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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >The Influence of Magnetic Field Topology and Orientation on the Distribution of Thermal Electrons in the Martian Magnetotail
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The Influence of Magnetic Field Topology and Orientation on the Distribution of Thermal Electrons in the Martian Magnetotail

机译：拓扑和磁场的影响取向分布的热电子在火星磁尾

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摘要

Thermal (<1 eV) electron density measurements, derived from the Mars Atmosphere and Volatile Evolution's (MAVEN) Langmuir Probe and Waves (LPW) instrument, are analyzed to produce the first statistical study of the thermal electron population in the Martian magnetotail. Coincident measurements of the local magnetic field are used to demonstrate that close to Mars, the thermal electron population is most likely to be observed at a cylindrical distance of ~1.1 Mars radii (R_M) from the central tail region during times when the magnetic field flares inward toward the central tail, compared to ~1.3 RM during times when the magnetic field flares outward away from the central tail. Similar patterns are observed further down the magnetotail with greater variability. Thermal electron densities are highly variable throughout the magnetotail; average densities are typically ~20–50 cm-3 within the optical shadow of Mars and can peak at ~100 cm-3 just outside of the optical shadow. Standard deviations of 100% are observed for average densities measured throughout the tail. Analysis of the local magnetic field topology suggests that thermal electrons observed within the optical shadow of Mars are likely sourced from the nightside ionosphere, whereas electrons observed just outside of the optical shadow are likely sourced from the dayside ionosphere. Finally, thermal electrons within the optical shadow of Mars are up to 20% more likely to be observed when the strongest crustal magnetic fields point sunward than when they point tailward.
机译：热(< 1 eV)电子密度测量,来自火星大气与挥发物进化的(MAVEN)朗缪尔探针和波(LPW)仪器,分析了生产第一次统计的研究热电子人口在火星磁尾。当地磁场的测量证明接近火星,热电子人口是最容易被观察到在一个圆柱形的距离~ 1.1火星半径(R_M)时尾巴中部地区当磁场耀斑向内朝中央的尾巴,而~ 1.3 RM时期当磁场耀斑向外远离中央的尾巴。在磁尾更大可变性。高度可变整个磁尾;平均密度通常~ 20 - 50 cm-3在火星的光的影子,可以达到~ 100 cm-3外光的影子。标准偏差的100%是观察平均密度测量在整个尾巴。当地磁场拓扑结构的分析表明热电子中观察到火星有可能采购的光的影子从阴面电离层,而电子观察到外面的光的影子可能来自的光面电离层。最后,热内的电子光学火星的影子更可能是20%当地壳磁场最强的点比当他们朝着太阳点tailward。

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