利用超高速碰撞引起的PSP和MAVEN电场天线信号探测宇宙尘埃

宇宙尘埃携带有关于星系演化、恒星行星系统形成乃至生命起源的重要信息，同时也威胁着航天器的安全。宇宙尘埃与航天器的超高速碰撞会产生快速扩张的等离子体云，扰动航天器电势并产生电场天线信号。利用电场天线探测宇宙尘埃已经在空间探测任务中得到了广泛应用，研究尘埃超高速碰撞产生的电场天线信号可以用来量化空间尘埃环境以及尘埃碰撞风险，具有十分重要的科学意义。

本文通过分析Parker Solar Probe（PSP）号航天器在全新环境中的尘埃观测数据，进一步探究尘埃碰撞信号的产生机制。研究发现，单、偶极电场天线对碰撞位置的响应存在差异，可通过分析不同天线信号的特征确定尘埃碰撞发生位置以及等离子体云扩散的方向。飞船电势通过影响碰撞等离子体云中粒子的扩散，进而影响尘埃碰撞信号的形态。统计得到太阳附近尘埃的空间分布特征，总体来说，尘埃碰撞率呈现出随距太阳中心距离减小而增加的趋势。此外，PSP在不同轨道近日点附近观测到的尘埃碰撞率变化趋势存在差异。

其次，本文基于波形互相关的方法对Mars Atmosphere and Volatile EvolutioN（MAVEN）号航天器2020年观测到的尘埃碰撞信号进行识别，得到火星附近尘埃的空间分布特征。统计结果显示，在同一纬度区间，北半球的尘埃碰撞率水平普遍比南半球高，这种差异在10^°~50^° 的中纬度地区表现最为明显。尘埃碰撞计数和尘埃碰撞率均未在火星赤道平面附近呈现出很强的分布，表明火星卫星环尘埃不是MAVEN观测的主要尘埃源。此外，尘埃碰撞主要集中分布在日侧低高度地区，且昏侧的碰撞率高于晨侧。受火星大气等离子体密度和飞船电势影响，尘埃碰撞率水平呈现出随高度降低而升高的变化趋势。

Cosmic dust carries important information about the evolution of galaxies, the formation of stellar and planetary systems and even the origin of life. At the same time, it also threatens the safety of spacecraft. Hypervelocity impacts between cosmic dust and spacecraft will produce rapidly expanding plasma cloud, which will disturb the spacecraft potential and generate signals detected by electric field antennas. Dust detection by electric field antennas has been widely used in space exploration missions. These electric field antenna signals generated by dust hypervelocity impacts can help quantify the dust environment and dust impact risk in space, which is of great scientific significance.

This thesis analyzes the dust observation data of the Parker Solar Probe（PSP）in a new environment to further explore the generation mechanism of dust impact signals. It is found that the monopole and dipole electric field antennas show differences in their response to impact position, and the dust impact location and the plasma cloud expanding direction can be determined by analyzing the signal characteristics of different antennas. The spacecraft potential can affect the morphology of the impact signals by controlling the particle diffusion in the expanding impact plasma cloud. The spatial distribution of the dust near the sun is statistically characterized. By and large, the dust impact rate increases with decreasing distance from the center of the sun. In addition, the dust impact rate profile observed by PSP near perihelion varies in different orbits.

Secondly, based on the waveform cross-correlation method, this thesis identifies the dust impact signals observed by the Mars Atmosphere and Volatile EvolutioN（MAVEN）in 2020, and obtains the spatial distribution characteristics of dust near Mars. Statistical results show that in the same latitude range, the dust impact rate in the northern hemisphere is generally higher than that in the southern hemisphere, and the difference is most obvious in the mid-latitude region of 10^°~50^°. Neither the dust impact counts nor the impact rate shows a strong distribution near the Martian equatorial plane, suggesting that Mars satellite ring dust is not the main source for MAVEN observations. Moreover, dust impacts are mainly concentrated in the low altitude area on the day side, and the impact rate is higher on the dusk side than the dawn side. Influenced by the Martian atmospheric plasma density and spacecraft potential, the dust impact rate shows a trend of increasing with the decrease of altitude.

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