HAN基电控固体推进剂电热耦合特性及燃烧特性实验研究

为了探究HAN基电控固体推进剂(ECSP)的电热耦合特性和燃烧性能,通过改变施加电压和环境压力对ECSP进行燃烧性能测试。在ECSP燃烧性能测试装置中采用电压、电流探头记录燃烧过程中通过推进剂的电压和电流,利用高速摄影仪记录推进剂的燃烧过程,借助法拉第电化学分解定律计算推进剂理论电化学分解质量在总燃烧消耗质量中的占比,分析电压和压力对推进剂燃速和质量损失的影响,同时拟合出ECSP燃速(r)与功率(P₁)和压力(P₂)的经验公式。结果表明：随着电压和压力的增加,ECSP理论电化学分解质量和实际燃烧质量增加,理论/总燃烧质量比值降低,燃速和质量损失增加。在ECSP的可控燃烧范围内,其燃速与功率和压力满足r = 0.0105P_1^0.705P_2^0.251。本文得到了热分解反应在ECSP的燃烧过程中占主导地位,是高压力下造成推进剂不可控燃烧的主要原因,为揭示ECSP的燃烧可控机理提供理论基础。     

A new parameter to define interplanetary coronal mass ejections

The interplanetary manifestations of coronal mass ejections, ICMEs, have many signatures in the solar wind but none of these signatures in the velocity, density, temperature, magnetic field, plasma composition or energetic particles uniquely and unambiguously identifies the occurrence of an ICME. Different investigators identify different events when confronted with the same data. Herein, we present a single physical parameter that combines information from multiple plasma components and that holds the promise of defining a beginning and an end of the region of influence ICME and an indication of the location of the encounter with the ICME relative to its central meridian. This parameter is the total plasma pressure perpendicular to the magnetic field, consisting of the sum of the magnetic pressure and plasma kinetic or thermal pressure. It provides a vehicle for classifying the nature of the ICME encounter and, in many cases, provides an unambiguous start and stop time of the event. However, it does not provide a start and stop time for any embedded flux rope. This identification depends on examination of the magnetic field.     

Evolution of coronal mass ejections in the early stage

This work reports the investigation of two coronal mass ejections (CME) observed in white light, H, EUV and X-ray by various instruments both in space and on ground on February 18, 2003 and January 19, 2005, respectively. The white light coronal images show that the first CME began with the rarefaction of a region above the solar limb and was followed by the formation of its leading edge at the boundary of the rarefying region at altitude of 0.46 R from the solar surface. The rarefaction coincided the slow rising phase of the filament eruption, and the CME leading edge was observed to form as the filament eruption started to accelerate apparently. In the early stage of the second CME, a bright loop was first observed above the solar limb with height of 0.37 R in EUV images. We found that the more gradual CMEs initial process, the larger the timing difference between CMEs and their associated flares. The lower part of the filament brightened in H images as the filament rose to a certain height. These brightenings imply that the filament may be heated by magnetic reconnection below the filament in the early stage of the eruption. We suggest that the possible mechanism which led to the formation of the CME leading edge and cavity is magnetic reconnection which occurred under the filament when it reached a certain height.     

Force-free magnetic field in a cylindrical flux rope without a constant alpha

It is generally assumed that magnetic fields inside interplanetary magnetic clouds and flux ropes in the solar photosphere are force-free. In order to model such fields, the solution of rot B = B is commonly used where  = const. But comparisons of this solutions with observations show significant difference. To treat this problem,we examine the solutions with .     

Solar Elemental Composition Based on Studies of Solar Energetic Particles

Solar abundances can be derived from the composition of the solar wind and solar energetic particles (SEPs) as well as obtained through spectroscopic means. Past comparisons have suggested that all three samples agree well, when rigidity-related fractionation effects on the SEPs were accounted for. It has been known that such effects vary from one event to the next and should be addressed on an event-by-event basis. This paper examines event variability more closely, particularly in terms of energy-dependent SEP abundances. This is now possible using detailed SEP measurements spanning several decades in energy from the Ultra Low Energy Isotope Spectrometer (ULEIS) and the Solar Isotope Spectrometer (SIS) on the ACE spacecraft. We present examples of the variability of the elemental composition with energy and suggest they can be understood in terms of diffusion from the acceleration region near the interplanetary shock. By means of a spectral scaling procedure, we obtain energy-independent abundance ratios for 14 large SEP events and compare them to reported solar wind and coronal abundances as well as to previous surveys of SEP events.     

乙烯基硅橡胶生胶中低分子的脱除

由于硅橡胶是用催化平衡的方法制备，生胶中含有约3％的挥发性的低分子量环体，会对硅橡胶的热真空失重（TML）、可凝挥发物性能（CVCM）有极大影响。为使所制得的硅橡胶符合空间级材料要求，分别采用溶剂抽提法和热真空处理法来脱除乙烯基硅橡胶中的小分子，通过比较处理前后硅橡胶的分子量及其分布、TML、CVCM，对比了两种方法脱除小分子的效果；并制备得到了符合空间级标准的硅橡胶。     

军用飞机大修过程质量控制方法研究

结合飞机大修的常规流程,分析了各阶段产生的故障信息,从全面质量管理理念出发选取监控点,研究了故障数据分析方法,并利用C控制图实现了在不同维修工序后对大修飞机质量特性波动的定量认识、评估、处理和监控,保证了军用飞机大修后的安全性和可靠性。     

Direct thrust test and asymmetric performance of porous ionic liquid electrospray thruster

In order to meet the demand of CubeSats for low power and high-performance micro-propulsion system, a porous ionic liquid electrospray thruster prototype is developed in this study. 10 × 10 conical emitter arrays are fabricated on an area of 3.24 cm² by computer numerical control machining technology. The propellant is 1-ethyl-3-methylimidazolium tetrafluoroborate. The overall dimension of the assembled prototype is 3 cm × 3 cm × 1 cm, with a total weight of about 15 g (with propellant). The performance of this prototype is tested under vacuum. The results show that it can work in the voltage range of ±2.0 kV to ±3.0 kV, and the maximum emission current and input power are about 355 μA and 1.12 W. Time of Flight (TOF) mass spectrometry results show that cationic monomers and dimers dominate the beam in positive mode, while a higher proportion of higher-order solvated ion clusters in negative mode. The maximum specific impulse is 2992 s in positive mode and 849 s in negative mode. The thrust is measured in two methods: one is calculated by TOF results and the other is directly measured by high-precision torsional thrust stand. The thrust (T) obtained by these two methods conforms to a certain scaling law with respect to the emission current (I_em) and the applied voltage (V_app), following the scale of T ∼ I_emV_app^0.5, and the thrust range is from 2.1 μN to 42.6 μN. Many thruster performance parameters are significantly different in positive and negative modes. We speculate that due to the higher solvation energy of the anion, more solvated ion clusters are formed rather than pure ions under the same electric field. It may help to improve thruster performance if porous materials with smaller pore sizes are used as reservoirs. Although there are still many problems, most of the performance parameters of ILET-3 are good, which can theoretically meet the requirements of CubeSats for micro-propulsion system.     

导弹质量特性测量装置设计

设计了一种导弹质量、质心、转动惯量一体化测量设备，可在同一台设备设计上完成导弹质量、轴向和径向质心、俯仰偏航方向的转动惯量测量。该装置主要由测试平台、活动支架、沿导弹纵轴滑动的精确定位机构、三个测力传感器和一个倒扭摆机构组成。了该装置质量特性测量方法，定量分析了测量误差，并总结了此类装置设计的几个关键问题。     

虚拟仪器技术在发动机质心测量中的应用

研究了虚拟仪器技术在发动机质心测量中的应用，建立了电测系统的误差模型，对电测系统的误差进行校正，最终测试结果表明整个测量系统的测量精度得到了提高。