Magnetospheric convection at Saturn as a function of IMF BZ
Magnetospheric convection at Saturn as a function of IMF BZ
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DOI：
10.1029/2006gl028373
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发表时间：
2007-01
影响因子：
5.2
通讯作者：
K. Fukazawa;Shun‐ichi Ogi;T. Ogino;R. Walker
中科院分区：
文献类型：
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作者：
K. Fukazawa;Shun‐ichi Ogi;T. Ogino;R. Walker
我们已经使用三维磁流体动力学模拟研究的行星际磁场（IMF）对土星的磁层的影响的情况下，没有IMF，向北和向南IMF。太阳下磁层顶和弓形激波位置对太阳风动压的变化敏感，但对IMF的变化不敏感。在没有IMF的情况下，黎明附近共转流和太阳风方向相反的地方产生了涡旋。对于BZ 0涡产生在早晨和傍晚，在那里的流动从尾部重联是相反的太阳风和共转。我们使用电离层的能量通量和向上的场向电流（FACs）作为扩散和离散极光的代理。当BZ > 0时，强劲的上行FAC延伸到上午的板块。最强的FAC产生在流动涡流中。
We have used three dimensional magnetohydrodynamic simulations to investigate the influence of the interplanetary magnetic field (IMF) on Saturn's magnetosphere for cases with no IMF, northward and southward IMF. The subsolar magnetopause and bow shock positions are sensitive to changes in the solar wind dynamic pressure but insensitive to changes in the IMF. Without an IMF vortices were generated near dawn where the corotating flows and solar wind are opposite. For BZ 0 vortices were generated in the morning and evening where the flows from tail reconnection are opposite to the solar wind and corotation. We used the energy flux to the ionosphere and upward field‐aligned currents (FACs) as proxies for diffuse and discrete aurora. Strong upward FACs extend to the morning sector when BZ > 0. The strongest FACs are generated in the flow vortices.