A magnetohydrodynamic simulation of the bifurcation of tail lobes during intervals with a northward interplanetary magnetic field
A magnetohydrodynamic simulation of the bifurcation of tail lobes during intervals with a northward interplanetary magnetic field
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DOI：
10.1029/gl011i010p01018
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发表时间：
1984-10
影响因子：
5.2
通讯作者：
T. Ogino;R. Walker
中科院分区：
文献类型：
--
作者：
T. Ogino;R. Walker
利用三维磁流体动力学模型，研究了太阳风在向北行星际磁场作用下与地球磁层的相互作用。当向北的行星际磁场为5nt时，等离子体厚度在正午至午夜子午线平面附近变厚。当投射到极帽上时，它看起来像一条从午夜延伸到正午的狭窄通道。这种等离子体模式与三对对流细胞有关。高纬向太阳对流和北B/sub z/ Birkeland流是由极地磁合并引起的。
The interaction of the solar wind with the Earth's magnetosphere during a northward interplanetary magnetic field was studied by using a three-dimensional magnetohydrodynamic model. For a northward interplanetary magnetic field of 5 nT, the plasma sheer thickens near the noon-midnight meridian plane. When projected onto the polar cap this appears as a narrow channel extending from midnight towards noon. This plasma pattern is associated with three pairs of convection cells. The high latitude sunward convection and northern B/sub z/ Birkeland current are caused by magnetic merging in the polar region.