无线电引信抗海杂波干扰方法

无线电引信抗海杂波的能力决定了舰空导弹无线电引信低空和超低空工作性能,针对海杂波对无线电引信的影响,分析了海面回波的平均功率、海面散射系数、海杂波的多普勒频谱等海杂波特性,提出了无线电引信抗海杂波干扰方法。     

超宽带射频仿真系统中的低RCS三轴转台设计

提出了在超宽带射频仿真系统中三轴转台的低RCS设计方法.该方法采用转台机械结构设计、低RCS外形优化分析与测试测量相结合的方式.首先基于低RCS要求及三轴转台的结构特性,对其进行外形优化.通过计算三轴转台的表面感应电流分布,分析三轴转台的强散射区域,并选取相应吸波材料及涂敷方法对三轴转台进行处理.实际测量表明,涂敷吸波材料后三轴转台散射回波幅度显著减小,分布均匀,达到了预设的效果.     

X-ray and radio observations of the galaxy cluster 3C 129

The galaxy cluster 3C 129 contains two radio galaxies, the prototypical head tail radio galaxy 3C 129 and the weaker radio galaxy 3C 129.1. The tail of the first radio galaxy extends over more than 15′ across the sky. In this paper, we report on Chandra spectroscopy observations of the galaxy cluster, complemented by new and archival radio data taken with the Very Large Array (VLA) at 0.33, 1.4, 5, and 8 GHz and by HI-observations performed with the dominion radio astrophysical observatory (DRAO). We describe the Chandra results on the properties of the Intra-Cluster Medium (ICM) and discuss extended X-ray emission detected from the host galaxy of the radio galaxy 3C 129.1 and from the inner jet of the radio galaxy 3C 129. Finally, we report on the results of an ICM/radio plasma pressure balance study along the tail of the radio galaxy 3C 129.     

光学加工射频离子源的去除函数与稳定性研究

在研究了射频离子源的结构、工作原理和性能的基础上,进行了光学镜面抛光离子束的去除效率与稳定性测试。实验结果表明射频离子源去除函数的形状为回转高斯形,利用Φ15mm的栅网,在靶距为30mm、离子能量900eV时,去除函数的峰值去除率为194nm/min,体积去除率为19.2×10-3mm3/min,半峰全宽值为9.2mm;并且去除函数的峰值去除率与体积去除率的变化均在3%以内,半峰全宽值的变化在1.7%以内。因此,射频离子源具有光学镜面抛光加工所需的去除效率,而且射频离子源具有好的稳定性,具备光学加工的潜能。     

Non-Gaussian clutter characterization applied to OTHR using a mixture of two Rayleigh probability density functions

A practical technique for characterizing non-Gaussian radar clutter is specified and demonstrated using Over The Horizon Radar (OTHR) data, as an example. The technique employs maximum likelihood to fit the probability density of the clutter amplitude returns to a mixture of two Rayleigh probability densities instead of the single Rayleigh density typically used for Gaussian clutter. This model for non-Gaussian clutter is fully specified for any set of clutter amplitudes by a log likelihood, two Rayleigh parameters, and a mixing coefficient. A 3D plot of these values yields an easily-visualized clutter characterization, as is illustrated using OTHR data. This technique is a demonstration of clutter characterization using OTHR data, but the method can be applied to characterize other types of clutter data.     

民用无线电发射信号对电磁环境的影响

对世界范围内的典型民用无线电业务进行了归纳分析,在空域、时域、频域和能量域等详细参数计算的基础上,分析了民用发射信号对电磁环境中电子设备接收机的影响,并提出了多种建议方法以最大限度地减小民用发射信号对电子设备系统设计的影响。     

雷达射频掩护信号分析及对抗方法研究

为提高抗干扰能力,雷达采用射频掩护信号对抗有源干扰机.分析射频掩护信号的产生机理和工作波形,以及射频掩护信号对雷达有源干扰机中测频接收机、信号处理机、数字射频存储器及脉冲行波管发射机的影响,从而给出雷达有源干扰机对抗射频掩护信号的方法.     

浅谈奥米加导航系统的位置误差

奥米加导航系统是一种全球性导航系统.在一般天气条件下,该系统具有良好的导航性能,但是在复杂天气条件下,也暴露出了一些缺点或不足。本文针对使用中出现的问题,根据其工作特性、信号格式、信息处理、定位计算,误差处理方式进行一些理论分析,并对改进系统操作进行一些探索。     

Measurements of the 12C/13C Ratio in Planetary Nebulae and Implications for Stellar Evolution

We present the results of a study aimed at determining the 12C/13C ratio in two samples of planetary nebulae (PNe) by means of mm-wave observations of 12CO and 13CO. The first group includes six PNe which have been observed in the 3He+ hyperfine transition; the other group consists of 23 nebulae with rich molecular envelopes. We have determined the isotopic ratio in 14 objects and the results indicate a range of values between 9 and 23. In particular, three PNe have ratios well below the value predicted by standard evolutionary models ( 20), indicating that some extra-mixing process has occurred in these stars. We briefly discuss the implications of our results for standard and nonstandard stellar nucleosynthesis.     

Particle Acceleration by the Sun: Electrons, Hard X-rays/Gamma-rays

Observations of hard X-ray (HXR)/γ-ray continuum and γ-ray lines produced by energetic electrons and ions, respectively, colliding with the solar atmosphere, have shown that large solar flares can accelerate ions up to many GeV and electrons up to hundreds of MeV. Solar energetic particles (SEPs) are observed by spacecraft near 1 AU and by ground-based instrumentation to extend up to similar energies, but it appears that a different acceleration process, one associated with fast Coronal Mass Ejections (CMEs) is responsible. Much weaker SEP events are observed that are generally rich in electrons, ³He, and heavy elements. The energetic particles in these events appear to be similar to those accelerated in flares. The Ramaty High Energy Solar Spectroscopic Imager (RHESSI) mission provides high-resolution spectroscopy and imaging of flare HXRs and γ-rays. The observations of the location, energy spectra, and composition of the flare accelerated energetic particles at the Sun strongly imply that the acceleration is closely related to the magnetic reconnection that releases the energy in solar flares. Here preliminary comparisons of the RHESSI observations with observations of both energetic electrons and ions near 1 AU are reviewed, and the implications for the particle acceleration and escape processes are discussed.