原子氧对红外干扰材料消光性能的影响研究

为探索大气中的红外干扰材料可否应用于外层空间, 利用原子氧效应地面模拟装置对铜粉和石墨粉两种红外干扰材料样品进行了原子氧暴露实验, 并对样品进行了质量分析、XRD分析和红外透过率测试. 结果表明, 原子氧累积通量达到5.0×1019cm-2时, 铜粉样品质量增加0.004mg•cm-2,石墨粉样品质量损失0.117mg•cm-2; 原子氧暴露后, 铜粉对3~5μm与8~12μm红外质量消光系数由3.64 m2•g-1与2.74 m2•g-1变为3.14 m2•g-1与2.65 m2•g-1, 消光能力降低; 石墨粉对3~5μm和8~12μm红外的质量消光系数由6.54 m2•g-1和5.78 m2•g-1减小为2.38 m2•g-1和2.27 m2•g-1, 消光能力明显减弱.      

GEO螺旋巡游轨道的相对运动分析和螺旋环设计

摘要： GEO螺旋巡游轨道采用螺旋巡游方式,以不同的构型“上下浮动”在GEO轨道附近,可实现对该轨道上空间目标和空间环境的高精度探测.本文在分析GEO轨道航天器运动规律的基础上,应用小偏差理论分析螺旋巡游轨道与GEO目标之间的相对运动,给出平面螺旋环和三维螺旋环的设计方法,为GEO螺旋巡游轨道的设计奠定基础.     

双臂空间机器人姿态调整运动的最优控制规划

讨论了双臂空间机器人系统姿态调整运动的最优控制规划问题.以多体动力学理论为基础,导出了载体位置、姿态均不受控制情况下,双臂空间机器人系统的动量矩守恒关系,并将其转化为系统状态方程;利用近似优化方法给出了一种双臂空间机器人姿态、关节协调运动的最优控制算法.其优点在于,仅控制双臂空间机器人的关节运动,即可同时获得载体姿态及机械臂关节需要的终端位置.系统数值仿真,证实了算法的有效性.     

相邻两航天器相对运动近似方程的解析解及比动能方程

给出了地心引力场中受控航天器相对目标航天器运动的推力加速度随时间线性变化时Hill方程的解析解，根据Hill方程导出了受控航天器相对目标航天器运动的比动能方程，并讨论了比动能方程在上述两天器轨道相遇和轨道交会问题中的应用。     

基于自适应搜索的快速运动估计算法

在MPEG和H.263的运动估计中,全搜索(FS)效果虽好但时间开销巨大,以三步搜索法为代表的一些快速算法不仅在搜索精度方面与FS相比有较大的差距,而且搜索时间仍不能满足实际的需要.提出的基于自适应搜索的快速运动估计算法(ASA)充分利用了视频序列运动矢量在空间分布上的中心偏置特性和相邻块运动的相关性,在大幅度提高搜索效率的情况下,得到了与全搜索非常接近的搜索效果.与现有算法相比,该算法具有高效、鲁棒性强的特点.      

基于目标性权值度量的多示例学习目标跟踪

针对多示例学习(MIL)跟踪算法在包概率计算过程中对示例样本不加以区分导致分类器性能下降,及采用最大化似然函数选择相应的弱分类构造强分类增加了算法复杂度的问题,提出了一种基于目标性权值学习的多示例目标跟踪算法,该算法利用目标性测量每个示例样本对包概率的重要性,根据其目标性测量结果对每个正示例样本赋予相应的权值,从而判别性地计算包概率,提高跟踪精度。同时在弱分类器选择过程中,采用最大化弱分类器与似然函数概率内积的方法从弱分类器池中选择弱分器构造强分类器,减少算法的计算复杂度。通过对不同复杂场景下视频序列的跟踪,实验结果表明,本文所提出的目标性权值学习的多示例目标跟踪算法优于其对比算法,表现出较好的跟踪精度和鲁棒性能。     

直线电机定位平台的摩擦建模与补偿

介绍了一种由双边直线电机驱动的H型精密定位平台,为了减小运动平台的速度跟随误差和定位误差,研究了该精密定位系统的摩擦建模和补偿问题.由于工作台的滑块在导轨的不同位置表现出不同的摩擦特性,为改善补偿效果,提出了一种基于经典Stribeck摩擦力模型和工作台运动副位置参数的摩擦建模新方法,通过实验和回归的方法辨识出了工作台双边导轨的改进型Stribeck摩擦模型.基于建立的摩擦模型,采用前馈技术进行摩擦力补偿控制.实验结果表明,基于模型的摩擦补偿提高了系统的控制性能;改进型Stribeck摩擦模型比传统Stribeck摩擦模型有更好的补偿效果,适合具有大行程工作台的摩擦建模与补偿.      

Prospects in the orbital and rotational dynamics of the Moon with the advent of sub-centimeter lunar laser ranging

Lunar laser ranging (LLR) measurements are crucial for advanced exploration of the laws of fundamental gravitational physics and geophysics as well as for future human and robotic missions to the Moon. The corner-cube reflectors (CCR) currently on the Moon require no power and still work perfectly since their installation during the project Apollo era. Current LLR technology allows us to measure distances to the Moon with a precision approaching 1 mm. As NASA pursues the vision of taking humans back to the Moon, new, more precise laser ranging applications will be demanded, including continuous tracking from more sites on Earth, placing new CCR arrays on the Moon, and possibly installing other devices such as transponders, etc. for multiple scientific and technical purposes. Since this effort involves humans in space, then in all situations the accuracy, fidelity, and robustness of the measurements, their adequate interpretation, and any products based on them, are of utmost importance. Successful achievement of this goal strongly demands further significant improvement of the theoretical model of the orbital and rotational dynamics of the Earth–Moon system. This model should inevitably be based on the theory of general relativity, fully incorporate the relevant geophysical processes, lunar librations, tides, and should rely upon the most recent standards and recommendations of the IAU for data analysis. This paper discusses methods and problems in developing such a mathematical model. The model will take into account all the classical and relativistic effects in the orbital and rotational motion of the Moon and Earth at the sub-centimeter level. The model is supposed to be implemented as a part of the computer code underlying NASA Goddard’s orbital analysis and geophysical parameter estimation package GEODYN and the ephemeris package PMOE 2003 of the Purple Mountain Observatory. The new model will allow us to navigate a spacecraft precisely to a location on the Moon. It will also greatly improve our understanding of the structure of the lunar interior and the nature of the physical interaction at the core–mantle interface layer. The new theory and upcoming millimeter LLR will give us the means to perform one of the most precise fundamental tests of general relativity in the solar system.     

Study of correlations between waves and particle fluxes measured on board the DEMETER satellite

The topic of relativistic electron dynamics in the outer radiation belt has received considerable attention for many years. Nevertheless, the problem of understanding the physical phenomenon involved is far from being resolved. In this paper, we use DEMETER observations to examine the variations of the energetic electron fluxes and ELF/VLF wave intensities in the inner magnetosphere during the intense 8 November 2004 magnetic storm. Electron flux spectra and associated wave intensity spectra are analysed throughout the magnetic storm and common characteristics or differences to other storm events are retained. The overall objective of this study is to identify and derive parameters that are relevant for particle flux modelling; the time constant characterizing the persistent decay after particle enhancement was found to be one of these important model parameters.The analysis of the 8 November 2004 event reveals that for L-shell parameter higher than 4, an electron flux dropout is observed during the storm’s main phase for electrons in the energy range 0.1–1 MeV, as has been reported from other measurements. Characteristic wave spectra accompanying this phase are analysed. They show a typical enhancement in the frequency range 0.3–10 kHz at onset for all L-shell values under consideration (2 < L < 5). During the first stage of the recovery phase, the electron fluxes are increased to a level higher than the pre-storm level, whereas the level of wave intensity in the frequency range observed below 300 Hz is at its highest. In the second stage, the particle flux decrease goes hand in hand with a global wave activity decline, the relaxation time of the latter being smaller than the former’s one. In some other cases, long-lasting electron enhancement associated with constant wave activity has been observed during this latter stage. For the above mentioned storm, while at low L values the decay time constants are higher for low energy electrons than for high energy electrons, this order is reversed at high L values. At about L = 3.6 the time constant is independent of electron energy.