Observations of loops and prominences

We review recent observations by the Yohkoh-SXT in collaboration with other spacecraft and ground-based observatories of coronal loops and prominences. These new results point to problems that SoHO will be able to address. With a unique combination of rapid-cadence digital imaging (32 s full-disk and 2 s partial-frame images), high spatial resolution (2.5 arcsec pixels), high sensitivity (EM 10⁴² cm^–3), a low-scatter mirror, and large dynamic range, SXT can observe a vast range of targets on the Sun. Over the first 21 months of Yohkoh operations, SXT has taken over one million images of the corona and so is building up an invaluable long-term database on the large-scale corona and loop geometry. The most striking thing about the SXT images is the range of loop sizes and shapes. The active regions are a bright tangle of magnetic field lines, surrounded by a network of large-scale quiet-Sun loops stretching over distances in excess of 10⁵ km. The cross-section of most loops seems to be constant. Loops displaying significant increase in the ratio of the footpoint to loop-top diameter () are the exception, not the rule, implying the presence of widespread currents in the corona.All magnetic structures show changes. Time scales range from seconds to months. The question of how these structures are formed, become filled with hot plasma, and are maintained is still open. While we see the propagation of brightenings along the length of active-region loops and in X-ray jets with velocities of several hundred km/s, much higher velocities are seen in the quiet Sun. In XBP flares, for example, velocities of over 1000 km/s are common. Active-region loops seem to be in constant motion, moving slowly outward, carrying plasma with them. During flares, loops often produce localized brightenings at the base and later at the apex of the loop. Quiescent filaments and prominences have been observed regularly. Their coronal manifestation seems to be an extended arcade of loops overlying the filament. Reliable alignment of the ground-based data with the X-ray images make it possible to make a detailed intercomparison of the hot and cold plasma structures over extended periods. Hence we are able to follow the long-term evolution of these structures and see how they become destabilized and erupt.     

大攻角非对称流动的非定常弱扰动控制

 研制了一种新的大攻角细长旋成体非对称涡的主动控制技术, 即在细长旋成体头部施加非定常弱扰动来控制头部非对称背涡。应用七孔探针测量的空间截面流场揭示了非定常控制下非对称涡变成对称涡的流态特征。测力试验研究结果表明该方法不仅能完全消除背涡的非对称性及其产生的侧向力, 并且有效控制攻角范围从30b直到80b。     

有限元动力模型优化的一种方法

本文研究以振动试验测得的飞机结构的固有频率为目标值的有限元动力模型的优化问题。应用了一种迭代优化法,该方法基于动力平衡方程以及正交性。通过修改刚度矩阵的元素来优化,使计算出的固有频率与试验测得的频率值基本一致,并成功地应用于无人机水平尾翼模型上,效果良好。     

采用逐次正交化法的最优分布式Kalman滤波器

为解决大系统中应用整体式Kalman滤波遇到的非实时性难题,本文提出一种能保持最优的分布式Kalman滤波计算方法——逐次正交化法。这是一种适合多微机并行计算的最优算法,确保滤波的“实时性”,优于一般次优分布式Kalman滤波器。     

面内强磁场下铁磁板壳的自由振动

本文研究了面内强磁场环境下铁磁板壳的自由振动问题。基于Eringen-Maugin的关于磁弹性作用的理性力学模型,从理论上推导了一般壳体在磁场中的运动方程,进而求解了面内强磁场作用下的小磁化率悬臂铁磁薄板自由振动频率。数值计算结果表明,本文模型和已有的实验结果吻合很好。     

基于数字滤波的B-样条插值法在图像旋转中的应用

提出一种基于无限脉冲响应和有限脉冲响应数字滤波技术的快速 B-样条插值法 ,并将其应用于实时图像旋转处理中。为了优化旋转后的图像质量 ,本文采用 3次 B-样条对图像旋转后的像素点灰度值进行插值运算。另外 ,通过对传统图像旋转矩阵的分解 ,将图像在二维空间中的旋转运算分解成为三步在一维空间内平移运算 ,使插值运算在一维空间中完成 ,从而简化了图像旋转数据处理中的插值运算。最后 ,还提出了一种以硬件方法完成高阶图像插值运算实现图像旋转的新方法 ,并针对 2 5 6灰度级 ,2 5 6× 2 5 6像素的图像 ,设计出一个以 FPGA为核心的实时、高质量的硬件图像旋转系统。     

羊毛精纺织物服用性能优选的多属性模糊决策

本文应用多属性目标决策的方法,评判不同规格毛织面料的"满意度",客观地提供一个重要的优选辅助依据。     

面向代理模型的机翼变形计算方法

按照机翼结构设计的原则,对内部结构还未确定的机翼提出了一种通用的变形计算方法。机翼的平面形状可看作由多个梯形组成,机翼弯曲变形为三次函数,扭转变形为一次函数。只要给定翼梢挠度与扭转角,即可计算机翼变形情况下的几何模型,使代理模型能够预测变形后机翼的气动载荷分布。文中给出了两个实际机翼的算例。算例结果表明,本文模型预测的变形与实际结构有限元分析给出的变形吻合较好。     

基于响应面法的超燃冲压发动机进气道多目标优化

基于响应面法进行了二维混合压缩超燃冲压发动机进气道的多目标优化研究.采用均匀试验设计确定试验方案,运用计算流体动力学求解进气道的性能.根据分析结果构造了响应面近似模型,该模型采用了完全二阶多项式模型.通过响应面近似模型的优化,实现了超燃冲压发动机进气道优化,得到了Pareto最优集.结果表明,采用均匀试验设计和响应面法可以大大减小数值模拟的计算量,提高优化效率.     

用电离层特性参量提取等效风场信息

导出了利用中低纬电离层特性参量获取电离层F层峰区高度上等效风场（包含电场和风场信息在内）的基本方程，并尝试用该方法从电离层特性参量（峰高和临频）提取等效风场信息，利用武汉站DGS-256电离层数字测高仪数据及由美国Massachusetts Lowell大学最新版的剖面反演程序换算得到F层峰高，获得了武汉地区夏季至日点附近，冬季至日点附近，冬季地磁特别宁静的九天和冬季平均等效风场的初步特征，并利用Fejer经验电场模式计算冬季电场引起的垂直漂移，估计电场和风场对武汉地区的垂直等效风场的贡献大小，结果表明：等效风场呈现出白天与夜晚幅度和方向的差异。至日点附近冬季与夏季白天的幅度差异以及明显的凌晨凹陷现象；平均情况下，垂直等效风场幅度和方向的变化主要是由中性风引起，受电场的影响不大。