Three-dimensional magnetic reconnection in the solar corona
Three-dimensional magnetic reconnection in the solar corona
复制标题
日冕中的三维磁重联
DOI：
10.1063/1.872571
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发表时间：
1997
影响因子：
2.2
通讯作者：
E. Priest
中科院分区：
文献类型：
--
作者：
E. Priest
在二维空间中，磁拓扑和零点分岔的概念是简单的。此外，磁重联的性质已经被相当好地理解，并且可以用新一代的快速重联机制来描述，称为几乎均匀重联和非均匀重联。然而，在复杂的三维（3-D）磁场中，例如存在于日冕中，这些现象才刚刚开始被探索，并且要复杂得多。最近研究了光球层由两个、三个和更多磁源依次产生的磁场的结构特性。通过每个3-D磁零点有一个孤立的脊柱磁力线和磁通表面称为风扇。扇形形成分界线表面，将体积分成拓扑上不同的区域，并且一个空的扇形可以终止于另一个空的脊，而脊终止于源或无穷远。复杂三维场景的骨架
In two dimensions the notions of magnetic topology and null-point bifurcations are straightforward. In addition, the nature of magnetic reconnection is fairly well understood and can be described by a new generation of fast reconnection mechanisms known as almost-uniform reconnection and nonuniform reconnection. However, in complex three-dimensional (3-D) magnetic fields, such as exist in the solar corona, these phenomena are only just beginning to be explored and are considerably more complex. The structural properties of the magnetic field created in turn by two, three and more magnetic sources at the photosphere have been recently studied. Passing through each 3-D magnetic null there is an isolated spine field line and a flux surface known as a fan. The fans form separatrix surfaces that separate the volume into topologically distinct regions, and the fan of one null can terminate at the spine of another null, while the spine terminates either at a source or at infinity. The skeleton of complex 3-D fie...
影响因子：
4.6
作者：
D. Biskamp
通讯作者：
D. Biskamp