Saturn's magnetospheric dynamics
Saturn's magnetospheric dynamics
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DOI：
10.1002/2013gl057967
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发表时间：
2013-10
影响因子：
5.2
通讯作者：
M. Thomsen
中科院分区：
文献类型：
--
作者：
M. Thomsen
土星磁层的动力学是由该系统的两个主要特征驱动的：首先，磁层等离子体的主要来源是位于磁层深处的冰卫星土卫二;其次，像木星一样，土星是一个非常快的旋转体，旋转周期只有10.7小时。动力学的要求是使磁层摆脱持续供应的等离子体，而快速旋转提供了这样做的机制。因此，磁层动力学与质量传输过程密切相关，包括径向扩散、通量管交换、磁重联和等离子体团形成。我们回顾最近的进展和新的问题，这些过程在土星。
The dynamics of Saturn's magnetosphere are driven by two major features of the system: First, the dominant source of magnetospheric plasma is the icy moon Enceladus, located deep within the magnetosphere; and second, like Jupiter, Saturn is a very fast rotator, with a rotational period of only 10.7 h. The dynamical imperative is to rid the magnetosphere of the continuously supplied plasma, and the fast rotation provides the mechanisms to do so. Thus, magnetospheric dynamics are intimately related to mass transport processes, including radial diffusion, flux tube interchange, magnetic reconnection, and plasmoid formation. We review recent progress and new questions relating to these processes at Saturn.