OBSERVING FLUX ROPE FORMATION DURING THE IMPULSIVE PHASE OF A SOLAR ERUPTION
OBSERVING FLUX ROPE FORMATION DURING THE IMPULSIVE PHASE OF A SOLAR ERUPTION
复制标题
观察太阳喷发脉冲阶段磁通绳的形成
DOI：
10.1088/2041-8205/732/2/l25
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发表时间：
2011-05-10
影响因子：
7.9
通讯作者：
Ding, M. D.
中科院分区：
文献类型：
--
作者：
Cheng, X.;Zhang, J.;Ding, M. D.
磁通绳被认为是日冕物质抛射（CME）的重要结构组成部分。虽然存在大量喷发后磁通绳的观测证据，例如。例如，从遥感日冕仪图像或现场太阳风数据中可以看出，在日冕物质抛射脉冲阶段直接观测磁通绳是很少见的。在这封信中，我们对仍处于低电晕形成阶段的磁通绳进行了明确的观察。感兴趣的日冕物质抛射发生于 2010 年 11 月 3 日，其脚点部分被遮挡。磁通绳被视为大气成像组件 (AIA) 131 埃通带（峰值温度类似于 11 MK）中的一团明亮的热等离子体，从源活动区域的核心升起，快速向外移动，并向上拉伸周围的背景磁场。拉伸的磁场似乎在核心后面弯曲，类似于喷发耀斑中的经典磁重联场景。另一方面，磁通绳在AIA 211埃通带（2.0 MK）和171埃通带（0.6 MK）中表现为暗腔；在这些相对较冷的温度带中，明亮的边缘清楚地包围了黑暗的空腔。明亮的边缘可能代表了周围日冕等离子体被膨胀的通量绳压缩的堆积。 AIA 多个温度带中看到的复合结构与相应日冕仪图像中的复合结构非常相似，由明亮的前缘和黑暗的空腔组成，通常认为是磁通绳。
Magnetic flux ropes are believed to be an important structural component of coronal mass ejections (CMEs). While there exists much observational evidence of flux ropes after the eruption, e. g., as seen in remote-sensing coronagraph images or in situ solar wind data, the direct observation of flux ropes during CME impulsive phase has been rare. In this Letter, we present an unambiguous observation of a flux rope still in the formation phase in the low corona. The CME of interest occurred above the east limb on 2010 November 3 with footpoints partially blocked. The flux rope was seen as a bright blob of hot plasma in the Atmospheric Imaging Assembly (AIA) 131 angstrom passband (peak temperature similar to 11 MK) rising from the core of the source active region, rapidly moving outward and stretching the surrounding background magnetic field upward. The stretched magnetic field seemed to curve-in behind the core, similar to the classical magnetic reconnection scenario in eruptive flares. On the other hand, the flux rope appeared as a dark cavity in the AIA 211 angstrom passband (2.0 MK) and 171 angstrom passband (0.6 MK); in these relatively cool temperature bands, a bright rim clearly enclosed the dark cavity. The bright rim likely represents the pileup of the surrounding coronal plasma compressed by the expanding flux rope. The composite structure seen in AIA multiple temperature bands is very similar to that in the corresponding coronagraph images, which consists of a bright leading edge and a dark cavity, commonly believed to be a flux rope.