Dynamics of solar coronal magnetic fields
Dynamics of solar coronal magnetic fields
复制标题
太阳日冕磁场的动力学
DOI：
10.1086/170799
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发表时间：
1991
期刊：
影响因子：
--
通讯作者：
T. Zang
中科院分区：
文献类型：
--
作者：
R. Dahlburg;S. Antiochos;T. Zang
开发了日冕磁场足点应力的 3D 时间相关数值模拟，以便将日冕活动与光球上足点运动造成的日冕磁场应力联系起来。模拟结果没有揭示磁重联、扭结或适合日珥形成的凹上磁场线的形成。结论是，与许多模型相反，单个拱廊的光球扭曲不会导致解释太阳活动所需的过程类型。
A 3D time-dependent numerical simulation of the foot-point stressing of coronal magnetic field was developed in order to relate coronal activity with the stressing of the coronal magnetic field by foot-point motions at the photosphere. The results of the simulation did not reveal magnetic reconnection, kinking, or the formation of concave-up magnetic field lines suitable for prominence formation. It is concluded that, contrary to many models, photospheric twisting of a single arcade does not lead to the type of processes required to explain solar activity.