液体发动机涡轮泵端面密封长期贮存变形研究

为分析长期贮存条件下液体火箭发动机涡轮泵端面密封变形问题,采用有限元分析软件对其静环组件过盈配合过程中的变形及长期贮存中的蠕变进行了分析计算,考虑静环座与石墨环间摩擦不均匀及二者为椭圆等因素对变形的影响,估算得到最大变形量引起的介质泄漏率。研究表明:长期贮存条件下,石墨环端面沿圆周方向会出现马鞍形变形,径向为内高外低,石墨环变形会引起较大的介质泄漏率,长期贮存条件下的石墨环变形会对液体发动机安全使用构成隐患。     

雷达对扩频通信系统干扰分析方法

针对雷达与扩频通信系统的电磁兼容问题,提出一种基于时域符号级的雷达干扰分析方法.首先详细分析了雷达对扩频通信系统电磁辐射干扰的机理,推导得出扩频通信系统在脉冲雷达干扰下的误码率公式和曲线;然后利用建立的雷达电磁干扰仿真模型,对扩频通信系统采用不同扩频因子以及不同频率隔离度时的受扰性能进行了仿真分析,验证了理论分析结果的合理性;最后利用所提方法计算给出了微波频段5种典型雷达与扩频通信系统的频率-距离隔离关系.研究结果表明:该方法对于在更深层次上揭示雷达辐射干扰的本质,提高频谱利用效率具有重要意义.     

一种计算非定常二维流动的无网格算法

主要目的是发展一套求解非定常流动的无网格算法。计算区域的离散方面,提出了一种按区域进行填充布点的点云自动生成方法;发展了一种点云的运动技术来实现离散点云对物面边界的随体运动;在点云离散的基础上,采用最小二乘法求解矛盾方程的方法来求取空间导数,进而获得数值通量;采用双时间方法进行时间离散推进,其中物理时间迭代采用二阶隐式格式,伪时间迭代采用四步龙格一库塔显式格式,为了加速收敛,在伪时间迭代中采用了当地时间步长和隐式残值光顺等加速收敛措施。最后,利用本文算法模拟了NACA0012翼型和NACA64A010翼型的跨音速非定常流动,并将计算结果与实验测量结果进行了对比分析,验证了上述方法的正确性和实用性。     

航天电磁继电器可靠性容差分析技术的研究

航天电磁继电器是在航天电子系统中完成信号传递、执行控制、系统配电等功能的主要电子元器件之一，其可靠性直接影响整个航天电子系统的可靠性。航天继电器可靠性设计技术是其产品可靠性工程的关键技术。本文分析了当前各领域可靠性研究现状及航天电磁继电器产品的可靠性现状与问题，提出并建立了基于正交试验表的电磁吸力可靠性容差分析数学模型、基于概率统计方法的机械反力可靠性容差分析数学模型及基于“应力-强度干涉法”的吸反力配合特性可靠性容差分析数学模型。以某型号航天电磁继电器为例，进行了可靠性容差分析与研究，给出了对航天电磁继电器可靠性设计具有指导作用的重要结论。     

具有混合约束的DES Petri网控制器的设计

针对基于Petri网离散事件系统库所和变迁混合不等式约束反馈控制器的设计问题,提出一项新型设计具有库所和变迁混合约束的Petri网控制器的方法——利用Petri网简化技术把所有约束库所融合为一个与它们标识总量相等的库所,然后再与受约束的变迁进行对照比较,使控制器的设计更为简单并且避免了死锁,尤其是对规模较大的系统,其优势更加明显。借助一个应用实例．将该控制器设计方法与Yamalidou等人提出的控制器设计方法作比较,表明所提出的控制器设计方法不仅更简单、更有效而且可以应用到推广Petri网。     

四轴自由曲面非接触测量系统

提出一种四轴复合式自由曲面非接触测量系统,介绍了系统的组成及工作原理。阐述了该系统的两种测量功能,即回转式测量和多角度平面测量,并给出了测量实例。最后分析了系统的测量精度,实验证明本系统的精度优于0.1mm。     

基于LMI的结构摄动系统二次稳定裕度分析

研究了结构摄动系统满足指定性能的稳定裕度问题。从系统完全二次稳定性出发 ,给出了结构摄动系统满足 H∞ 性能指标的二次稳定半径定义 ,并且转化为基于线性矩阵不等式 (LMI)的极值问题进行计算。对于广义参数不确定性系统 ,基于 L MI给出了使二次稳定裕度尽可能大的 H∞ 控制器设计方法。该方法应用于某型双转子涡喷发动机稳态控制器的设计 ,拓宽了系统的鲁棒稳定界     

月球重力场模型精度比较研究

从阶方差、谱域分析以及大地水准面自由空气重力异常3个方面分析了月球重力场模型LP150Q,LP165P与SGM150各自的特点及差异,研究结果表明,SGM150重力场在中高阶项上得到了明显改善,在远月面可以发现明显的重力异常正负交替的现象。另外,对"嫦娥二号"变轨试验期间的测轨数据进行了轨道解算和预报,比较不同重力场模型的精度影响,发现基于SGM150模型的解算结果优于基于LP150Q和LP165P的,在定轨弧段内有10m量级的精度提升,可用于高精度的月球探测器精密定轨。     

半模机翼振动的风洞实验技术研究

飞行器机模型振动是影响其风洞实验数据可靠性的主要因素之一。为此,通过专门研制的半模振动模型,采用对称翼型NACA0012和层流翼型NACA64-210两种半模机翼进行了低速风洞振动实验。选取五种激振方式,用直接测力法得到模型在静态和不同激振方式下升力特性变化曲线,研究了振动频率、自然转捩和固定转捩、数据采集方式等参数对机翼气动特性测量结果的影响。结果表明：振动对半模机翼气动特性的影响程度因不同翼型构型、不同采集方式和翼面不同流动模式等而产生不同效果。结论对提高飞机模型风洞实验大迎角振动情况下的测量精准度有参考价值。     

Properties of Ground Level Enhancement Events and the Associated Solar Eruptions During Solar Cycle 23

Solar cycle 23 witnessed the most complete set of observations of coronal mass ejections (CMEs) associated with the Ground Level Enhancement (GLE) events. We present an overview of the observed properties of the GLEs and those of the two associated phenomena, viz., flares and CMEs, both being potential sources of particle acceleration. Although we do not find a striking correlation between the GLE intensity and the parameters of flares and CMEs, the solar eruptions are very intense involving X-class flares and extreme CME speeds (average ～2000?km/s). An M7.1 flare and a 1200?km/s CME are the weakest events in the list of 16 GLE events. Most (80?%) of the CMEs are full halos with the three non-halos having widths in the range 167 to 212?degrees. The active regions in which the GLE events originate are generally large: 1290?msh (median 1010?msh) compared to 934?msh (median: 790?msh) for SEP-producing active regions. For accurate estimation of the CME height at the time of metric type?II onset and GLE particle release, we estimated the initial acceleration of the CMEs using flare and CME observations. The initial acceleration of GLE-associated CMEs is much larger (by a factor of 2) than that of ordinary CMEs (2.3?km/s² vs. 1?km/s²). We confirmed the initial acceleration for two events for which CME measurements are available in the inner corona. The GLE particle release is delayed with respect to the onset of all electromagnetic signatures of the eruptions: type?II bursts, low frequency type?III bursts, soft X-ray flares and CMEs. The presence of metric type?II radio bursts some 17?min (median: 16?min; range: 3 to 48?min) before the GLE onset indicates shock formation well before the particle release. The release of GLE particles occurs when the CMEs reach an average height of ～3.09?R _s (median: 3.18?R _s ; range: 1.71 to 4.01?R _s ) for well-connected events (source longitude in the range W20–W90). For poorly connected events, the average CME height at GLE particle release is ～66?% larger (mean: 5.18?R _s ; median: 4.61?R _s ; range: 2.75–8.49?R _s ). The longitudinal dependence is consistent with shock accelerations because the shocks from poorly connected events need to expand more to cross the field lines connecting to an Earth observer. On the other hand, the CME height at metric type?II burst onset has no longitudinal dependence because electromagnetic signals do not require magnetic connectivity to the observer. For several events, the GLE particle release is very close to the time of first appearance of the CME in the coronagraphic field of view, so we independently confirmed the CME height at particle release. The CME height at metric type?II burst onset is in the narrow range 1.29 to 1.8?R _s , with mean and median values of 1.53 and 1.47?R _s . The CME heights at metric type?II burst onset and GLE particle release correspond to the minimum and maximum in the Alfvén speed profile. The increase in CME speed between these two heights suggests an increase in Alfvénic Mach number from?2 to?3. The CME heights at GLE particle release are in good agreement with those obtained from the velocity dispersion analysis (Reames in Astrophys. J. 693:812, 2009a; Astrophys. J. 706:844, 2009b) including the source longitude dependence. We also discuss the implications of the delay of GLE particle release with respect to complex type?III bursts by ～18?min (median: 16?in; range: 2 to 44?min) for the flare acceleration mechanism. A?similar analysis is also performed on the delay of particle release relative to the hard X-ray emission.