The Dynamical Behavior of Reconnection-driven Termination Shocks in Solar Flares: Magnetohydrodynamic Simulations
The Dynamical Behavior of Reconnection-driven Termination Shocks in Solar Flares: Magnetohydrodynamic Simulations
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太阳耀斑中重新连接驱动的终止激波的动力学行为：磁流体动力学模拟
DOI：
10.3847/1538-4357/aaeed3
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发表时间：
2018-12
影响因子：
4.9
通讯作者：
Chen Bin
中科院分区：
文献类型：
--
作者：
Shen Chengcai;Kong Xiangliang;Guo Fan;Raymond John C.;Chen Bin
在爆发性太阳耀斑中，当高速重联外流与闭合的密集耀斑环碰撞时形成的终止激波（TSs）被认为是等离子体加热和粒子加速的可能候选因素之一。在这项工作中，我们……
In eruptive solar flares, termination shocks (TSs), formed when high-speed reconnection outflows collide with closed dense flaring loops, are believed to be one of the possible candidates for plasma heating and particle acceleration. In this work, we perform resistive magnetohydrodynamic simulations in a classic Kopp–Pneuman flare configuration to study the formation and evolution of TSs, and we analyze in detail the dynamic features of TSs and variations of the shock strength in space and time. This research focuses on the fast-reconnection phase when plasmoids form and produce small-scale structures inside the flare current sheet. It is found that the TS emerges once the downward outflow colliding with closed magnetic loops becomes supermagnetosonic and immediately becomes highly dynamical. The morphology of a TS can be flat, oblique, or curved depending on the detailed interactions between the outflows/plasmoids and the highly dynamic plasma in the loop-top region. The TS becomes weaker when a plasmoid is crossing through, or may even be destroyed by well-developed plasmoids and then reconstructed above the plasmoids. We also perform detailed statistical analysis on important physical quantities along and across the shock front. The density and temperature ratios range from 1 to 3 across the TS front, and the pressure ratio typically has larger values up to 10. We show that weak guide fields do not strongly affect the Mach number and compression ratios, and the TS length becomes slightly larger in the case with thermal conduction.
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影响因子：
2.5
作者：
A. Soward;E. Priest
通讯作者：
A. Soward;E. Priest
DOI：
10.1088/0004-637x/737/1/14
发表时间：
2011-08
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Chengcai Shen;Jun Lin;N. Murphy
通讯作者：
Chengcai Shen;Jun Lin;N. Murphy
DOI：
10.1029/97ja00976
发表时间：
1997-01
期刊：
Journal of Geophysical Research: Space Physics
影响因子：
--
作者：
James A. Miller;P. Cargill;A. Emslie;G. Holman;B. Dennis;T. N. Rosa;R. Winglee;S. G. Benka
通讯作者：
James A. Miller;P. Cargill;A. Emslie;G. Holman;B. Dennis;T. N. Rosa;R. Winglee;S. G. Benka
DOI：
10.1086/304449
发表时间：
1997-08
期刊：
The Astrophysical Journal
影响因子：
--
作者：
B. Somov;T. Kosugi
通讯作者：
B. Somov;T. Kosugi
DOI：
10.3847/1538-4357/aabad4
发表时间：
2018-04
期刊：
The Astrophysical Journal
影响因子：
--
作者：
T. Forbes;D. Seaton;K. Reeves
通讯作者：
T. Forbes;D. Seaton;K. Reeves