2009年1月5日廊坊OH气辉观测图像的谱分析

2009年1月5日在中国河北省廊坊市韩村镇(39.4°N,116.6°E)进行了中国首次中间层顶大气重力波成像观测实验,记录了近4 h的OH气辉辐射数据,给出了依据该数据计算所得的该时间段内廊坊韩村附近水平方向约185 km范围内的中间层顶OH气辉扰动的谱分析结果.所得到的传播方向确定的二维功率谱和角度谱揭示了该时间段内重力波活动的波长和传播方向分布特点,表明波长下限较短,西向传播分量明显大于东向分量.     

基于多目标遗传算法的太阳高纬探测器轨道设计

针对太阳高纬度探测器轨道设计任务要求, 研究了基于多目标遗传算法的小推力借力飞行轨道设计方法. 基于圆锥曲线拼接假设, 将探测器轨道分为小推力日心转移轨道段和木星借力飞行轨道段两部分. 在日心转移轨道段, 选择燃料最省为优化目标, 采用标称轨道法设计小推力的推力控制率. 在借力飞行轨道段, 选择借力后日心轨道倾角为优化目标, 对借力飞行的关键参数进行分析. 采用多目标遗传算法对该多目标进行了优化. 结果表明, 多目标遗传算法可以有效地解决轨道设计中的多目标优化问题. 优化得到的小推力控制率不仅可以节省发射能量, 还可以保证借力飞行后探测器能够进入太阳高纬度探测轨道.      

木星系探测及行星穿越任务轨迹初步设计

基于我国未来木星系探测任务需求,初步设计了任务轨迹。以目前的发射能力,要实现木星的环绕探测必将利用行星借力,需设计借力轨迹。首先将脉冲变轨的轨迹设计问题转化为参数优化问题,在满足2029—2032年间发射并且飞行时间不超过7年的约束条件下,使用PSO算法对发射时刻、借力时刻、深空机动时刻、到达时刻等参数进行优化,使得探测器需提供的总速度增量最小。探测器进入木星系后,利用木卫3借力捕获至环木大椭圆轨道,又利用木卫4构造共振借力,最终捕获至木卫4的环绕轨道。在此基础上,还考虑了天王星飞越的拓展任务,天王星探测器在到达木星时与木星系探测器分离,利用木星借力可无消耗飞往天王星,并在2043年完成天王星的飞越探测任务。     

不同重力环境下空间机械臂神经自适应鲁棒控制

针对空间机械臂从地面装调到空间应用过程中重力项的变化问题,提出了一种神经网络自适应鲁棒补偿控制策略用于空间机械臂的末端控制,从而实现在地面重力环境下装调好的空间机械臂在空间微重力环境下实现在轨操控任务。通过神经网络在线建模来逼近系统模型中变化的重力项,逼近误差及系统的不确定性通过自适应鲁棒控制器来补偿。该控制策略不依赖于系统的模型,避免了回归矩阵的复杂计算及未知参数的估计,降低了计算量。基于李亚普诺夫理论证明了闭环系统的渐近稳定性。仿真结果表明该控制器对不同重力环境下空间机械臂的末端控制均能达到较高的控制精度,具有重要的理论研究和工程应用价值。     

考虑重力影响的柔性关节空间机械臂任务空间神经网络控制

针对柔性关节空间机器人地面模拟及空间应用受到重力或微重力不确定项干扰的问题,提出一种基于奇异摄动的任务空间神经网络自适应控制算法。首先建立了考虑重力影响的柔性关节空间机器人的模型,通过奇异摄动方法将系统降阶处理后,转换到任务空间进行控制器的设计,利用神经网络自适应算法对系统的不确定性进行逼近,并针对逼近误差设计了鲁棒控制器补偿,最后将控制量转换为关节空间的控制力矩。对系统进行了稳定性分析和仿真校验,结果表明,控制器可以解决柔性带来的系统高频谐振和失稳问题,并能有效抵抗系统扰动,具有很好的跟踪性能。     

CNES/GRGS 10-day gravity field models (release 2) and their evaluation

GRACE, designed to monitor temporal variations in the fluid mass at the surface of the Earth, is still operating and providing invaluable data 7 years after launch. One hundred and ninety-nine satellite-only geopotential solutions to degree and order 50 were recomputed per 10-day interval for the period 29 July 2002–27 May 2008 using an improved data editing and solution regularization procedure. These release 2 solutions are significantly improved compared to release 1 solutions, the noise over deserts and oceans in the form of North–South striping being reduced by 20–40%. This is thanks to the tailored regularization of each individual Stokes coefficient applied in the solution procedure, and to a time-variable reference model containing mean annual, semiannual and secular variations for degrees 2–50 towards which the variations per 10-day solution are constrained. It may attenuate signals of the order of a few percent, whereas this always occurs when applying a Gaussian smoother even with a half-width smoothing radius as small as 300 km. The uncertainty of an individual point in the time series of a basin expressed in equivalent water height inferred from the 10-day solutions is approximately 20 mm. Comparison of these 10-day solutions to monthly GRACE project solutions (CSR, GFZ and JPL) shows substantial differences. Even for the largest basin, the Amazon, a 15% difference in annual amplitude is found between CNES release 2 and CSR versus GFZ and JPL. The mass-loss estimates for East and West Greenland vary by 100%. Sometimes clear outliers are detected in the GFZ and JPL solutions when a particular basin is studied, which have to be eliminated. In view of the large differences detected between the time series for specific basins, it is hazardous to draw conclusions based on a single solution.     

弹道导弹主动段扰动引力的一种逼近算法

弹道导弹扰动引力的计算量非常大,目前的弹载计算机因计算速度限制,是不可能实现计算的,必须采用快速的扰动引力逼近算法。针对地面司托克斯积分方法等方法计算扰动引力的不足,提出了利用重力线求解重力的一种方法,并用该方法计算标准弹道附近的扰动引力,作为实际弹道扰动引力的逼近准备数据。给出了弹道主动段扰动引力的BP-神经网络逼近算法,并通过算例证明扰动引力的神经网络逼近是可行的。     

重力波波包在耗散大气中的非线性传播

本文对具有高斯分布的重力波波包在耗散大气中的非线性传播过程进行数据模拟和分析,并与重力波波包在无耗大气中非线性传播的数值计算结果进行了比较,以辨明耗散在重力波非线性传播过程中所起的作用。     

重力波对中层顶区光化加热的影响

计算了重力波过程对光化加热的影响,并研究了不同温度背景及不同氧原子的背景分析对该过程的影响,计算表明重力波可以造成中层顶光反应加热的损失。     

An investigation of the solar cycle impact on the lower thermosphere O(S) nightglow emission as observed by WINDII/UARS

The yearly variation of the integrated emission rate of the O(¹S) nightglow in the lower thermosphere is studied and the solar cycle impact is examined from the observations of the Wind Imaging Interferometer (WINDII) operated on the Upper Atmosphere Research Satellite (UARS). More than 300,000 volume emission rate profiles of the O(¹S) nightglow observed by WINDII for 40°S–40°N latitudes during November 1991–August 1997 over half of a solar cycle are utilized. These profiles are vertically integrated for the altitude range of 80–100 km and the equivalent column integrated emission rates are then zonally averaged for bins with 10° latitude and 3 month intervals. It is found that for each latitude the O(¹S) nightglow emission rate appears to increase with increasing solar F10.7 cm flux, following a linear relationship. This characterizes the solar cycle impact on the O(¹S) nightglow, while the solar influence is modulated by a seasonal variation. Based on these variations, an empirical formula is derived for predicting the three-month averages of the O(¹S) nightglow integrated emission rate. The standard error of the estimated values from the formula is smaller than 30 Rayleigh.