齿轮箱中滚动轴承的故障诊断

提出了一种基于自适应除噪技术(ANC)和共振解调技术(DRT)的齿轮箱中滚动轴承的故障诊断方法。该方法先后用同一传感器和测量系统、在同一位置采集被诊断轴承在无故障时的振动信号和在状态监测过程中的振动信号,然后把这两次拾取的信号分别作为自适应除噪系统的参考输入和主输入进行除噪处理,最后用共振解调技术对除噪后的振动信号进行包络解调,实现齿轮箱中滚动轴承的故障诊断。实际应用表明,该方法能够从齿轮箱振动信号中剔除齿轮啮合振动等背景噪声,提高滚动轴承振动信号的信噪比,可以有效地诊断齿轮箱中滚动轴承的故障。      

解决有效性与公平性的一种TCP拥塞控制算法

提出了显式通告分队列服务算法,用以解决低业务量用户相对高业务量用户对带宽占有的不公平性和传输效率比较低的问题。该算法中,源端和路由器在接收到包含业务类型(高/低业务量)、传输开始或者传输结束等控制信息时,把高/低业务量用户的数据分配到具有相应服务速率的队列中,或者将传输结束但仍占有相应服务速率的空闲队列合并到非空闲队列,增加非空闲队列的服务速率,这样在保护低业务量用户对带宽共享的公平性的同时,提高了带宽的利用率,即传输效率,从而提高了网络的性能。     

CBERS-1卫星红外多光谱扫描仪分系统简介

文章介绍了CBERS -1卫星红外多光谱扫描仪 (IRMSS)分系统的主要性能和基本组成     

SAR图像目标峰值特征提取与方位角估计方法研究

目标峰值特征是SAR图像目标识别的重要特征之一。峰值特征提取是SAR图像目标识别的一个重要步骤，为了由SAR图像快速、精确地提取目标峰值特征．本文首先研究了SAR图像目标峰值特征提取方法，提出了一种“子像素”级精度的SAR图像目标峰值特征提取方法．并通过仿真实验分析了峰值位置、峰值幅度的估计精度。由于目标SAR图像或SAR图像特征矢量对目标方位角变化的敏感性，因此，为了提高SAR图像目标识别系统的分类效率，本文还研究了SAR图像目标方位角估计方法，提出了一种利用峰值特征基于线性回归的sAR目标方位角估计方法，和现有方法相比，该方法除了计算速度快，估计精度较高之外，还能在估计方位角的同时，给出该估计的置信区间，从而更好的满足SAR ATR的实际需要。文中通过对大量实测MSTAR SAR图像目标方位角的估计实验，验证了本文目标峰值特征提取及方位角估计方法的有效性。     

热处理对PBO纤维分子链结构和性能的影响

利用红外光谱分析(FTIR)、示差扫描量热法(DSC)和磷含量分析方法研究了热处理对PBO纤维结构和性能的影响。结果表明,热处理使PBO纤维分子链中聚合后期少量的未关环反应趋向完全,使得PBO分子的共轭链长增加,弱键消失,提高了PBO纤维的力学性能;提高了分子链与链之间排列的有序性,使链与链之间堆砌更加紧密,使得热处理后的纤维较难溶于MSA中;热处理使PBO纤维表面化学组成发生变化,并使其表面粗糙化,能改善其表面润湿性能;热处理对纤维强度影响甚微,提高热处理温度、延长热处理时间和增大热处理张力,能提高PBO纤维的模量。     

基于FPGA的M位并行分布式算法的FIR滤波器设计

介绍基于查找表结构的分布式算法的基本原理,提出M位并行分布式算法的实现方法。以2位并行分布式算法结构的FIR滤波器设计为例,在Altera Cyclone系列芯片上实现32阶12位FIR滤波器,并对其性能和资源占用进行分析。     

Integral inversion of GRAIL inter-satellite gravitational accelerations for regional recovery of the lunar gravitational field

We present an integral-based approach for high-resolution regional recovery of the gravitational field in this article. We derive rigorous remove-compute-restore integral estimators relating the line-of-sight gravitational acceleration to an arbitrary order radial derivative of the gravitational potential. The integral estimators are composed of three terms, i.e., the truncated integration, the low-frequency line-of-sight gravitational acceleration, and the high-frequency truncation error (effect of the distant zones). We test the accuracy of the integral transformations and of the integral estimators in a closed-loop simulation over the Montes Jura region on the nearside of the Moon. In this way, we determine optimal sizes of integration radii and grid discretisation. In addition, we investigate the performance of the regional integral inversion with synthetic and realistic GRAIL observations. We demonstrate that the regional inversion results of the disturbing gravitational potential and its first order radial derivative in the Montes Jura mountain range are less contaminated by high-frequency noise than the global spherical harmonic models.     

Study of hot flow anomalies using Cluster multi-spacecraft measurements

Hot flow anomalies (HFAs) were first discovered in the early 1980s at the bow shock of the Earth. In the 1990s these features were studied, observed and simulated very intensively and many new missions (Cluster, THEMIS, Cassini and Venus Express) focused the attention to this phenomenon again. Many basic features and the HFA formation mechanism were clarified observationally and using hybrid simulation techniques. We described previous observational, theoretical and simulation results in the research field of HFAs. We introduced HFA observations performed at the Earth, Mars, Venus and Saturn in this paper. We share different observation results of space mission to give an overview to the reader.     

Model of a fluxtube with a twisted magnetic field in the stratified solar atmosphere

We build a single vertical straight magnetic fluxtube spanning the solar photosphere and the transition region which does not expand with height. We assume that the fluxtube containing twisted magnetic fields is in magnetohydrostatic equilibrium within a realistic stratified atmosphere subject to solar gravity. Incorporating specific forms of current density and gas pressure in the Grad–Shafranov equation, we solve the magnetic flux function, and find it to be separable with a Coulomb wave function in radial direction while the vertical part of the solution decreases exponentially. We employ improved fluxtube boundary conditions and take a realistic ambient external pressure for the photosphere to transition region, to derive a family of solutions for reasonable values of the fluxtube radius and magnetic field strength at the base of the axis that are the free parameters in our model. We find that our model estimates are consistent with the magnetic field strength and the radii of Magnetic bright points (MBPs) as estimated from observations. We also derive thermodynamic quantities inside the fluxtube.     

A topside investigation over a mid-latitude digisonde station in Cyprus

We examine the systematic differences between topside electron density measurements recorded by different techniques over the low-middle latitude operating European station in Nicosia, Cyprus (geographical coordinates: 35.14^oN, 33.2^oE), (magnetic coordinates 31.86^oN, 111.83 ^oE). These techniques include space-based in-situ data by Langmuir probes on board.European Space Agency (ESA) Swarm satellites, radio occultation measurements on board low Earth orbit (LEO) satellites from the COSMIC/FORMOSAT-3 mission and ground-based extrapolated topside electron density profiles from manually scaled ionograms. The measurements are also compared with International Reference Ionosphere Model (IRI-2016) topside estimations and IRI-corrected NeQuick topside formulation (method proposed by Pezzopane and Pignalberi (2019)). The comparison of Swarm and COSMIC observations with digisonde and IRI estimations verifies that in the majority of cases digisonde underestimates while IRI overestimates Swarm observations but in general, IRI provides a better topside representation than the digisonde. For COSMIC and digisonde profiles matched at the F layer peak the digisonde systematically underestimates topside COSMIC electron density values and the relative difference between COSMIC and digisonde increases with altitude (above hmF2), while IRI overestimates the topside COSMIC electron density but after a certain altitude (~150 km above hmF2) this overestimation starts to decrease with altitude. The IRI-corrected NeQuick underestimates the majority of topside COSMIC electron density profiles and relative difference is lower up to approximately 100 km (above the hmF2) and then it increases. The overall performance of IRI-corrected NeQuick improves with respect to IRI and digisonde.