Emergence of a Partially Split Flux Tube into the Solar Atmosphere
Emergence of a Partially Split Flux Tube into the Solar Atmosphere
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DOI：
10.1093/pasj/60.4.809
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发表时间：
2008-08
影响因子：
2.3
通讯作者：
T. Magara
中科院分区：
文献类型：
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作者：
T. Magara
我们进行了一个三维MHD模拟出现的部分分裂通量管进入太阳大气，这是集中在太阳上观察到的活动机制，如合并的磁极性区域的光球和形成的多通量域的日冕。模拟再现了与旋转流相关联的小极性区域合并成主极性区域，并且主极性区域随后在与小极性区域相同的方向上发展旋转流。根据光球合并过程，多通量域形成的日冕和电流层分离这些通量域向外传播的通量域扩展。我们还调查了注入到大气中的磁通量，能量和螺旋度的时间变化的部分分裂通量管看到的性质，在多极系统的螺旋度注入。
We performed a three-dimensional MHD simulation for the emergence of a partially split flux tube into the solar atmosphere, which was focused on the mechanism of activity observed on the Sun, such as the merging of magnetic polarity regions in the photosphere and the formation of multi-flux domains in the corona. The simulation reproduced that a small polarity region associated with a rotational flow merges into a main polarity region, and the main polarity region later develops a rotational flow in the same direction as the small polarity region. In accordance with the photospheric merging process, multi-flux domains form in the corona and a current layer separating these flux domains travels outward as the flux domains expand. We also investigated the time variations of the magnetic flux, energy, and helicity injected into the atmosphere by the partially split flux tube to see the nature of helicity injection in a multi-pole system.