月面高温下推力器可靠性试验

嫦娥五号着陆上升组合体落月后将经历月昼强红外辐射环境，由于推力器喷管导热影响，使推进剂管路与电磁阀面临高温环境，推进系统存在管路内氧化剂汽化和推力器性能下降甚至无法正常工作的问题，影响上升器月面起飞正常姿态控制。为了研究高温下推力器的工作性能，进行了高温下氟塑料阀芯与氧化剂相容性调研，提出了电磁阀和推力器可靠性增长及可靠性验证试验方法，分析了温度与电磁阀阀芯行程的关系，获取了高温环境下推力器的稳态及脉冲工作性能，在小子样条件下评估了推力器可靠性置信下限及月面起飞上升推进系统可靠度，通过月面高温排气及月面起飞上升姿态控制对研究结果进行了航天器在轨飞行验证，圆满完成了上升器月面起飞上升任务。所提出的研究方法及思路具有很好的工程适用性。     

Implication of multiple dipolarization event near 9 RE for the physics of substorms

In 2001, 2002 and 2003, the Polar spacecraft probed the near equatorial plasma sheet at 9 R_E near local midnight. Using the magnetic field observations, the signatures at substorm onsets are studied. Close to the flux pile-up region, the Polar spacecraft readily detects the dipolarization front, especially for pseudo onsets. An event with two distinct onsets has been examined. The signatures are found to be consistent with the multiple-onset model suggested by Russell [Russell, C.T. How northward turnings of the IMF can lead to substorm expansion onsets. Geophys. Res. Lett. 27, 3257–3259, 2000] which is a modified Near-Earth Neutral Line (NENL) model. Another similar event is also examined showing the effects of different Interplanetary Magnetic Field (IMF) conditions upon substorms. Moreover, ground effects can be very weak compared to in situ observations, especially for pseudo onsets, because these signatures appear to be localized and not global.     

The evolution of mirror type magnetic fluctuations in the magnetosheath based on multipoint observations

Two orbits were selected in January–February 2006 when the separation between the Cluster spacecraft was large and mirror type magnetic field fluctuations were observed by all spacecraft in different regions of the terrestrial magnetosheath. Minimum variance analysis was applied to find the mirror type fluctuations, and the amplitude of the fluctuations was determined individually. Mirror mode structures are moving along the streamlines frozen in the plasma. A model was developed for the calculation of plasma flowtime from the bow shock to the observation point. The growth rate of the field strength perturbations was estimated by comparing the amplitudes of fluctuations observed simultaneously at distant locations (∼10,000 km) based on the assumption that δB ∼ exp(γt). The obtained growth rate values were about an order of magnitude smaller than those provided by linear models and they decreased in the inner regions of the magnetosheath, indicating some saturation in the growth of the waves when proceeding towards the magnetopause. The results of these two case studies suggest that mirror type fluctuations originate from the compression region downstream of the quasi-perpendicular bow shock, and the growth of the fluctuations cannot be described by linear approximations.     

Plasma and electromagnetic wave simulations of meteors

Every day billions of meteoroids impact and disintegrate in the Earth’s atmosphere. Current estimates for this global meteor flux vary from 2000 to 200,000 tons per year, and estimates for the average velocity range between 10 km/s and 70 km/s. The basic properties of this global meteor flux, such as the average mass, velocity, and chemical composition remain poorly constrained. We believe much of the mystery surrounding the basic parameters of the interplanetary meteor flux exists for the following reason, the unknown sampling characteristics of different radar meteor observation techniques, which are used to derive or constrain most models. We believe this arises due to poorly understood radio scattering characteristics of the meteor plasma, especially in light of recent work showing that plasma turbulence and instability greatly influences meteor trail properties at every stage of evolution. We present our results on meteor plasmas simulations of head echoes using particle in cell (PIC) ions, which show that electric fields strongly influence early stage meteor plasma evolution, by accelerating ions away from the meteoroid body. We also present the results of finite difference time domain electromagnetic simulations (FDTD), which can calculate the radar cross section of the simulated meteor plasmas. These simulations have shown that the radar cross section depends in a complex manner on a number of parameters. These include the angle between radar and meteor entry, a large dependence on radar frequency, which shows that for a given meteor plasma size and density, the reflectivity as a function of probing radar frequency varies, but typically peaks below 100 MHz.     

稳态等离子体推进器羽流场数值模拟

采用二维轴对称模型,使用粒子网格法(PIC)和直接模拟蒙特卡洛法(DSMC)相结合的方法,对稳态等离子体推进器(SPT)羽流场进行了数值模拟.采用DSMC方法中的随机取样频率法(RSF)求解粒子碰撞过程,并对比了不同的分配电荷方式、电子运动模型及SPT出口条件时的羽流场.将不同条件计算得到的羽流场中距SPT出口0.1?m,0.5?m及1.0?m处的离子电流密度和电荷密度与实验结果进行了对比,得出在采用面积权重法分配电荷、等熵模型描述电子运动和用实验值设定发动机出口参数时对SPT羽流场数值模拟的电流密度和轴向附近的电荷密度结果与实验结果符合程度较好的结论.     

面向深空探测的30cm离子推力器寿命预估

为评价30cm离子推力器的寿命,提出了有限寿命考核结合栅极仿真模型的推力器寿命预估方法,利用粒子-蒙特卡洛（PIC-MCC）方法建立了栅孔溅射腐蚀模型,开展了30cm离子推力器寿命预估研究,分析了栅孔刻蚀速率、单孔电场及离子引出特性,给出了30cm推力器寿命预估值。结果表明,栅孔直径仿真与实测值一致性较好,误差在20%以内,基于每个寿命小节栅孔实测值对模型的修正是有效的;根据仿真结果,10000h寿命考核后,减速栅最先失效,30cm离子推力器在最大功率（3kW）工况下预估寿命为37540h,能够满足小天体探测任务对电推进系统的长寿命需求。     

固体推进剂等离子体点火研究

为了研究等离子体对固体推进剂点火性能的影响，分别对双基药和硝胺药等两种固体推进剂，进行了等离子体点火实验。实验装置包括等离子体源、热电偶丝和动态信号分析仪。通过实验，获得了两种固体推进剂在不同的等离子体能量输入的条件下，其表面温度随时间变化的曲线。与常规点火数据相比，固体推进剂的等离子体点火延迟时间明显缩短。不同类型的固体推进剂，在相同的等离子体能量输入条件下，其点火性能不同；同一种类型的固体推进剂，在不同的等离子体能量输入条件下，其点火性能也不一样。     

Langmuir双探针测量Hall推力器羽流特性

应用Langmu ir双探针测量了距离Hall推力器出口30~100 cm的羽流特性。实验中真空舱压力保持在5×10-4~2×10-3Pa之间。实验证明,电子温度和数密度随着角度和轴向距离的变化而变化,但羽流中远场的电子温度变化幅度很小,基本稳定在0.455 eV左右;电子数密度随着与轴向距离和中心轴夹角的增加而减小。实验结果可为高性能的Hall推力器设计提供参考依据,并为等离子体羽流的数值模拟提供输入条件和验证依据。     

低轨航天器致空间等离子体尾流

建立起一个低轨道航天器引起的等离子体尾的二维计算机模式，结果表明：（１）尾流的宽度随表面负电位值的增加而变窄。（２）随离子马赫数增加尾流位垒变宽；（３）对正电位表面情况尾流近区有电子聚集，并且离子的放空更远。