空间站大面积太阳翼热分析

本文在一定的假设条件下，对空间站大面积太阳翼进行了系统的热流和温度场计算。在计算中利用矢量分析和坐标变换的方法求解出了太阳直接辐射1地球红外辐射和地球反照的辐射角系数，再根据传热学理论建立了瞬态热平衡方程，应用有限单元法对热平衡方程进行了求解。本文通过计算给出了各项热流的大小及在总热流中所占的比例和太阳民办的瞬态温度场分布，对空间站大面积太阳翼设计及热控制具有一定的参考价值。     

斜置尾桨对直升机飞行特性的影响

基于叶素理论建立了斜置尾桨的数学模型,以UH-60A直升机为对象,计算了平飞配平特性,并与试飞结果进行对比,完成了对模型的验证。验证结果表明,所建的斜置尾桨模型合理准确,能满足工程精度。本文从直升机悬停需用功率研究了尾桨斜置角的设计,计算了不同尾桨斜置角对直升机悬停需用功率的影响,得出UH-60A直升机的尾桨斜置角优化值为20~25°。通过计算和对比斜置尾桨与常规尾桨直升机的平飞配平特性,得出尾桨斜置主要影响直升机的纵向配平特性。最后,对斜置尾桨的利与弊进行了一些讨论。     

模型变形视频测量的相机位置坐标与姿态角确定

高速风洞试验中的模型变形视频测量(VMD)要求双(多)相机大角度大重叠的测量方式,而通过现有共线方程的线性化模型难以取得高精度的相机位置与姿态角,故推导包含共线方程泰勒展开二次项的非线性误差模型,建立3控制点的VMD相机位置与姿态确定技术.多个工程实例表明该技术能取得高精度的相机位置坐标与姿态角,有实用价值.     

投影图像法对旋转体空间扫描角和转速的测量研究

扫描角和转速是某伞一弹系统风洞试验中要求必须测量的重要技术参数.对伞-弹系统扫描角和转速进行定量动态测量是试验中必不可少的技术环节.投影图像法测量的原理就是利用一定截面积的两路正交平行光源,将旋转弹体分别投影到两个正交的投影屏上,利用两套高速CCD成像系统,将两路弹体投影图像同步采集并实时记录下来,试验结束后利用图像处理软件自动计算出两路图像序列角度分量,按照时序合成出每一时刻弹体的空间扫描角,并根据序列角度分量,计算出弹体的瞬时转速和全周期平均转速.利用该测量方法,在西安某所立式风洞中成功对多个型号的伞-弹旋转弹体空间扫描角和弹体转速进行了测量,取得了良好的测量结果.旋转体的静态角度测量精度为0. 18°,动态扫描角测量精度控制在0. 25°以内.作者从扫描角测量原理和方法人手,着重介绍该投影图像处理测量系统的设计和实际运用,给出了某伞-弹系统风洞试验的测量结果.     

基于风洞试验的非定常空气动力模型识别

在某飞机模型大振幅风洞试验的基础上,分析讨论了单自由度叠加模型、动导数模型、混合模型和非定常模型的适用性.结果表明,单自由度叠加模型、动导数模型和混合模型在小攻角时均是可用的,在大攻角时都不能正确反映飞机的非定常迟滞特性;但与前两种模型相比,混合模型在中等攻角时仍然适用.对于非定常模型,无论在小攻角还是大攻角时,均能较好地反映耦合运动的非定常气动特性.     

广州地磁Z分量日变幅的谱特征

利用1972—1993年广州地磁资料，分析了Z分量日变幅的年平均、年变化和半年变化等低频成分的逐年变化，以及小于60天的短周期变化特征．同时对1972—1993年的F10.7日均值进行了谱分析．结果指出，广州地磁Z分量日变幅的年平均与太阳活动指数F10．7的年平均存在良好的线性相关；具有幅度大约5nT夏季极大的年变化，与太阳活动没有明显相关，是一种季节效应；存在春秋分极大的半年变化，幅度与太阳活动有关，高年的幅度明显大于低年；具有明显的与太阳自转相关的27天左右的变化和明显的与行星波有关的接近16日、10日、5日、2日等短周期变化．广州地磁Z分量日变幅的这些谱特征，有助于更深入地了解中低层大气对电离层影响的物理机制．     

昆虫翅膀图像特征的亚像素级提取方法

昆虫翅脉、翅脉交点及翅膀边缘是昆虫翅膀运动变形三维重构的主要依据.通过分析这三种特征的图像特点,对于翅脉中心,采用Hessian矩阵求出灰度极值点方向,并用二次曲线拟合该方向的灰度变化,通过确定该曲线极值点位置来提取亚象素翅脉中心;然后通过求灰度图像的梯度,在其梯度变化方向求极值点的方法提取翅膀边缘特征;此外根据翅脉方向变化的连续性提出了邻域角度约束方法确定翅脉交叉点,从而最终提取到亚像素级的翅膀边缘、翅脉及交叉点等特征.实际应用证明该方法是较为有效的.     

Interplanetary shocks and sudden impulses during solar maximum (2000) and solar minimum (1995–1996)

In this work a study is performed on the correlation between fast forward interplanetary shock parameters at 1 Astronomical Unit and sudden impulse (SI) amplitudes in the H-component of the geomagnetic field, for periods of solar activity maximum (year 2000) and minimum (year 1995–1996). Solar wind temperature, density and speed, and total magnetic field, were taken to calculate the static pressures (thermal and magnetic) both in the upstream and downstream sides of the shocks. The variations of the solar wind parameters and pressures were then correlated with SI amplitudes. The solar wind speed variations presented good correlations with sudden impulses, with correlation coefficients larger than 0.70 both in solar maximum and solar minimum, whereas the solar wind density presented very low correlation. The parameter better correlated with SI was the square root dynamic pressure variation, showing a larger correlation during solar maximum (r = 0.82) than during solar minimum (r = 0.77). The correlations of SI with square root thermal and magnetic pressure were smaller than with the dynamic pressure, but they also present a good correlation, with r > 0.70 during both solar maximum and minimum. Multiple linear correlation analysis of SI in terms of the three pressure terms have shown that 78% and 85% of the variance in SI during solar maximum and minimum, respectively, are explained by the three pressure variations. Average sudden impulse amplitude was 25 nT during solar maximum and 21 nT during solar minimum, while average square root dynamic pressure variation is 1.20 and 0.86 nPa^1/2 during solar maximum and minimum, respectively. Thus on average, fast forward interplanetary shocks are 33% stronger during solar maximum than during solar minimum, and the magnetospheric SI response has amplitude 20% higher during solar maximum than during solar minimum. A comparison with theoretical predictions (Tsyganenko’s model corrected by Earth’s induced currents) of the coefficient of sudden impulse change with solar wind dynamic pressure variation showed excellent agreement, with values around 17 nT/nPa^1/2.     

Research on a complex CME event including Hα, LASCO, radio and MDI observations

We present our research on a fast and decelerating partial halo coronal mass ejection (CME) event detected in multi-wavelengths in the chromosphere and the corona on 14 October, 1999. The event involved a whole complex active area which spanned more than 40° of heliolongitude. It included a strong solar flare (XI/1N) and a complex eruptive filament within an active region of the entire complex. Especially, several radio sources were detected in the decimetric range prior to the CME by the Nançay Radioheliograph (NRH). A linear force-free field extrapolation of the Michelson Doppler Imager (MDI) magnetogram was performed to calculate the magnetic topology of the complex prior to the triggering of the event. The presence of a coronal null point combined with the occurrence of two distant and nearly simultaneous radio sources put strong arguments in favor of the generalized breakout model for the triggering of the eruption. The analysis of the subsequent development of the event suggests that large interconnecting loops were ejected together with the CME.     

水基有机硅憎水剂对A3钢憎水处理的应用

以市售聚硅氧烷乳液为基料,辅以金属盐催化剂和醇胺类改性植酸水溶性缓蚀剂制备的水溶性有机硅憎水剂,用以处理A3钢磷化试样表面.考察了催化剂质量分数、植酸质量分数、植酸溶液的pH值、乳液与改性植酸的比率对憎水剂憎水处理效果及稳定性的影响;探讨了不同热处理温度、浸渍时间及热处理时间等工艺条件下憎水剂对金属表面憎水性的影响并确定了憎水剂配方和憎水处理工艺.结果表明,用该憎水剂处理的A3钢磷化试样接触角可达132°左右,A3钢磷化处理表面的耐腐蚀性能得到明显改善.