On the coronal magnetic field: Consequences of large-scale motions
On the coronal magnetic field: Consequences of large-scale motions
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DOI：
10.1086/307556
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发表时间：
1999-08-20
影响因子：
4.9
通讯作者：
Schwadron, NA
中科院分区：
文献类型：
--
作者：
Fisk, LA;Zurbuchen, TH;Schwadron, NA
介绍了日球层磁场的一个模型，在该模型中，磁力线在日光纬度上发生较大的漂移。这些漂移是由于光球层的差异旋转和太阳附近太阳风的非径向膨胀之间的相互作用造成的。该模型解释了观察到的低刚性粒子在太阳风中在纬度上传播的容易程度。本文探讨了该模型对日冕磁场行为的影响。指出该模型解释了极地冕洞的时间演化和视刚性自转以及快太阳风和慢太阳风的差异。
A model has been introduced for the magnetic field in the heliosphere in which the field lines execute large excursions in heliographic latitude. The excursions result from the interplay between the differential rotation of the photosphere and the nonradial expansion of the solar wind near the Sun. The model accounts for the observed ease with which low-rigidity particles propagate in latitude in the solar wind. In this paper the consequences of this model for the behavior of the coronal magnetic field are explored. It is pointed out that the model provides an explanation for the time evolution and apparent rigid rotation of polar coronal holes and the differences between fast and slow solar wind.