A forward‐reverse shock pair in the solar wind driven by over‐expansion of a coronal mass ejection: Ulysses observations
A forward‐reverse shock pair in the solar wind driven by over‐expansion of a coronal mass ejection: Ulysses observations
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由日冕物质抛射过度膨胀驱动的太阳风中的正向-反向激波对：尤利西斯观测
DOI：
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发表时间：
1994
期刊：
影响因子：
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通讯作者：
A. Balogh
中科院分区：
文献类型：
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作者：
J. Gosling;S. Bame;D. McComas;J. Phillips;E. Scime;V. Pizzo;B. Goldstein;A. Balogh
在4.64 Au和S32.5°的太阳风正-反向激波对中，观测到了一种以前未被确认的类型。与大多数由快速太阳风等离子体和慢速等离子体之间的速度差驱动的太阳风正向-反向激波对相反，这个特殊的激波对纯粹是由来自太阳的日冕物质抛射（CME）的过度膨胀驱动的。一个简单的数值模拟表明，过度膨胀的结果是一个高的初始内部等离子体和磁场压力内的CME。在4.64 Au观测到的CME具有磁通绳的内部场结构。这一事件与太阳扰动有关，在11天前，新的磁环几乎直接在日冕的正下方形成。这种关联表明，通量绳是由于上升的CME内相邻磁环的“腿”之间的重连而产生的。
A previously unidentified type of solar wind forward-reverse shock pair has been observed by Ulysses at 4.64 AU and S32.5°. In contrast to most solar wind forward-reverse shock pairs, which are driven by the speed difference between fast solar wind plasma and slower plasma ahead, this particular shock pair was driven purely by the over-expansion of a coronal mass ejection, CME, in transit from the Sun. A simple numerical simulation indicates that the overexpansion was a result of a high initial internal plasma and magnetic field pressure within the CME. The CME observed at 4.64 AU had the internal field structure of a magnetic flux rope. This event was associated with a solar disturbance in which new magnetic loops formed in the corona almost directly beneath Ulysses ∼11 days earlier. This association suggests that the flux rope was created as a result of reconnection between the “legs” of neighboring magnetic loops within the rising CME.