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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Magnetospheric configuration and dynamics of Saturn's magnetosphere: A global MHD simulation
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Magnetospheric configuration and dynamics of Saturn's magnetosphere: A global MHD simulation

机译：磁性层的配置和动态土星磁层:全球磁流体动力模拟

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We investigate the solar wind interaction with Saturn's magnetosphere by using a global magnetohydrodynamic simulation driven by an idealized time-varying solar wind input that includes features of Corotating Interaction Regions typically seen at Saturn. Our model results indicate that the compressibility of Saturn's magnetosphere is intermediate between the Earth's and Jupiter's, and the magnetopause location appears insensitive to the orientation of the interplanetary magnetic field. The modeled dependences of both the magnetopause and bow shock locations on the solar wind dynamic pressure agree reasonably well with those of data-based empirical models. Our model shows that the centrifugal acceleration of mass-loaded flux tubes leads to reconnection on closed field lines forming plasmoids, an intrinsic process ("Vasyliunas-cycle") in Saturn's magnetosphere taking place independent of the external conditions. In addition, another type of reconnection process involving open flux tubes ("Dungey-cycle") is also seen in our simulation when the external condition is favorable for dayside reconnection. Under such circumstances, plasmoid formation in the tail involves reconnection between open field lines in the lobes, producing stronger global impacts on the magnetosphere and ionosphere compared to that imposed by the Vasyliunas-cycle directly. Our model also shows that large-scale tail reconnection may be induced by compressions driven by interplanetary shocks. In our simulation, large-scale tail reconnection and plasmoid formation take place in a quasi-periodic manner but the recurrence rate tends to be higher as the dynamic pressure becomes higher. While large-scale plasmoid release clearly is an important process in controlling the magnetospheric dynamics, it appears insufficient to account for all the losses of plasma added by the magnetospheric sources. We find that a large fraction of the planetary plasma is lost through the magnetotail near the flanks probably through relatively small-scale plasmoids, a situation that may also exist at Jupiter.
机译：我们研究太阳风相互作用土星磁层通过使用一个全局的磁流体动力模拟驱动的理想化的时变输入,太阳风包括共转交互的特点区域通常出现在土星。结果表明,压缩系数土星磁层之间的中间地球和木星的磁层似乎不敏感方向位置行星际磁场。依赖性的磁层和弓太阳风动态冲击位置压力与合理地同意基于数据的实证模型。mass-loaded通量的离心加速度管导致封闭电场线重新连接形成等离子粒团,一个内在的过程(“Vasyliunas-cycle”)在土星的磁场发生独立的外部条件。重联过程涉及开放通量管(“Dungey-cycle”)也出现在我们的模拟当外部条件是有利的的光面重新连接。尾巴等离子粒团的形成涉及到重新连接开放电场线之间叶,产生更强的全球影响磁层、电离层相比直接Vasyliunas-cycle强加的。模型还表明,大规模的尾巴重新连接可能引起按压由行星际的冲击。模拟、大规模的尾巴重新连接等离子粒团形成准周期性的发生但是复发率往往是更高的随着动态压力变得更高。大型等离子粒团显然是一种释放重要的过程控制磁性层的动态,似乎不够占所有添加的等离子体的损失地球资源。行星的一部分等离子体丢失附近的磁尾侧翼可能通过相对小规模的等离子粒团,情况在木星也可能存在。

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