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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Model-Based Assessments of Magnetic Reconnection and Kelvin-Helmholtz Instability at Jupiter's Magnetopause
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Model-Based Assessments of Magnetic Reconnection and Kelvin-Helmholtz Instability at Jupiter's Magnetopause

机译：基于模型的磁场重联的评估并在木星的Kelvin-Helmholtz不稳定磁层

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摘要

The interaction between the solar wind and Jupiter's magnetic field confines the planetary field to the largest magnetosphere in the Solar System. However, the full picture of when and where key processes operate at the magnetopause boundary of the system remains unclear. This is essential for testing understanding with observations and for determining the relative importance of different drivers of Jovian magnetospheric dynamics. Here we present a global analytical model of Jovian magnetopause conditions under steady state, which forms the basis of boundary process assessments. Sites of magnetic reconnection at Jupiter's magnetopause are expected to be in regions of sufficiently high magnetic shear across the boundary, controlled by the orientation of the interplanetary magnetic field. Reconnection rates are also most sensitive to changes in the highly variable IMF, followed by changes in the solar wind plasma mass density. The largest plasma flow shear across the boundary is in the equatorial dawn region, producing a region that is typically unstable to growth of the Kelvin-Helmholtz (K-H) instability. Compared to magnetopause reconnection site locations, this K-H-unstable region at dawn is less sensitive to changing conditions. Motion of K-H boundary perturbations typically includes dawn-to-dusk motion across the subsolar region. Model-predicted reconnection voltages are typically hundreds of kV but rely on steady solar wind conditions on a time scale that is longer than typical at Jupiter's orbit. How the reconnection voltage compares to the voltage applied due to the "viscous-like" interaction involving K-H instability remains unclear.
机译：太阳能风能和之间的交互木星的行星磁场范围最大的磁气圈太阳能领域系统。在磁层在关键过程操作吗系统的边界仍不清楚。对于测试的理解观察和确定的相对不同的威风凛凛的司机的重要性磁性层的动态。木星的磁层的分析模型稳态条件,形成了边界过程评估的基础。在木星的磁层磁场重联地区预计将足够吗高磁剪切边界,由的方向控制行星际磁场。也在高度变化最敏感变量国际货币基金组织(IMF),紧随其后的是太阳能的变化风等离子体质量密度。在赤道的边界剪切黎明的地区,通常是生产区域不稳定增长的Kelvin-Helmholtz (k - h)不稳定。重新连接站点位置,这K-H-unstable地区在黎明时分不太敏感的变化条件。通常包括在黎明到黄昏运动热带的地区。电压通常是几百千伏但依赖稳定的太阳风条件在时间范围内比典型的长在木星的轨道。重新连接电压与电压进行比较由于“viscous-like”互动应用包括k - h不稳定性仍不清楚。

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