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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Effects of finite plasma pressure on centrifugally driven convection in Saturn's inner magnetosphere
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Effects of finite plasma pressure on centrifugally driven convection in Saturn's inner magnetosphere

机译：的影响有限等离子体离心地压力驱动在土星磁层内部的对流

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[1] We have previously shown simulation results for centrifugally driven plasma convection in Saturn's inner magnetosphere (2 < L < 12) using the Rice Convection Model, including a continuously active distributed plasma source, and the effects of the Coriolis force and the pickup current. These simulations result in a quasi-steady state, in which fast, narrow inflow channels alternate with slower, wider outflow channels, consistent with Cassini Plasma Spectrometer observations. These previous simulations, however, did not include the plasma pressure. We investigate here the effects of finite plasma pressure and the associated gradient-curvature drift current by giving the cold plasma a finite temperature. Our simulations confirm the theoretical expectation that a finite plasma pressure produces a force in the positive radial direction, the same direction as the centrifugal force, and acts as an additional driver of plasma convection. Our simulations also confirm that the radial velocities can be reduced(to keep them within observational constraints)by increasing the assumed ionospheric Pedersen conductance(also within observational constraints).
机译：[1]我们以前显示仿真结果对离心地驱动等离子体对流土星的内部磁气圈(2 < L < 12)使用大米对流模型,包括一个分布的等离子体源不断活跃,和科里奥利力的影响小电流。准稳态,快,狭窄的流入渠道相间更慢,更广泛的流出渠道,与卡西尼等离子体一致光谱仪观测。模拟,然而,不包括等离子体压力。有限的等离子体和相关的压力通过给gradient-curvature漂流冷等离子体有限温度。确认一个有限的理论预期等离子体压力产生一种积极的力量径向方向,相同的方向离心力和作为一个额外的司机的等离子体对流。确认径向速度减少(让他们在观察约束)通过增加假定电离层皮德森电导(还在观察约束)。

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