月球风化层中静电荷形成与保持的机制
Mechanisms of Electrostatic Charge Formation and Retention in Lunar Regolith
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- Korea Advanced Institute of Science and Technology（韩国科学技术院）
- NASA Langley Research Center（美国国家航空航天局兰利研究中心）
- Imperial College London（伦敦帝国学院）
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中文总结 AI 辅助
该技术备忘录研究月球风化层中静电荷的形成与保持机制，提出以粒子分辨的有符号电荷分布为微观输入，结合宏观输运方程评估次表面电场和介电击穿风险，为月球极地探索提供关键依据。
中文摘要 AI 辅助
随着阿尔忒弥斯计划向月球南极和永久阴影区（PSRs）推进，理解月球充电对于保护宇航员、机器人系统、仪器和基础设施日益重要。持续的黑暗、低温、低风化层电导率和长的电荷弛豫时间可能允许高能粒子诱导的电荷在表面以下积累。本技术备忘录解决一个关键未解问题：静电电荷如何在月球风化层内产生、分离、保持和积累？现有模型预测，太阳高能粒子和银河宇宙射线可能产生接近介电击穿阈值的次表面电场，但入射粒子与宏观体积电荷源之间的微观联系仍不清楚。仅能量沉积并不能决定保持的电荷。入射粒子及其次级粒子可能停止、注入、背散射、透射、复合、被捕获或逃逸。因此，本备忘录将所需的微观输入定义为每单位深度和入射粒子的平均有符号保持电荷分布，按粒子种类和能量解析。结合入射通量和能量谱，该响应提供了深度相关的体积电荷源速率，可与电荷连续性、传导、介电弛豫和泊松方程耦合。关键不确定性包括矿物学、颗粒和孔隙几何形状、温度以及预先存在的电位对电荷保持的影响。需要粒子分辨建模和低温高真空辐照实验来约束这些过程，并评估次表面电场、介电击穿、尘埃输运、污染以及持续月球极地探索的电荷缓解要求。
英文摘要
As the Artemis program advances toward the lunar south pole and permanently shadowed regions (PSRs), understanding lunar charging is increasingly important for protecting astronauts, robotic systems, instruments, and infrastructure. Persistent darkness, cryogenic temperatures, low regolith conductivity, and long charge-relaxation times may allow energetic-particle-induced charge to accumulate beneath the surface. This Technical Memorandum addresses a key unresolved question: how is electrostatic charge generated, separated, retained, and accumulated within lunar regolith? Existing models predict that solar energetic particles and galactic cosmic rays may produce subsurface electric fields approaching dielectric breakdown thresholds, but the microscopic connection between incident particles and macroscopic volumetric charge sources remains unclear. Energy deposition alone does not determine retained charge. Incident particles and their secondary particles may stop, implant, backscatter, transmit, recombine, become trapped, or escape. This memorandum therefore defines the required microscopic input as the average signed retained-charge distribution per unit depth and incident particle, resolved by particle species and energy. Combined with incident flux and energy spectra, this response provides a depth-dependent volumetric charge-source rate that can be coupled with charge continuity, conduction, dielectric relaxation, and Poisson's equation. Key uncertainties include the effects of mineralogy, grain and pore geometry, temperature, and pre-existing potential on charge retention. Particle-resolved modeling and cryogenic high-vacuum irradiation experiments are needed to constrain these processes and assess subsurface electric fields, dielectric breakdown, dust transport, contamination, and charge-mitigation requirements for sustained lunar polar exploration.
