具侧向脉冲力制导炮弹的非线性稳定性分析

研究了制导炮弹受侧向脉冲推力作用后处于大攻角情况下的非线性运动稳定性问题.应用首次积分描述了弹丸的运动方程,得到了描述攻角余弦变化的多项式,通过对多项式的分析将弹丸角运动稳定性的问题转化为求解多项式的负根问题,最后运用霍尔维茨定理给出了弹丸非线性运动稳定的充分条件,为非线性运动条件下弹丸的飞行形态的预测、脉冲执行机构的设计等问题提供了一定的理论依据.      

卫星编队的多脉冲队形重构方法

主要研究了椭圆轨道燃料消耗最优的多脉冲编队队形重构问题.首先,基于Lawden方程的解析解,推导了多脉冲机动的数学模型.然后构造燃料最优目标函数,将总脉冲写成关于各脉冲作用时间和前n-2次脉冲大小的函数.然后利用遗传算法对问题进行求解,将结果转换到时间域,确定最终各脉冲的大小、方向和作用时间.最后进行了数学仿真,验证了算法的正确性.     

一个大范围同胚定理

本文给出了一个大范围同胚定理。它类似于Mananvich[1]中的一个极小极大原理。这个定理可以用于讨论形如AU=V的一类算子方程的解的存在唯一性问题。其中算子A可以是无位和不可微的。     

带VSCMGs的航天器姿态稳定及功率补偿控制

基于变速控制力矩陀螺群动力学模型建立其复合控制方程和分系统解耦约束方程,用矩阵投影方法同步设计得到航天器姿态与能量一体控制复合操纵律,利用Lyapunov方法分析了转子轴向惯量误差对姿态控制分系统的影响.根据飞轮转子轴向惯量与功率输出之间的误差关系设计出功率控制补偿器.复合操纵律中的力矩和功率两解形式相同,约束方程使得姿态与能量控制两分系统解耦,便于进行考虑执行机构特性的闭环控制系统性能分析.考虑飞轮转子轴向惯量误差时,姿态控制分系统的输出耗散特性使其能够保持稳定,而功率控制分系统输出误差与转子轴向惯量误差成比例关系,经过补偿后功率输出能满足控制要求.     

航天器轨道交会迭代制导算法

针对航天器轨道交会的脉冲推力模型与实际发动机连续推力模型不相符的问题,研究一种脉冲变轨策略的工程实现方法,使脉冲变轨策略可应用于工程实际.基于Lambert飞行时间定理和遗传算法,研究航天器最优脉冲变轨策略.根据脉冲变轨优化的结果,采用迭代制导算法研究脉冲变轨工程化问题.仿真结果验证了迭代制导算法在航天器轨道交会中的有效性.     

基于长方体禁飞区的安全绕飞轨迹设计

摘要： 以C W方程为基础针对圆轨道近距离双脉冲绕飞问题,研究基于长方体禁飞区的安全绕飞轨迹设计方法.针对双脉冲绕飞动力学模型中的变量进行代数变换,在此基础上对变量间的关系进行推导,证明部分变量在特定区间范围内具有单调性的定理;给出保证绕飞轨迹安全的约束条件,进而结合推导出的定理和安全约束条件得到轨道面内全方位安全绕飞轨迹的一般性设计方法.通过针对以目标器正后方为绕飞起点的两种典型绕飞以及到任意方位的绕飞进行仿真,验证方法的有效性.     

一类加权不等式及在临界指数问题中的应用

研究了关于调和算子的加权不等式,推广了Bernis等人关于类似问题的结果,并且得到一些新结果．利用这些新结果,讨论了关于半线性部分是多调和算子的临界指数问题. 改进了问题存在非平凡径向解的必要条件,使该问题存在非平凡径向解的范围比已知的范围增大一倍.      

超快变换复合脉冲方波变极性TIG电弧行为

基于一种新型超快变换复合脉冲变极性电路变换拓扑,在正极性电流持续期间,叠加超音频直流脉冲方波电流,获得了过零无死区时间且具有快速电流上升沿和下降沿变化速率的复合超音频脉冲变极性方波电流,将其应用于铝合金的变极性TIG焊接过程,试验研究复合超音频脉冲方波变极性TIG电弧电学特性及其对铝合金焊缝成形等行为的变化规律.研究结果表明:超音频脉冲方波电流对变极性TIG电弧具有显著的收缩效应,电弧径向尺寸明显减小,在一定范围内提高脉冲电流频率,减小脉冲占空比,增加脉冲电流幅值,可提高铝合金焊缝熔透率,有利于改善和提高铝合金的焊接质量.     

激光微推力器的控制系统设计

针对微小卫星、钠卫星编队飞行时的姿态和轨道控制要求,提出星载微推力器的概念,而激光微推力器在众多的微推力器中以能产生10^-7N·s-10^-4N·s的最小冲量受到了国内外研究学者的关注。激光微推力器系统包括五个分系统,通过采用软件芯片DSP驱动步进电机的控制策略对控制分系统进行设计,实验结果表明可以取得较高的控制准确度。     

一类最省燃料优先的多圈飞行脉冲交会

通过分析采用多圈飞行Lambert解的双脉冲交会的特征速度与转移轨道半长轴的关系,指出其最优解实际上是2N+1条满足时间约束的转移轨道中燃料较省的,而非最省燃料轨道.提出将双脉冲交会的首次脉冲矢量分解成方向相同的两次脉冲,使得追踪器在特定的滑行轨道飞行N圈以消耗多余的转移时间,利用剩余的转移时间沿最省燃料轨道与目标交会.几何上证明了这种交会的特征速度与最省燃料转移相同,并且给出了解的存在性条件.通过仿真验证了这种交会比采用多圈飞行Lambert解的双脉冲交会更省燃料,解的存在性对转移时间的长度要求更低.     

Physics of the impulsive phase of solar flares

The physics of the impulsive phase of solar flares is discussed in relation to high resolution microwave, hard X-ray and ultraviolet observations. High spatial resolution observations of the structure of microwave flaring loops and their interpretation in terms of arcades of loops as the sites of primary energy release are presented. Theoretical interpretation of the confinement of microwave producing energetic electrons in the coronal part of loops is discussed. High temporal and spatial resolution measurements in hard X-rays, as well as observations of the spectral evolution of the hard X-ray emission are presented. Observations of the relative locations of microwave and hard X-ray emitting regions are presented and their significance with respect to the energy release site and electron acceleration is discussed. The relative timing of the peaks of impulsive hard X-ray and microwave burst is discussed. The significance of ultraviolet measurements in obtaining the density of flaring regions is discussed. Possible diagnostics of impulsive phase onsets from cm-λ polarization data are presented, and the role of the emergence of new flux and of the current sheet formed between closed loops in producing impulsive energy release at centimeter wavelengths are analyzed. Decimeter and meter wave manifestations of preflash phase and millisecond pulsations at centimeter and decimeter wavelengths and the relevant physical processes involved are discussed.     

自适应评判神经网络在微分对策中的应用

采用由3个神经网络组成的自适应评判神经网络结构求解微分对策的2点边值问题,其中2个 为控制神经网络,分别实现对微分对策系统中双边控制器的优化,一个为协 态神经网络,用于对2点边值问题中的协态变量进行求解,协态网络的输出对控制网络进行 校正,训练以后的2个控制网络作为双边的反馈控制器在线应用.并将神经网络结果与采用 Chebyshev技术的微分对策数字解进行了对比.追逃微分对策仿真结果表明了该方法的有效 性,并且对初始条件和测量噪声具有较强的鲁棒性.      

树形多体Hamilton系统的Lyapunov指数计算方法

研究了树形多体Hamilton系统Lyapunov指数的数值方法.利用多体Hamilton系统的正则方程和辛算法, 给出了多体Hamilton系统Lyapunov指数的计算方法,该算法具有较好的计算精度和通用性.利用该算法可对系统的运动稳定性进行分析.最后用算例说明了该算法的有效性.      

差分不等式与离散系统的稳定性

采用“差分不等式”的方法研究离散系统稳定性。文中首先建立几个差分不等式。然后,利用这些不等式来研究非线性离散系统和离散大系统的零解的稳定性问题,得到了用级数的敛散性来判定系统的零解的稳定性的几个充分准则。     

Onset study of impulsive solar energetic particleevents

Impulsive solar energetic particle (SEP) events are associated with impulsive X-ray flares, energetic electrons,and enhanced heavy ion abundances. Using instruments on ACE, we have examined the composition and origin of twelve impulsive SEP events from November 1997 to June 2000. All selected impulsive SEP events have enhanced ³He/⁴He ratios compared with the solar wind values. The range of ³He/⁴He ratios varies from 0.01 to 7.8. By assuming scatter-free propagation at zero degree pitch-angle, we fitted the minimum particle path lengths (from 1.2 to 1.4 AU, as expected), and estimated the ion event release time back at the Sun to within better than 30 minutes in most cases. We found only four events in which the release times agree for both 38–50 keV electrons and <1 MeV/nucleon ions. Five of our events have significant differences (>40 minutes) between the electron and ion onset times, all with ions injected later. Three impulsive ion events have no association with any impulsive electron event. Seven events have associated solar electromagnetic signatures (Type III radio bursts and/or X-ray flares).     

输入受限卫星姿态的鲁棒非线性镇定与跟踪控制

研究控制输入受限的卫星在存在外部干扰和转动惯量不确定性时的姿态镇定和姿态跟踪控制问题,利用双曲正切函数的性质分别设计了两种有界鲁棒非线性反馈控制律,并用李雅普诺夫方法证明：通过适当选择两种控制律中的参数,可保证闭环系统角速度误差渐近趋于零,且姿态误差收敛到事先给定的原点小邻域内．仿真结果表明利用所设计的控制律可在控制输入受限情况下有效抑制外部干扰和转动惯量不确定性的影响,达到预期控制目标．     

Stability of relative equilibria of the full spacecraft dynamics around an asteroid with orbit–attitude coupling

The full dynamics of spacecraft around an asteroid, in which the spacecraft is considered as a rigid body and the gravitational orbit–attitude coupling is taken into account, is of great value and interest in the precise theories of the motion. The spectral stability of the classical relative equilibria of the full spacecraft dynamics around an asteroid is studied with the method of geometric mechanics. The stability conditions are given explicitly based on the characteristic equation of the linear system matrix. It is found that the linearized system decouples into two entirely independent subsystems, which correspond to the motions within and outside the equatorial plane of the asteroid respectively. The system parameters are divided into three groups that describe the traditional stationary orbit stability, the significance of the orbit–attitude coupling and the mass distribution of the spacecraft respectively. The spectral stability of the relative equilibria is investigated numerically with respect to the three groups of system parameters. The relations between the full spacecraft dynamics and the traditional spacecraft dynamics, as well as the effect of the orbit–attitude coupling, are assessed. We find that when the orbit–attitude coupling is strong, the mass distribution of the spacecraft dominates the stability of the relative equilibria; whereas when the orbit–attitude coupling is weak, both the mass distribution and the traditional stationary orbit stability have significant effects on the stability. We also give a criterion to determine whether the orbit–attitude coupling needs to be considered.     

一类混合动态系统的稳定性

混合动态系统是一类同时含有连续时间变量和离散事件变量的系统，在这类系统中，两类变量耦合在一起，具有复杂的动力学特性和时钟关系。本文在一般度量空间上刻画了混合动态系统，并给出了混合动态系统在Ｌｙａｐｕｎｏｖ意义下稳定和渐近稳定的定义及其充分必要条件，同时研究了一类混合动态系统稳定与其连续和离散事件子系统的稳定性之间的关系。     

An Integer Precise Point Positioning technique for sea surface observations using a GPS buoy

GPS data dedicated to sea surface observation are usually processed using differential techniques. Unfortunately, the precision of resulting kinematic positions is baseline-length dependent. So, high precision sea surface observations using differential GPS techniques are limited to coasts, lakes, and rivers. Recent improvements in GPS satellite products (orbits, clocks, and phase biases) make phase ambiguity fixing at the zero difference level achievable and opens up the observation of the sea surface without geographical constraints. This paper recalls the concept of the Integer Precise Point Positioning technique and discusses the precision of GPS buoy positioning. A sequential version of the GINS software has been implemented to achieve single epoch GPS positioning. We used 1 Hz data from a two week GPS campaign conducted in the Kerguelen Islands. A GPS buoy has been moored close to a radar gauge and 90 m away from a permanent GPS station. This infrastructure offers the opportunity to compare both kinematic Integer Precise Point Positioning and classical differential GPS positioning techniques to in situ radar gauge data. We found that Precise Point Positioning results are not significantly biased with respect to radar gauge data and that horizontal time series are consistent with differential processing at the sub-centimetre precision level. Nevertheless, standard deviations of height time series with respect to radar gauge data are typically [4–5] cm. The dominant driver for noise at this level is attributed to errors in tropospheric estimates which propagate into position solutions.     

Chromospheric line emission in seismically active flares

Some flares are known to drive seismic transients into the solar interior. The effects of these seismic transients are seen in helioseismic observations of the Sun’s surface thousands of km from their sources in the hour succeeding the impulsive phase of the flare. Energetic particles impinging from the corona into the chromosphere are known to drive strong, downward-propagating shocks in active region chromospheres during the impulsive phases of flares. H observations have served as an important diagnostic of these shocks, showing intense emission with characteristic transient redshifts. In most flares no detectable transients penetrate beneath the active region photosphere. In those that do, there is a strong correlation between compact white-light emission and the signature of seismic emission. This study introduces the first known H observations of acoustically active flares, centered in the core of the line. The morphology of line-core emission H in the impulsive phase of the flare is similar to that of co-spatial line-core emission in NaD₁, encompassing the site of seismic emission but more extended. The latter shows a compact red shift in the region of seismic emission, but a similar feature is known to appear in a conjugate magnetic footpoint from which no seismic emission emanates. Radiative MHD modelling based on the profiles of chromospheric line emission during the impulsive phases of flares can contribute significantly to our understanding of the mechanics of flare acoustic emission penetrating into the solar interior and the conditions under which it occurs.