Modeling of Ground Deformation and Shallow Surface Waves Generated by Martian Dust Devils and Perspectives for Near-Surface Structure Inversion

We investigated the possible seismic signatures of dust devils on Mars, both at long and short period, based on the analysis of Earth data and on forward modeling for Mars. Seismic and meteorological data collected in the Mojave Desert, California, recorded the signals generated by dust devils. In the 10–100 s band, the quasi-static surface deformation triggered by pressure fluctuations resulted in detectable ground-tilt effects: these are in good agreement with our modeling based on Sorrells’ theory. In addition, high-frequency records also exhibit a significant excitation in correspondence to dust devil episodes. Besides wind noise, this signal includes shallow surface waves due to the atmosphere-surface coupling and is used for a preliminary inversion of the near-surface S-wave profile down to 50 m depth. In the case of Mars, we modeled the long-period signals generated by the pressure field resulting from turbulence-resolving Large-Eddy Simulations. For typical dust-devil-like vortices with pressure drops of a couple Pascals, the corresponding horizontal acceleration is of a few nm/s² for rocky subsurface models and reaches 10–20 nm/s² for weak regolith models. In both cases, this signal can be detected by the Very-Broad Band seismometers of the InSight/SEIS experiment up to a distance of a few hundred meters from the vortex, the amplitude of the signal decreasing as the inverse of the distance. Atmospheric vortices are thus expected to be detected at the InSight landing site; the analysis of their seismic and atmospheric signals could lead to additional constraints on the near-surface structure, more precisely on the ground compliance and possibly on the seismic velocities.     

Michelson Interferometer for Global High-Resolution Thermospheric Imaging (MIGHTI): Monolithic Interferometer Design and Test

The design and laboratory tests of the interferometers for the Michelson Interferometer for Global High-resolution Thermospheric Imaging (MIGHTI) instrument which measures thermospheric wind and temperature for the NASA-sponsored Ionospheric Connection (ICON) Explorer mission are described. The monolithic interferometers use the Doppler Asymmetric Spatial Heterodyne (DASH) Spectroscopy technique for wind measurements and a multi-element photometer approach to measure thermospheric temperatures. The DASH technique and overall optical design of the MIGHTI instrument are described in an overview followed by details on the design, element fabrication, assembly, laboratory tests and thermal control of the interferometers that are the heart of MIGHTI.     

Michelson Interferometer for Global High-Resolution Thermospheric Imaging (MIGHTI): Instrument Design and Calibration

The Michelson Interferometer for Global High-resolution Thermospheric Imaging (MIGHTI) instrument was built for launch and operation on the NASA Ionospheric Connection Explorer (ICON) mission. The instrument was designed to measure thermospheric horizontal wind velocity profiles and thermospheric temperature in altitude regions between 90 km and 300 km, during day and night. For the wind measurements it uses two perpendicular fields of view pointed at the Earth’s limb, observing the Doppler shift of the atomic oxygen red and green lines at 630.0 nm and 557.7 nm wavelength. The wavelength shift is measured using field-widened, temperature compensated Doppler Asymmetric Spatial Heterodyne (DASH) spectrometers, employing low order échelle gratings operating at two different orders for the different atmospheric lines. The temperature measurement is accomplished by a multichannel photometric measurement of the spectral shape of the molecular oxygen A-band around 762 nm wavelength. For each field of view, the signals of the two oxygen lines and the A-band are detected on different regions of a single, cooled, frame transfer charge coupled device (CCD) detector. On-board calibration sources are used to periodically quantify thermal drifts, simultaneously with observing the atmosphere. The MIGHTI requirements, the resulting instrument design and the calibration are described.     

基于随机减量的运行模态频域分析方法

以高层建筑、大跨桥梁等难以进行人工激励的大型复杂结构为对象,提出并实现了一种基于随机减量技术和复模态指示因子函数法的新型频域运行状态模态参数识别方法.由随机运行响应估计随机减量函数,然后通过时频域变换得到频域的半功率谱密度函数,并用复模态指示因子函数法从半功率谱密度函数中识别结构模态参数.最后对1个三维空间结构模型进行算法验证,得到相应的各阶模态参数,证明了将随机减量技术和复模态指示因子函数法相结合的方法识别大型结构模态参数的有效性和合理性.     

型号标准化文件体系的建立与管理

概述型号标准化文件体系的内涵、特点、作用以及文件体系的组成,阐明型号标准化文件体系与企业标准体系以及型号文件系统的关系.介绍型号标准化文件体系的运行与管理.     

舰载导弹红外射频导引头电磁兼容设计

采用分层与综合设计法对舰载战术导弹导引头的有源器件选型,印制板、接地、屏蔽、滤波和瞬态骚扰抑制等电磁兼容（EMC）设计进行了研究。分析了各层次传导和辐射的电磁兼容性,给出了设计策略及某导引头壳体电子设计与仿真结果。研究对改善整个导引头的电磁兼容性设计有一定的参考价值。     

大型稀疏线性方程组改进的ICCG方法

有限元分析求解的大型线性方程组．其系数矩阵中只有少量的元素不为零，是一个稀疏矩阵，而且一般都是对称的。求解过程中只存贮对称部分的非零元素，这种全稀疏存贮策略采用链表式管理，使存贮结构可以动态更改。在带双门槛值ICCG方法的基础上加上对角元修正策略，产生了一种改进的ICCG求解法，它不仅节省了存贮空间，而且便于元素的查询、插入和删除，提高了求解效率。这里也给出了验证算例。     

基于BLUE的多窗口谱估计

文章提出了一种基于BLUE的多窗口功率谱估计算法。该算法是在无偏估计的约束条件下，使其方差最小化而得到的特征谱的最佳线性组合。通过仿真实例分析得到，与自适应的MTM相比，该算法的计算量大大减小了。由于正弦窗具有解析的表达式，不需要进行特征值分解，并且有良好的统计性能，因此，使用正弦窗的MTM可以进一步降低计算量并改善估计性能。     

2边连通3正则平面图的边着色

对具有正常３边着色的２边连通３正则平面图的顶点定义了方向，并且在这样的图上建立了路径上的积分，进一步给出了２边连通３正则平面图是３边可着色的等价条件。     

High-energy gamma radiation of solar flares as an indicator of acceleration of energetic protons

Using the SONG detector onboard the CORONAS-F satellite, gamma-ray emission of high energies (>100 MeV) was recorded during four solar flares. In the sequential spectra of gamma rays the peculiarity caused by generation and decay of neutral pions was isolated, which made it possible to determine with a high accuracy the moments of appearance in the solar atmosphere of protons accelerated up to energies above 300 MeV.