Evidence of a Flux-Rope Model for Corona Mass Ejections Based on Observations of the Limb Prominence Eruption on 2002 January 4
Evidence of a Flux-Rope Model for Corona Mass Ejections Based on Observations of the Limb Prominence Eruption on 2002 January 4
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基于 2002 年 1 月 4 日肢突喷发观测的日冕物质抛射通量绳模型的证据
DOI：
10.1086/341628
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发表时间：
2002
期刊：
影响因子：
--
通讯作者：
V. Yurchyshyn
中科院分区：
文献类型：
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作者：
V. Yurchyshyn
我们报告了在Kanzelhöhe太阳天文台Hα图像，太阳和日光层天文台（SOHO）EUV成像望远镜（EIT）195图像和日冕SOHO大角度光谱日冕仪C2图像中看到的日珥喷发。我们的数据支持日冕物质抛射（CME）的通量绳模型，这表明通量绳在喷发之前很久就形成了。我们的结论是基于爆发前磁场结构的三部分结构，以及第一次Hα，SOHO EIT 195 α增亮发生在暗条开始上升后约15分钟的事实。这些数据还清楚地表明了标准耀斑模型中两个很少观察到的组成部分：（1）覆盖在爆发前暗条上的磁环和（2）由上升暗条垂直拉伸的磁力线。这些磁力线在水平方向上被压缩，并相互靠近，在那里它们重新连接，形成了一个明显增长的耀斑后环系统。
We report on a prominence eruption as seen in Kanzelhöhe Solar Observatory Hα images, Solar and Heliospheric Observatory (SOHO) EUV Imaging Telescope (EIT) 195 Å images, and coronal SOHO Large Angle Spectrometric Coronograph C2 images. Our data favor the flux-rope model for coronal mass ejections (CMEs), which suggests that a flux rope is formed long before the eruption. Our conclusion is based on a three-part structure of the pre-erupted configuration of the magnetic field and on the fact that the first Hα, SOHO EIT 195 Å brightenings occurred some 15 minutes after the filament began to ascend. The data also clearly demonstrate two rarely observed components of the standard flare model: (1) magnetic loops that overlay the pre-erupted filament and (2) magnetic field lines stretched vertically by the ascending filament. These field lines are compressed horizontally and move toward each other where they reconnect to form an apparently growing post-flare loop system.