/EUVI A and B in the He ii λ304 line were used to study the 3-D expansion of the filament. A slow rising phase, during which the filament moved southward, was followed by an impulsive phase during which the filament appeared to change direction and then contribute to the westward-expanding CME as seen in STEREO/COR 1. Hinode/EIS was scanning with the 2” slit the region where the filament erupted. The EIS spectra show remarkable non-thermal broadening in lines emitted at different temperatures at the location of the filament eruption. The CME was also observed by the SOHO/UVCS instrument: the spectrograph slit was centered at 1.7 solar radii, at a latitude of 5SW and recorded a sudden increase in the O VI λλ1032−1037 and Si xii λ520 spectral line intensities. We discuss the overall morphology of this interesting eruptive event, and provide a preliminary assessment of its temperature and density structure.