NUMERICAL SIMULATION OF FAST-MODE MAGNETOSONIC WAVES EXCITED BY PLASMOID EJECTIONS IN THE SOLAR CORONA
NUMERICAL SIMULATION OF FAST-MODE MAGNETOSONIC WAVES EXCITED BY PLASMOID EJECTIONS IN THE SOLAR CORONA
复制标题
日冕等离子体喷射激发的快模磁声波的数值模拟
DOI：
10.1088/0004-637x/800/2/111
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发表时间：
2015-02
影响因子：
4.9
通讯作者：
Feng Xueshang
中科院分区：
文献类型：
--
作者：
Yang Liping;Zhang Lei;He Jiansen;Peter Hardi;Tu Chuanyi;Wang Linghua;Zhang Shaohua;Feng Xueshang
太阳动力学观测台上的大气成像组件仪器直接对沿着日冕磁漏斗连续向外传播的快速传播磁声波进行了成像。在这项研究中，我们进行了一个数值调查的激励的FMWs在交换重联的情况下，与足点剪切流被用来激励系统和驱动重联。模拟结果表明，由于磁场重联，电流片中的等离子体被焦耳耗散加热到1000 MK，并迅速喷出，发展出热流出。与此同时，电流片被撕裂成等离子体团，这些等离子体团被快速地向上和向下射出。当等离子体团到达流出区域时，它们与那里的环境磁场发生碰撞和碰撞，从而连续发射FMW。FMWs从撞击区域向外发散传播，其相速度为Alfvén速度的1000 km s−1。在傅立叶波功率的k − ω图中，FMWs显示了一个宽的频率分布，其中有一个代表色散关系的直脊。在WKB近似下，在距波源15 Mm处，我们估计FMWs的能流为E = 7.0 × 106 erg cm−2 s−1，比管道通道重联流出的能流小50倍。这些模拟结果表明，在能量和动力上，外流比波浪重要得多。
The Atmospheric Imaging Assembly instrument on board the Solar Dynamics Observatory has directly imaged the fast-propagating magnetosonic waves (FMWs) successively propagating outward along coronal magnetic funnels. In this study we perform a numerical investigation of the excitation of FMWs in the interchange reconnection scenario, with footpoint shearing flow being used to energize the system and drive the reconnection. The modeling results show that as a result of magnetic reconnection, the plasma in the current sheet is heated up by Joule dissipation to ∼10 MK and is ejected rapidly, developing the hot outflows. Meanwhile, the current sheet is torn into plasmoids, which are shot quickly both upward and downward. When the plasmoids reach the outflow regions, they impact and collide with the ambient magnetic field there, which consecutively launches FMWs. The FMWs propagate outward divergently away from the impact regions, with a phase speed of the Alfvén speed of ∼1000 km s−1. In the k − ω diagram of the Fourier wave power, the FMWs display a broad frequency distribution with a straight ridge that represents the dispersion relation. With the WKB approximation, at the distance of 15 Mm from the wave source region, we estimate the energy flux of FMWs to be E ∼ 7.0 × 106 erg cm−2 s−1, which is ∼50 times smaller than the energy flux related to the tube-channeled reconnection outflow. These simulation results indicate that energetically and dynamically the outflow is far more important than the waves.
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影响因子：
56.9
作者：
T. J. Okamoto;S. Tsuneta;T. E. Berger;K. Ichimoto;Y. Katsukawa;B. Lites;S. Nagata;K. Shibata
通讯作者：
T. J. Okamoto;S. Tsuneta;T. E. Berger;K. Ichimoto;Y. Katsukawa;B. Lites;S. Nagata;K. Shibata
影响因子：
56.9
作者：
Jess, David B.;Mathioudakis, Mihalis;Christian, Damian J.
通讯作者：
Christian, Damian J.
DOI：
10.1088/2041-8205/775/1/l23
发表时间：
2013-08
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
Tongjiang Wang;L. Ofman;J. Davila
通讯作者：
Tongjiang Wang;L. Ofman;J. Davila
影响因子：
6.5
作者：
M. Bárta;B. Vršnak;M. Karlický
通讯作者：
M. Bárta;B. Vršnak;M. Karlický
DOI：
10.1046/j.1365-8711.2001.04491.x
发表时间：
2001-09
影响因子：
4.8
作者：
David R. Williams;K. Phillips;P. Rudawy;M. Mathioudakis;P. Gallagher;E. O'Shea;F. Keenan;P. Read-P
通讯作者：
David R. Williams;K. Phillips;P. Rudawy;M. Mathioudakis;P. Gallagher;E. O'Shea;F. Keenan;P. Read-P