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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Electron density images of the middle- and high-latitude magnetosphere in response to the solar wind
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Electron density images of the middle- and high-latitude magnetosphere in response to the solar wind

机译：电子密度的图像中高纬度地区的磁气圈太阳风

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Electron density distributions and plasma dynamics in the middle- and high-latitude dayside magnetosphere are studied with observations from the IMAGE radio plasma imager. Remote measurements of the electron densities along magnetic field lines were made before and during a magnetic storm when the solar wind and interplanetary magnetic field (IMF) impinging on the magnetopause varied considerably. Several regions of different density distribution characteristics, including plasmasphere, plasma trough, subauroral/auroral density depletion, density enhancements in the aurora/cusp, and polar cap, are identified in “two-dimensional images,” i.e., along the satellite orbit and field lines. The plasma dynamics, such as the plasma refilling in the outer plasmasphere and the plasma acceleration in the aurora/cusp region, are inferred from density gradients along the field lines. It is shown that the densities and locations of the plasma regions vary in accordance with the solar wind, particularly with the IMF variations for the case examined. In the partial recovery phase of the magnetic storm when the IMF was northward, the density depletion region expanded to wider latitude range and extended to lower altitudes, with much lower densities than those in the density depletion regions of the other RPI measurement periods. The density enhancements associated with the aurora/cusp region were not visible, possibly because of the diffusive nature of the dayside aurora and higher-latitude location of the cusp during this period. At the peak of the storm, characterized by a persistent southward IMF B_z , all plasma regions moved to lower L shells. The results imply that the solar wind/IMF effects should be included in any statistical study of the electron density distributions in these regions.
机译：电子密度分布和等离子体动力学在中高纬度地区的光面磁气圈的观测研究图像广播等离子体成像。测量电子的密度磁场线是由之前和期间当太阳风和磁性风暴行星际磁场(IMF)侵犯磁层大大不同。地区不同的密度分布特征,包括等离子体层,等离子体槽,subauroral /极光密度损耗,在极光/尖端密度增强,在“二维极地冰冠,确定图像”,即沿卫星轨道和电场线。填充外等离子体层和等离子体极光的等离子体加速/尖端地区,推断出从密度梯度电场线。和位置不同的等离子体区域根据太阳风,特别是国际货币基金组织变化的情况下检查。部分恢复阶段的磁暴国际货币基金组织(IMF)向北,密度减少地区扩展到更广泛的范围和纬度扩展到低海拔地区,低得多密度比密度损耗其他地区的零售物价指数测量时间。密度增强有关极光/尖端区域是不可见的,可能因为的光面的扩散性质极光和高纬度尖端的位置在这段时间。国际货币基金组织向南持续说是,所有等离子体区域转移到低L贝壳。结果表明,太阳风/国际货币基金组织(IMF)的影响应该被包括在统计的研究吗在这些电子密度分布地区。

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