数字化干涉仪测角技术

数字化干涉仪测角采用的是高精度数字鉴相技术，该技术与传统的模拟鉴相技术相比可以大幅度提高鉴相精度，从而满足高精度干涉仪测角的要求。基于数字干涉仪鉴相算法，通过两路正交本振信号分别与两路待测相信号相乘，使用CIC 滤波器除乘积中的高频信号，最后通过CORDIC 算法计算出相位差。经过干涉仪测角模拟器上测试结果表明，其数字鉴相误差小于0.2°。     

三维曲面测量新方法：半球头测量法

提出的半球头测量法从理论上消除了三维曲面截形测量时由于被测曲面的扭曲对测头所造成的干涉,使曲面测量直接转化为曲线测量,从而简化了测量和数据处理过程,为曲面测量提供了一种既简便实用又具有较高精度的新方法。     

Structure and development of quiet loops in the solar corona

X-ray emission from solar coronal loops changes on two different timescales: a) flare loops and transient active region brightenings show a rapid variability, b) quiet region loops are quasi-steady and change only slowly with time. This different time behavior has been analyzed on the basis of Yohkoh SXT observations and we report here on the results from our analysis, mainly focussing on quiet loop variability.     

海防导弹主发动机的安装与测量

论述了某海防导弹主地发动机安装测量的意义和作用。介绍了发动机安装测量步骤，公差确定和分配，安装曲线制作依据和实际使用情况。     

非线性编辑在电视节目制作中的应用

以DY-3000型非线性编辑系统的应用实践出发，论述了非线性编辑的特点及在实际工作中的应用，同时指出了它的不足及今后的发展趋势。     

微弱电信号检测技术

主要介绍微弱电压信号和电流产生的主要因素及其测量方法，指出在精密测量过程中需要注意的一些问题：如接地、屏蔽和抗干扰等。     

On the optical variability of a be star,HDE 245770, — the optical counterpart of the transient X-ray pulsar A0535+26

Photoelectric WBVR observations of Be star HDE 245770=V 725 Tau, the optical counterpart of the transient X-ray pulsar A0535+26, having a pulse period of about 104 s, were conducted for more than 10 years. An irregular long-term optical variability of the star with amplitudes of the order of a few tenths of magnitude was found to be a usual phenomenon. In some cases rapid changes of the star's optical luminosity with a characteristic period of a few tens of minutes or a few hours, and an amplitude of several hundredths of magnitude in all the spectral bands used, which have practically coincided or correlated with the X-ray pulsar outbursts detected by X-ray satellites, were observed.Photoelectric recording of the optical flux from HDE 245770 were made in 1981–1982 with a time resolution of 1 second and 10 s, respectively, in theR spectral band (₀ 7000 Å) and in the narrowH -emission-line band (_1/2 75 Å) using a 48-cm reflector of High-Mountain Tien-Shan observatory of the Sternberg Astronomical Institute near Alma-Ata. An analysis of autocorrelation functions of the flux changes from object under study and a comparison with the star BD+26° 876 indicated the variability of luminosity of V 725 Tau in theR spectral band on a time scale of a few tens of second; this variability resembles shot noise with a characteristic time of stochastic bursts of about 15–20 s and their amplitudes of about a few tenths of a percent. InH -emission-line radiation autocorrelation functions and power spectra show quasiperiodic variability of luminosity of HDE 245770 with a characteristic period of about 100–150 s and an amplitude in the neighbour-hood of 0.5%. The latter result is not quite reliable because of not quite fine weather conditions during the observations; independent observations and check-up are required.     

星间二维光CDMA系统方案及性能分析

为了充分利用星间光通信的丰富带宽，提出并设计了星间二维光CDMA系统方案。考虑背景光、多用户干扰、APD接收机噪声及热噪声，给出了星间二维光CDMA通信系统的系统模型。采用数值分析的方法，分析了该通信系统的误码率性能。结果表明：星间二维光CDMA通信系统易受多用户干扰、码速率以及背景光等因素的影响；通过合理的设计各种参数，在星间二维光CDMA通信系统中可以获得多用户、高数据速率的通信性能。     

卫星多源遥感图像融合研究

卫星多源遥感图像融合技术可以综合利用多源信息,从而获得对同一目标更全面、更清晰、更准确的认识。文中简介卫星多源遥感图像融合系统所包含的三个过程,即预处理、图像融合、综合评价及应用;详细分析像素层、特征层和决策层三个不同融合层次的融合原理和方法;归纳融合效果的主客观评价标准和熵、平均梯度等六种评价指标;最后从空间配准模型、建立统一的数学融合模型、关联的二义性、数据融合方法与融合系统实施存在的问题、有效的评价准则等方面讨论了卫星多源遥感图像融合目前存在的问题,并对今后的发展趋势作出展望。     

图象的分形压缩方法

本文介绍一种适于对高分辨率（大数据量）遥感图象实现高倍（几十至几百倍）压缩的方法。文中简述分形几何的基本概念，给出了一种分形压缩的模型，以北航的图象分形压缩研究结果为例，阐述了分形压缩方法的特点。