Solar Plasma Electrostatic Analyzer

A hemispherical electrostatic analyzer was used to study the directional intensity of positive ions and electrons in the solar wind, magnetosheath, and magnetotail. Ions as heavy as oxygen were resolved when the solar wind temperature was low. Energy analysis was accomplished by charging the plates to known voltage levels and allowing them to discharge with known RC time constants. In the solar wind, positive ions from 200 eV to 5 keV (15% spacing, 3% resolution) and electrons from 5 eV to 1 keV (30% spacing, 15% resolution) were studied. In the magnetosheath, positive ions from 200 eV to 5 keV (15% spacing, 3% resolution) and from 200 eV to 2 keV (30% spacing, 15% resolution) and electrons from 5 eV to 1 keV (30% spacing, 15% resolution) were studied. In the magnetotail, positive ions from 200 eV to 20 keV (30% spacing, 15% resolution) and electrons from 5 eV to 1 keV (30% spacing, 15% resolution) and from 100 eV to 20 keV (15% resolution) were studied. For further details see W. C. Feldman et al., J. Geophys. Res., v. 80, p. 4181, 1975.

本研究采用半球形静电分析仪对太阳风、磁层和磁尾中的正离子和电子的方向强度进行了研究。当太阳风温度较低时，能够解析出如氧离子般重质的离子。通过将电极充电至已知电压水平并使其以已知的RC时间常数放电，实现了能量的分析。在太阳风中，对200 eV至5 keV（15%间隔，3%分辨率）的正离子和5 eV至1 keV（30%间隔，15%分辨率）的电子进行了研究。在磁层中，研究了200 eV至5 keV（15%间隔，3%分辨率）以及200 eV至2 keV（30%间隔，15%分辨率）的正离子，以及5 eV至1 keV（30%间隔，15%分辨率）的电子。在磁尾中，研究了200 eV至20 keV（30%间隔，15%分辨率）的正离子，以及5 eV至1 keV（30%间隔，15%分辨率）和100 eV至20 keV（15%分辨率）的电子。详情请参阅W. C. Feldman等人发表的《地球物理学研究杂志》，第80卷，第4181页，1975年。