固体火箭发动机羽焰测温方法研究

根据固体火箭发动机羽焰特征研制了多目标多光谱高温仪,它可同时测量羽焰六个目标点的温度,每个目标点均有八个工作波长。同时提出了求解真温的实用方法,完成了固体火箭发动机羽焰温度及其分布的测量。     

利用谱方法数值求解三维球坐标系下的Navier-Stokes方程

从三维球坐标系下的Navier-Stokes方程出发,采用谱配置方法建立了一个三维球坐标系下中层大气波动传播的全非线性动力学数值模式;构造了合理的纬向边界,并利用初始给定的重力波波包对该模式进行了数值检验．计算结果展示了重力波波包在大气中传播的三维图像,波包整体向上传播,波相关扰动速度随高度的增加而增长．     

弹载SAR大斜视改进CS成像算法

针对弹载SAR在成像过程中复杂的运动状态,以及大斜视所造成的频谱混叠问题,建立了大斜视加速运动模型.引入新的CS因子,有效解决了距离频谱混叠问题并补偿了导弹在三方向速度和加速度的影响;引入方位deramp处理方法,有效解决了方位多普勒频谱混叠问题.仿真结果表明该方法优于现有算法.     

随机材料板结构的传递函数分析方法

本文将二维随机材料场作Karhunen-Loeve正交展开，应用传统有限条理论和摄动随机分析思想建立起静态随机板结构－系列微分方程，然后用传递函数方法求解这些微分方程得到结构的随机响应，该方法是一种半解析数值计算方法。     

单帧数字图像分辨率改善的频域正则化方法

现有多帧序列频域分辨率改善方法主要基于柯西-高斯先验模型，对单帧图像处理效果不理想。在分析频谱混叠公式的基础上，研究了单帧图像分辨率改善的频域方法。提出了基于柯西-高斯先验模型的正则化方法，由于柯西-高斯先验模型具有较好的信号稀疏表示能力，因此能有效地改善图像的分辨率。设计了迭代求解算法，给出了迭代初值的稳健算法，并将二维计算问题转化为一维计算问题，实现了方法的快速计算，同时大大地减少了存储量。文中给出了一维信号和遥感图像两个算例，计算结果表明，方法可以有效地改善图像的分辨率。     

铷光谱灯老化自动测试设备研制与应用

介绍了铷光谱灯老化自动测试设备的研制与应用,应用ATE技术实现了铷光谱灯的批量老化及长期自动测量,为筛选评估提供数据,解决了高性能铷原子钟的产品化研制和小型铷原子钟批量生产中的重要问题。系统功能完善、测量准确度高、软件界面清晰、操作简单,有效改进了铷原子钟研制生产的工艺水平,提高了研制生产过程的信息化程度。     

OBSCA谱相关分析器的实现研究

文章研究了一比特谱相关算法（OBSCA）,简化了相关运算环节,进一步研究了其数字实现方法,并设计了一种OBSCA高效并行实现方案,大大提高了谱相关函数的计算效率。     

Assessment of depth to magnetic sources using high resolution aeromagnetic data of some parts of the Lower Benue Trough and adjoining areas,Southeast Nigeria

High resolution airborne magnetic data acquired between 2005 and 2010 were used to determine depth to shallow and deep magnetic sources in some parts of Southeastern Nigeria. Various depth estimation methods such as standard Euler deconvolution (SED), source parameter imaging (SPI), spectral depth analysis (SDA) and two dimensional (2-D) forward modeling were applied. Results obtained from SED, SPI and models of profiles 1 and 2 indicate that the Abakaliki Anticlinorium (AA) and Ikom-Mamfe Rift (IMR) regions are dominated by short wavelength magnetic anomalies caused by extensive tectonic events. The SED map showed depth to shallow and deep magnetic sources ranging from ~ 16.6 to ~ 338.3 m and ~ 394.3 to ~ 5748.1 m respectively. Likewise, depth estimates from the SPI map varies from ~ 147.1 to ~ 554.2 m (shallow magnetic sources) and ~ 644.2 to ~ 6141.6 m (deep magnetic sources). The result obtained from SDA revealed depths to deep magnetic basement in the range of ~ 769 to ~ 6666 m with an average of ~ 3449 m. Also, it showed that depth to shallow magnetic sources vary between ~ 119 and ~ 434 m with mean of ~ 269 m. The 2-D forward modelling showed maximum depth values of ~ 4700, ~4600 and ~ 6500 m in the models of profiles 1, 2 and 3 within the Anambra Basin (AB), Afikpo Syncline (AS) and Calabar Flank (CF) respectively. Generally, from all the various methods applied the results indicate that AB, AS and CF are dominated by long wavelength anomalies. The 2-D models indicated that the basement framework is undulant. Also, depth estimates involving the various methods used in this study correlate strongly with each other in the AB, AS and CF geological regions.     

Impacts of the PAH size and the radiation intensity on the IR features of illuminated dust within the reflection nebulae

Interstellar dust grains are illuminated in the reflection nebulae. Under conditions of the PAH size and the intensity of the interstellar radiation field, we follow their impact on the PAH aromatic infrared bands using the numerical DustEM code. For a dust model consisting of PAH, amorphous C and amorphous silicate, the PAH size varies in a range from 0.31 to 4.9 nm while the radiation intensity varies by a scale factor from 0.1 to 10⁴. Various trends of the results show the effect of varying both the PAH size and the radiation intensity on the strength of the aromatic mid-IR bands. Through small PAH sizes less than 0.7 nm, the grain temperature distribution of PAHs shows a small variation within 2–3 K at low radiation intensity while it increases to 15 and 8 K for PAH⁰ and PAH⁺, respectively, at higher radiation intensity. In final the variability in these results reveals the evolution of the dust grains under the physical space conditions of the reflection nebulae. In the mid-IR region, the contributions of PAH⁰ and PAH⁺ in the total SED intensity agree with the proportions of these PAHs observed in some reflection nebulae having higher radiation intensities.     

Quality assessment of sub-Nyquist recovery from future gravity satellite missions

Drawing on experience from Gravity Recovery and Climate Experiment (GRACE) data analysis, the scientific challenges were already identified in several studies. Any future mission should focus on improvement in both precision and resolution in space and time. For future gravity missions which use high quality sensors, aliasing of high frequency time-variable geophysical signals to the lower frequency signals is one of the most serious problems. The aliasing problem and the spatio-temporal resolution are mainly restricted by two sampling theorems describing the space-time sampling of satellite missions: (i) a Heisenberg-like uncertainty theorem which states that the product of spatial resolution and time resolution is constant, and (ii) the Colombo–Nyquist rule (CNR), which requires the number of satellite revolutions in a repeat period to be at least twice a given maximum spherical harmonic degree. The CNR holds under the assumption of equal ground-track spacing, and limits the spatial resolution of the gravity solution.