日冕场和新出射通量之间相对方位的影响：I.整体性质
The effect of the relative orientation between the coronal field and new emerging flux: I Global Properties
摘要：
从对流区进入日冕的磁通量的出现是日冕磁场动力学演化的一个重要过程。在本文中，我们扩展了我们以前的数值研究，在磁通量相互作用的过程中，作为一个最初扭曲的磁通量管出现到一个平面平行，冠状磁场。显着的差异被发现在动力学外观和演变的出现过程取决于上升的通量系统和任何预先存在的日冕场之间的相对取向。当通量系统几乎是反平行的，实验表明大量的重联，并展示了清晰的签名的高温等离子体位于高速流出区域从重联区域延伸。然而，具有更平行方向的通量系统的情况下，显示非常有限的重联和没有相关的功能。尽管两个通量系统之间的重连量非常不同，但发现仍然连接到原始管的新兴通量作为时间的函数达到相同的高度。作为对管通量损失的补偿，在垂直于初始通量管的主轴的方向上的新兴环路的范围中发现了明显的差异。增加磁重联的量减小了体积，这限制了剩余的管通量。
英文摘要：
The emergence of magnetic flux from the convection zone into the corona is an important process for the dynamical evolution of the coronal magnetic field. In this paper we extend our previous numerical investigations, by looking at the process of flux interaction as an initially twisted flux tube emerges into a plane parallel, coronal magnetic field. Significant differences are found in the dynamical appearance and evolution of the emergence process depending on the relative orientation between the rising flux system and any preexisting coronal field. When the flux systems are nearly anti-parallel, the experiments show substantial reconnection and demonstrate clear signatures of a high temperature plasma located in the high velocity outflow regions extending from the reconnection region. However, the cases that have a more parallel orientation of the flux systems show very limited reconnection and none of the associated features. Despite the very different amount of reconnection between the two flux systems, it is found that the emerging flux that is still connected to the original tube, reaches the same height as a function of time. As a compensation for the loss of tube flux, a clear difference is found in the extent of the emerging loop in the direction perpendicular to the main axis of the initial flux tube. Increasing amounts of magnetic reconnection decrease the volume, which confines the remaining tube flux.
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