Coronal Condensations Caused by Magnetic Reconnection between Solar Coronal Loops
Coronal Condensations Caused by Magnetic Reconnection between Solar Coronal Loops
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太阳日冕环之间的磁重联引起的日冕凝聚
DOI：
10.3847/2041-8213/aad90a
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发表时间：
2018-08
影响因子：
7.9
通讯作者：
Yijun Hou
中科院分区：
文献类型：
--
作者：
Leping Li;Jun Zhang;Hardi Peter;Lakshmi Pradeep Chitta;Jiangtao Su;Chun Xia;Hongqiang Song;Yijun Hou
利用太阳动力学天文台/大气成像组件（AIA）多波长图像，我们报告了开环和闭环系统之间磁重联（MR）期间的日冕凝结。在太阳边缘上方的 AIA 171 Å 图像中观察到，地势较高的磁开放结构向下移动并与地势较低的闭合环相互作用，导致前者形成倾角。界面处形成X型结构。相互作用的循环重新连接并消失。然后，两组新重新连接的环路形成并从 MR 区域退出。在 MR 过程中，明亮的发射依次出现在较高位置开放结构的凹陷处的 AIA 131 和 304 Å 通道中。这表明较热等离子体从~0.9 MK 下降到~0.6 MK，然后到~0.05 MK 的冷却和凝结过程，AIA 171、131 和 304 Å 通道的光变曲线也支持这一点。支持凝结的部分较高位置的开放结构参与连续的MR。如果没有底层环路的支持，凝结物就会沿着新重新连接的环路雨点回到太阳表面。我们的结果表明，日冕环之间的磁流变导致了较热的日冕等离子体及其下流的凝结。因此，MR 在日冕等离子体的质量循环中发挥着积极作用，因为它可以引发灾难性的冷却和凝结。这强调了磁演化和热演化必须一起处理，不能分开，即使在灾难性冷却的情况下也是如此。
Employing Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA) multi-wavelength images, we report the coronal condensation during the magnetic reconnection (MR) between a system of open and closed coronal loops. Higher-lying magnetically open structures, observed in AIA 171 Å images above the solar limb, move downward and interact with the lower-lying closed loops, resulting in the formation of dips in the former. An X-type structure forms at the interface. The interacting loops reconnect and disappear. Two sets of newly reconnected loops then form and recede from the MR region. During the MR process, bright emission appears sequentially in the AIA 131 and 304 Å channels repeatedly in the dips of higher-lying open structures. This indicates the cooling and condensation process of hotter plasma from ∼0.9 MK down to ∼0.6 MK, and then to ∼0.05 MK, also supported by the light curves of the AIA 171, 131, and 304 Å channels. The part of higher-lying open structures supporting the condensation participate in the successive MR. Without support from underlying loops, the condensation then rains back to the solar surface along the newly reconnected loops. Our results suggest that the MR between coronal loops leads to the condensation of hotter coronal plasma and its downflows. MR thus plays an active role in the mass cycle of coronal plasma because it can initiate the catastrophic cooling and condensation. This underlines that the magnetic and thermal evolution has to be treated together and cannot be separated, even in the case of catastrophic cooling.
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影响因子：
2.8
作者：
W. Pesnell;B. Thompson;P. Chamberlin
通讯作者：
W. Pesnell;B. Thompson;P. Chamberlin
DOI：
10.1086/318053
发表时间：
2001
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
Takaaki Yokoyama;K. Akita;T. Morimoto;K. Inoue;Jeffrey Newmark
通讯作者：
Takaaki Yokoyama;K. Akita;T. Morimoto;K. Inoue;Jeffrey Newmark
DOI：
10.1088/2041-8205/723/1/l28
发表时间：
2010-09
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
Rui Liu;Jeongwoo Lee;Tongjiang Wang;G. Stenborg;Chang Liu;Haimin Wang
通讯作者：
Rui Liu;Jeongwoo Lee;Tongjiang Wang;G. Stenborg;Chang Liu;Haimin Wang
与受限细丝喷发相关的交汇处重新连接：对太阳风中瞬态冷密等离子体来源的影响
影响因子：
4.9
作者：
Zheng Ruisheng;Chen Yao;Wang Bing;Li Gang;Xiang Yongyuan
通讯作者：
Xiang Yongyuan
DOI：
10.1088/0004-637x/806/1/115
发表时间：
2015-04
期刊：
The Astrophysical Journal
影响因子：
--
作者：
T. Kaneko;T. Yokoyama
通讯作者：
T. Kaneko;T. Yokoyama