矩形截面管道气流中横向运动颗粒的碰壁条件

分析了矩形截面管道气流中横向运动颗粒的运动轨迹及碰壁条件，研究表明颗粒飞出的临界速度随着颗粒直径的增大而减小，当颗粒直径较小时受来流密度、马赫数影响较大，总趋势是来流密度、马赫数越大，颗粒越不容易与上壁面碰撞。但随着颗粒直径的增大，来流条件对颗粒是否碰壁的影响逐渐减弱，决定因素是颗粒直径的大小和颗粒的喷射速度。     

大型双曲冷却塔表面脉动风压随机特性——风压极值探讨

针对风压信号呈现的非高斯特性和传统极限估计方法的局限,首次提出基于保证率和相关性的极值估计方法——全概率迭代法进行冷却塔表面脉动风荷载极值分析,并和传统的峰值因子法及改进的Sadek-Simiu法计算结果进行对比验证。结果表明：全概率迭代法避开了对随机过程的高斯分布假定,相比传统的极值估计方法其结果更加真实可靠;表达风压极值中脉动分量的峰值因子数值沿着环向和子午向变化显著,如取为同一数值则偏于危险或过于保守;采用全概率迭代法得到的表面风压系数极值分布曲线与规范取值相比,迎风面和负压峰值区域极值偏小,背风区域极值偏大,且最小值对应角度相差约10°。     

数字示波器在尖峰干扰脉冲强度测量中的应用

运用数字示波器瞬态捕获能力及面积测量功能，快速、准确、不遗漏地测量电子设备的尖峰干扰信号（脉冲信号），用公式将脉冲强度单位换算为脉冲频谱密度单位。     

民机复合材料典型结构件检修间隔的概率分析

民机复合材料结构在服役过程中的损伤主要来源于意外冲击,会大幅度降低结构强度,影响飞机安全.以某型飞机外翼为例,考虑运行过程中意外冲击损伤的产生、载荷超限和维护过程中损伤的漏检等因素,采用概率分析方法对结构失效概率进行分析,并计算详细目视检测方法对应的检修间隔.结果表明,计算得到的检修间隔略大于工程实际中"4C"值.此概率分析方法用来确定复合材料结构件检修间隔是可行的,并可以实现检修间隔的动态化调整.     

网格拓扑对DLR-F6构型数值模拟的影响

基于TRIP3.0软件平台和多块结构网格技术,开展了控制方程和网格拓扑等因素对DLR-F6构型数值模拟的影响研究。数值计算采用与试验相同的参数,采用了RANS/TLNS方程,生成了O型和H型2种拓扑的粗、中、细网格进行模拟。分别从气动特性、压力系数分布曲线和表面流态3个方面对结果进行分析。通过与试验数据的对比表明,在模拟小分离流动时,采用H型拓扑网格和RANS方程模型,获得的计算结果会更为准确。     

基于序列近似优化算法的固体运载火箭弹道设计

采用打靶法研究固体运载火箭弹道优化设计问题。针对打靶法中智能优化算法效率、优化问题中约束条件提法等方面的不足,引入序列近似优化算法,提出算法中径向基函数高斯核宽度的高效确定方法。数值仿真实验表明,提出的方法可在基本不带来计算量增加的前提下,显著提高代理模型精度,使序列近似优化算法得到改进,提高优化效率。设计固体运载火箭飞行程序。建立弹道优化设计问题数学模型,并将模型中相关等式约束合理转化为不等式约束,降低优化问题求解难度;基于改进后的序列近似优化算法完成某固体运载火箭弹道优化,原始计算模型调用308次之后便搜索到最优解,较传统智能优化算法显著提高了优化效率,优化方案末助推级液体推进剂消耗比原方案减少25.7%。     

雷达侦察环境信号密度量化研究

在分析现代雷达侦察环境信号特点基础上,提出了以时域、空域、频域和功率域参数为参变量的雷达侦察环境信号密度量化参数——环境信号占空比,并通过理论分析和实验证明了其单调性、稳定性和可测性等基本性质.该量化参数对于测量评估现代战场雷达侦察环境信号密度、构设雷达侦察装备试验所需的复杂电磁环境,具有比较重要的意义.     

强光光学零件加工误差频谱分析与控制方法研究

本文利用功率谱密度分析磁流变抛光表面的敏感频率误差,发现走刀步距与中高频误差具有直接的关联性,通过小波算法确定其分布区域后,采用大束径的光顺抛光法对敏感频率误差进行控制,测试结果表明中高频误差得到了有效控制。本研究对强光光学零件加工误差的频谱分析、表征和控制具有指导意义。     

Solar cycle and latitude dependence of high-beta suprathermal plasma conditions in interplanetary space between 1.3 and 5.4 AU

The analysis of energetic particles and magnetic field measurements from the Ulysses spacecraft has shown that in a series of events, the energy density contained in the suprathermal tail particle distribution is comparable to or larger than that of the magnetic field, creating conditions of high-beta plasma. In this work we analyze periods of high-beta suprathermal plasma occurrences (β_ep > 1) in interplanetary space, using the ratio (β_ep) of the energetic particle (20 keV to ∼5 MeV) and magnetic field energy densities from measurements covering the entire Ulysses mission lifetime (1990–2009) in order to reveal new or to reconfirm some recently defined interesting characteristics. The main key-results of the work are summarized as follows: (i) we verify that high-beta events are detected within well identified regions corresponding mainly to the vicinity of shock surfaces and magnetic structures, and associated with energetic particle intensity enhancements due to (a) reacceleration at shock-fronts and (b) unusually large magnetic field depressions. (ii) We define three considerable features for the high-beta events, concentrated on the next points: (a) there is an appreciable solar-activity influence on the high-beta events, during the maximum and middle solar-cycle phase, (b) the annual peak magnitude and the number of occurrences of high events are well correlated with the sunspot number, (c) the high-beta suprathermal plasma events present a spatial distribution in heliographic latitudes (HL) up to ∼±80°, and a specific important concentration on the low (−25° ? HL < −6°, 6° < HL ? 25°) and median (−45° ? HL < −25°, 25° < HL ? 45°) latitudes. We also reconfirm by a statistical analysis the results of Marhavilas and Sarris (2011), that the high-beta suprathermal plasma (β_ep > 1) events are characterized by a very large parameter β_ep (up to 1732.5), a great total duration (406 days) and a large percentage of the Ulysses-mission lifetime (which is equal to 6.34% of the total duration with usable measurements, and 11.3% of the duration in presence of suprathermal particles events).     

A global survey of COSMIC ionospheric peak electron density and its height: A comparison with ground-based ionosonde measurements

With a network of ground-based ionosondes distributed around the world, the ionospheric peak electron density and its height measured by FORMOSAT-3/COSMIC satellites in terms of GPS radio occultation technique are extensively examined in this article. It is found that, in spite of the latitude, the mean values of the peak electron density measured by COSMIC satellites are systematically smaller than those observed by ground-based ionosondes. The discrepancy between them is dependent on the latitude, namely, it is small in low and mid-latitudes and large in high-latitude region. Moreover, statistical analysis shows that the slopes of the regression line that is best fitted to the scatter diagram of occultation-retrieved peak electron density (ordinate axis) versus ionosonde-observed peak density (abscissa axis) are universally less than one. This feature is believed to be the result of path average effect of non-uniform distribution of the electron density along the GSP ray during the occultation. A comparison between COSMIC-measured peak height and ionosonde-derived peak height hmF2 indicates that the former is systematically higher than the latter. The difference in the two can be as large as 20% or more in equatorial and low-latitude regions. This result implies that the peak height hmF2 derived from the virtual height through true height analysis based on Titheridge method seems to underestimate the true peak height. The correlation between COSMIC and ionosonde peak electron densities is analyzed and the result reveals that correlation coefficient seems to be dependent on the fluctuation of the occultation-retrieved electron density profile. The correlation will be higher (lower) for the electron density profiles with smaller (larger) fluctuations. This feature suggests that the inhomogeneous distribution of the electron density along the GPS ray path during the occultation plays an important role affecting the correlation between COSMIC and ionosonde measurements.