飞机复合材料修理中固化技术的探讨

对飞机复合材料固化工艺中热固化、微波固化、电子束固化、紫外光固化等技术的机理和研究现状进行了分析对比。     

高精度紫外探测器定标测试方法

文章研究分析了紫外电学定标探测器的主要光电不等效因素,并建立了基于紫外电学定标探测器的紫外辐射定标系统。在此基础上,利用紫外探测器定标测试平台,开展了紫外探测器的测试方法研究,响应率定标的总不确定度为3%～5%,相对光谱测试的总不确定度为3%。     

Method of the HF wave absorption evaluation based on GIRO network data

High frequency (HF) communication is strongly dependent on the state of the ionosphere, which specifies the mode structure of the radio wave propagating in ionosphere. Another core factor defining the strength of the HF signal at the receiving site is the ionospheric absorption. Accurate modelling the effect of absorption is an essential part of many studies of the HF propagation in the ionosphere.This paper proposes a method for estimating the absorption. The method is based on analysis of vertical sounding ionograms. The main idea of the approach is to compare the main parameters retrieved from measured and simulated ionograms. The combination of Global Ionospheric Radio Observatory (GIRO, http://giro.uml.edu) data and ionograms modelling allows for developing the empiric absorption model available at near real-time. The ionogram simulation taking into account absorption utilizes the NIM-RT (North Ionospheric Model and Ray Tracing) software. As a result, the proposed technique provides more reliable and accurate evaluation of minimum frequency at which echoes are observed in vertical incidence ionosonde soundings. The values of these frequencies should be used in the following simulation to optimize parameters in the empirical formulae for defining absorption HF wave in ionosphere.The ultimate objective of this work is the designing the method, which allows the simulating of HF radio channel accounting for regular absorption due to UV radiation of the Sun. Eventually it could be considered as some kind of the HF propagation forecasting.     

光固化巯基-乙烯基硅氮烷陶瓷前驱体制备氮化硅陶瓷

以不同用量的多官能巯基化合物与乙烯基硅氮烷预聚物组成液态光固化体系,经紫外光辐照后固化成聚合物陶瓷前驱体,后经1400℃无压热裂解制备氮化硅。采用热失重（TGA）分析陶瓷前驱体的热解特性,X射线衍射（XRD）分析热解后材料的相组成及晶态结构,场发射枪扫描电子显微镜（SEM）观察和表征材料的微观形貌。陶瓷前驱体在热解过程中分别在325—350℃和475—505℃出现两个失重峰,随着体系中巯基化合物含量的增加,前驱体的热解失重率增加,陶瓷收率降低,最终陶瓷的相对密度下降,结晶度增高,晶粒尺寸增大。经1400℃热解15h,得到部分α-Si3N4晶体;热解24h,得到大量α-Si3N4和少量β-Si3N4的材料,在空洞中发现富氮的细长纤状和片状晶体。     

通量限制器与LED性质、空间离散精度

本文从标量形式的ＵＳＬＩＰ格式出发,从理论上分析了通量限制器与ＬＥＤ性质和空间离散精度的关系。利用Ｒｏｅ平均矩阵的Ｕ特性和广义数值Ｒｉｅｍａｎｎ不变量的概念,将此类格式应用于二维翼型跨声流场的数值模拟,针对提供的来流条件,考查了不同的通量限制器对流场计算精度的影响。     

紫外辐照下透明聚氨酯胶片老化机理

针对高端夹层玻璃的老化问题,选用荧光紫外灯,对其主要粘结材料——透明聚氨酯胶片分别进行0/200/300/500 h的照射,借助紫外/可见光分光光度计、傅里叶红外光谱仪、扫描电镜等设备,研究照射过程中材料颜色、结构、微观形貌的变化。扫描电镜显示照射时间延长到500 h,材料表面出现龟裂。实验发现胶片的老化起始于硬段及软段部位与N,O相连的α位置的碳原子,在紫外光及氧气的联合作用下产生氢过氧化物;该过氧化合物一部分继续氧化成CO,一部分通过β分裂,使C—N,C—O键断裂,致使材料龟裂。     

基于MPS4021的20W LED驱动电源设计

采用原边反馈方案设计出一款20W LED驱动电源,通过变压器初次级隔离省去了副边反馈电路,提高了驱动电源的安全性和可靠性,并节约了BOM成本。所设计的驱动电源实现了在全电压范围内输出电流精度达±5%、功率因数大于0.9、效率大于85%,使用寿命大于3万小时,电磁干扰符合EN55015限制要求,并且具备有过流保护和过压保护功能,对设计大功率LED驱动电源具有一定的参考价值。     

Study of a Coronal Mass Ejection with SOHO/UVCS and STEREO data

We study the 3-D kinematics of a Coronal Mass Ejection (CME) using data acquired by the LASCO C2 and UVCS instruments on board SOHO, and the COR1 coronagraphs and EUVI telescopes on board STEREO. The event, which occurred on May 20, 2007, was a partial-halo CME associated with a prominence eruption. This is the first CME studied with UVCS data that occurred in the STEREO era. The longitudinal angle between the STEREO spacecrafts was ∼7.7° at that time, and this allowed us to reconstruct via triangulation technique the 3-D trajectory of the erupting prominence observed by STEREO/EUVI. Information on the 3-D expansion of the CME provided by STEREO/COR1 data have been combined with spectroscopic observations by SOHO/UVCS. First results presented here show that line-of-sight velocities derived from spectroscopic data are not fully in agreement with those previously derived via triangulation technique, thus pointing out possible limitations of this technique.     

Simulated observations of the electron coronal density irregularity\overline {n^2 } /(\bar n)^2

A technique to derive the coronal density irregularity factor , wheren is the electron density, has been proposed by Fineschi and Romoli (1993). This technique will exploit the unique UVCS capability of cotemporal and cospatial measurements of both UV line radiation and K-coronal polarized brightness,pB.The ratio of the measured H I Lyman (Ly-) line intensity to the resonant-scattering dominated H I Lyman (Ly-) intensity can be used to extract the collisional component of the Ly-. This component yields an estimate of . The quantity is then obtained from the UVCS white-light K-coronal measurements.We present simulated observations of the UVCS for coronal atmosphere models with different filling factors and electron density profiles, and for different coronal structures (e.g., coronal holes, streamers). These simulations will show how the proposed technique may be used to probe inhomogeneities of the solar corona.     

Ultraviolet spectroscopy of the extended solar corona during the Spartan 201 mission

The instruments on the Spartan 201 spacecraft are an Ultraviolet Coronal Spectrometer and a White Light Coronagraph. Spartan 201 was deployed by the Space Shuttle on 11 April 1993 and observed the extended solar corona for about 40 hours. The Ultraviolet Coronal Spectrometer measured the intensity and spectral line profile of HI Ly and the intensities of OVI 103.2 and 103.7 nm. Observations were made at heliocentric heights between 1.39 and 3.5 R. Four coronal targets were observed, a helmet streamer at heliographic position angle 135°, the north and south polar coronal holes, and an active region above the west limb. Measurements of the HI Ly geocorona and the solar irradiance were also made. The instrument performed as expected. Straylight suppression, spectral focus, radiometric sensitivity and background levels all appear to be satisfactory. The uv observations are aimed at determining proton temperatures and outflow velocities of hydrogen, protons and oxygen ions. Preliminary results from the north polar coronal hole observations are discussed.