月壤含水特性原位快速预判传感器设计与验证

基于月壤和水冰对不同谱段近红外激光存在吸收/反射差异性的特点,提出了采用多模近红外激光光强差异反演月壤含水特性的水冰原位快速预判方法。通过发射/接收光路同轴设计及多模激光光路分时复用设计,实现了多模激光光学系统轻小型化设计,研制出基于多模近红外激光的月壤水冰原位快速预判传感器工程样机,并开展了针对低含水率极区模拟月壤的含水特性原位预判试验。试验结果表明：该传感器水冰检测限可达0.39%,单次预判时间可优于1 s,光斑直径@检测距离为5 cm@500 mm,传感器具备对地面模拟月壤含水特性进行原位快速预判的能力。     

Weibull分布定时截尾寿命试验参数的近似联合置信域

研究了Weibull分布大样本定时截尾寿命试验，利用一种新的途径给出了试验参数的近似联合置信域。设产品寿命X服从Weibull分布，对n个受试样本x1,x2，…，xn进行定时（时间为t0）截尾试验，得到观察数据Si=min(x1,x0)，i=1,2,…，n。利用似然方程，分别得到参数λ，b的极大似然估计λ和b。进一步考察联合分布（λ，b）可以用二元正态分布来近似。再利用多元正态分布与X^2分布的关系，可以推导出未知参数u=（λ，b）的置信度为1－a的联合置信区域（x-u)′I0（x-y)≤xa^2。     

基于ODE参数辨识的液压伺服系统灰箱建模

 针对液压伺服系统常规"白箱"建模由于参数无法精确获得导致所得模型精度不高及"黑箱"建模所得模型内部结构未知的问题,本文提出基于ODE参数辨识的液压伺服系统"灰箱"建模。首先,建立了工程上实用的系统状态空间模型, 根据系统特征确定了待辨识参数,将模型辨识问题转化为常微分方程(ODE)参数辨识问题;然后,采用正弦扫频信号作为激励信号和基于带边界约束的信赖域优化算法的初值问题方法进行参数辨识;为了和ODE参数辨识结果进行对比,本文同时采用系统的频率响应数据和最小二乘法辨识得到系统的"黑箱"传递函数模型;最后,通过大量实验验证了辨识模型的精确度。实验结果表明,本文提出的基于信赖域算法的液压伺服系统模型辨识方法可以有效处理参数的边界问题,使辨识模型既具有实际的物理意义,又与实际系统高度符合。     

Novel approach of crater detection by crater candidate region selection and matrix-pattern-oriented least squares support vector machine

Impacted craters are commonly found on the surface of planets, satellites, asteroids and other solar system bodies. In order to speed up the rate of constructing the database of craters, it is important to develop crater detection algorithms. This paper presents a novel approach to automatically detect craters on planetary surfaces. The approach contains two parts: crater candidate region selection and crater detection. In the first part, crater candidate region selection is achieved by Kanade-Lucas-Tomasi (KLT) detector. Matrix-pattern-oriented least squares support vector machine (MatLSSVM), as the matrixization version of least square support vector machine (SVM), inherits the advantages of least squares support vector machine (LSSVM), reduces storage space greatly and reserves spatial redundancies within each image matrix compared with general LSSVM. The second part of the approach employs MatLSSVM to design classifier for crater detection. Experimental results on the dataset which comprises 160 preprocessed image patches from Google Mars demonstrate that the accuracy rate of crater detection can be up to 88%. In addition, the outstanding feature of the approach introduced in this paper is that it takes resized crater candidate region as input pattern directly to finish crater detection. The results of the last experiment demonstrate that MatLSSVM-based classifier can detect crater regions effectively on the basis of KLT-based crater candidate region selection.     

Photospheric flows in the active regions (asymmetric and localized Doppler velocities)

We observed 10 active regions through their disk passage during June 25–August 25, 1988, with the Tower Vector Magnetograph (TVM) of Marshall Space Flight Center. The TVM was used in scanning mode to measure the photospheric Doppler velocities with the Line-Center-Magnetogram (LCM) technique in the spectral line of FeI 5250.2 Å. In this paper we present the result of a subset of observations obtained while the active regions were situated away from the solar limb. A wide range of magnetic complexity and associated chromospheric activity characterized these active regions. It was found that the value of zero-crossing wavelength of the integrated Stokes-V profile of two opposite magnetic polarities were different, corresponding to Doppler velocities ranging from ∼100 m s⁻¹ to ∼1475 m s⁻¹. The measurements of relative velocities between different locations, connected by magnetic flux tubes as inferred from YOHKOH soft X-ray and TRACE 171 Å Fe IX images, showed widely different values of dominant localized flows. The region of parasite polarity, which showed recurrent chromospheric activity, was blue shifted with respect to the main “magnetic element” of the same polarity. Some of them were also the sites of sheared magnetic field configuration. The magnitude of the relative velocity between the leading and following polarity is more for the active regions of higher “field asymmetry”.     

IRI-2007预测TEC在广州地区的适用性分析

利用广州站(23.2°N, 113.3°E) GPS双频接收机监测的电离层TEC数据和IRI-2007模型不同电离层输入参数计算得到的TEC预测值, 对比分析了太阳活动低年(2008年)广州地区TEC的变化特征. 结果表明, TEC观测值周日变化在16:00LT左右达到最大值, 而IRI-TEC最大值出现时间较GPS-TEC提前1h左右. TEC季节变化在春秋分较高, 两至季节较低, 表现出明显的半年特性和季节依赖性, 并出现冬季异常现象. IRI-TEC与GPS-TEC在白天具有较好的一致性, 夜间偏差较大. 不同电离层输入参数得到的TEC预测值也相差较大, 选用顶部电子密度参数NeQuick、底部厚度参数B0 Table并用URSI系数计算F₂层峰值参数时, 能较好地反映TEC观测值的变化特征. 在对磁暴的响应上, 预测值无明显变化, 观测值则有比较明显的表现. 通过对比, 初步分析了利用IRI-2007模型预测TEC在广州地区的适用性, 并给出了合理的参数选择方案.      

太阳风中磁场重联离子扩散区的大尺度特征

利用ACE和WIND卫星2007年1月6日的联合探测, 在1AU附近发现了一个等离子体密度极低的Petschek-like重联喷流区. 该喷流区内部出现了非常明显的Hall双极磁场、等离子体密度下降区以及与Hall电流相符的低能段电子投掷角分布. 这些特征与重联离子扩散区的Hall效应非常吻合, 说明很可能在太阳风中观测到了一个离子扩散区. 分析表明, 与之相关的磁场重联为准稳态快速完全反向重联, 其扩散区以一对慢模波为边界, 空间尺度达到80个离子惯性长度, 表现出了大尺度重联的特征.      

基于参数辨识原理的飞机参数分析及算法研究

提出一种在飞机概念设计中基于参数辨识理论的设计参数分析方法。在给定的设计重量和任务剖面要求下,利用基于物理的运动方程和动力学方程模型辨识出飞机气动力参数,并在总体性能评估的基础上进行设计参数分析,给气动设计提供了设计参考;在辨识过程中针对参数可行域离散度很高使得很难收敛到Pareto解的问题,提出了将神经网络预测模型融合到遗传操作过程,使得尽量在可行域内搜索。最后通过对某客机进行算例分析,表明基于辨识理论的参数分析方法和改进的算法是合理和可行的。与一般经验公式方法相比,该方法对布局类型的限制较小,在满足概念设计参数分析准确度要求的条件下能够为下一步的气动设计提供设计指标。     

Seasonal patterns of condensation and sublimation cycles in the cryptic and non-cryptic regions of the South Pole

The South Pole of Mars is characterized by an asymmetric residual ice cap composed of water ice and CO₂ ice. On the opposite side of the residual cap, there exists an area called cryptic region which is relatively free of ice during summer time. Many fan-shaped km-scale structures apparently caused by a wind-blown system of dust-laden gas jets occurred dozens degrees of Ls before the complete sublimation of the CO₂ frost layer. We have examined the seasonal cycles of condensation and sublimation in the cryptic and non-cryptic regions by using the topographic data from the MOLA/MGS measurements. Using the MOLA topography data collected over one Martian year (1999–2001), we have studied the temporal elevation change and the seasonal cycle of the carbon dioxide frost on the southern polar caps. We have produced mapping of the seasonal CO₂ frost thickness variation for seven Ls (30°, 60°, 90°, 120°, 150°, 180°, 210°, 240°, 270° and 330°). It is found that the time variations of the CO₂ frost thickness in these two regions are quite similar. The greatest thickness of the CO₂ frost layer is about 0.76–0.78 m in both places occurs at Ls = 150°.