基于粒子图像法的气枪喷嘴除法效率研究

倔枪喷嘴广泛地应用于工业除水除尘中，但如何直接量化衡量和评价气枪喷嘴的除尘效果或效率，是一个非常困难且有意义的问题。本文作者提出了通过图像处理的方式，利用除尘前后粒子的浓度同所反射的光强的相应关系来测算气枪喷嘴的除尘效率的方法。此法能有效地对全场表面的除尘效率分布进行较为精确的测算，且操作简便、可重复性强。利用该方法对影响气枪喷嘴除尘效率的多个因素；如一次侧压力、喷嘴到平板的距离和射流攻角进行了研     

月尘对登月服的影响及研究进展

概述了月尘对登月服带来的影响与危害,以及国外有关月尘对登月服影响研究的重点及最新进展,包括研究方向、研究内容、试验方法、环境模拟设备情况、试验评价体系、防尘与除尘技术等;特别针对月尘对登月服外层材料的影响,介绍了国外的研究发展情况及最新成果,提炼出了国外研究的总体思路逻辑框图,并对我国开展该领域技术研究提出了合理化建议。     

旋风式燃气过滤器的冷流实验和内流场模拟

为了考察某导弹系统燃气发生器的旋风式燃气过滤器的除尘特性，对其进行了冷流实验研究，对除尘效率进行了模拟测量，并应用多流体模型的IPSA算法对其内流场进行了三维两相的数值模拟。计算结果与实验结果较符合，计算得到的分离界限粒径为2μm--3μm。     

气力输送原理在吹砂除尘系统中的应用

为了提高吹砂作业自动化程度和工作效率,减轻工人劳动强度,改善通风除尘效能和工人劳动条件,我厂曾本着大胆尝试的态度,改变了以往吹吵除尘的一般设计方法,把气力输送原理运用到吹吵设备和通风除尘系统上来,设计试制出一种气力输送自动回砂除尘装置(图1),取的了较好的效果。     

电晕线布置方式对静电旋风除尘器除尘性能影响的研究

本文对静电旋风除尘器内部流场及浓度场分析的基础上，提出了电晕线靠近筒壁布置的构想，并通过实验证明，壁面布置方式大大提高了静电力的作用，提高了除尘性能，明显优于传统的中心布置电晕线方式，并从理论上给予了分析与探讨。     

软件故障树分析技术

介绍了在开发高可靠性软件系统中，软件故障树分析技术的概念、基本技术，给出了故障树的建造方法，并用一个简单的例子，介绍了软件故障树的应用。     

基于IPSec的VPN技术原理与实现

描述了VPN技术的基本原理以及IPSec规范，通过基本原理详细介绍了对数据包进行加密和认证原理。逐一介绍了IPSec主要协议，通过IPSec协议的论证说明了安全通信的原理，论证了VPN系统设计，在此基础上介绍了VPN技术的实现方法和几种典型应用方案。最后，作者对VPN技术的推广与应用提出了自己的看法。     

多目标跟踪（MTT）技术的发展

本文介绍了多目标跟踪（ＭＴＴ）技术的起源，发展概况和应用前景，还介绍了ＭＴＴ中主要技术的组成和现状。     

ADSL宽带接入网及其网络优化的几种方案探讨

ADSL技术作为实现宽带接入的解决方案，现阶段技术上已趋成熟，并在国内大多数机场得到应用，本文首先介绍了ADSL技术，然后阐述ADSL网络现状和发展情况，指出目前该网络拥塞状况，着重提出了几种网络优化方案，并对这几种方案进行了技术经济比较，最后简单探讨新建ADSL网络和介绍了ADSL技术的新发展ADSL2和ADSL2＋。     

机载设备校准技术的现状和发展

介绍了目前国内机载设备校准技术的基本现状，同时介绍了目前国际上较为普遍采用的先进的校准技术－－“零距离校准技术”。     

智能微尘技术的发展及应用

智能微尘是一种关于微型无线传感器的新兴技术.本文着重介绍了智能微尘技术的应用情况,并对目前存在的问题和发展趋势做了简要的叙述.     

The flux of interstellar dust observed by Ulysses and Galileo

Interstellar dust detected by the dust sensor onboard Ulysses was first identified after the Jupiter flyby when the spacecraft's trajectory changed dramatically (Grün et al., 1994). Here we report on two years of Ulysses post-Jupiter data covering the range of ecliptic latitudes from 0° to –54° and distances from 5.4 to 3.2 AU. We find that, over this time period, the flux of interstellar dust particles with a mean mass of 3·10^–13 g stays nearly constant at about 1·10^–4, m^–2 s^–1 ( sr)^–1, with both ecliptic latitude and heliocentric distance.Also presented are 20 months of measurements from the identical dust sensor onboard the Galileo spacecraft which moved along an in-ecliptic orbit from 1.0 to 4.2 AU. From the impact direction and speeds of the measured dust particles we conclude that Galileo almost certainly sensed interstellar dust outside 2.8 AU; interstellar particles may also account for part of the flux seen between 1 and 2.8 AU.     

Dust Environment Modelling of Comet 67P/Churyumov-Gerasimenko

Dust is an important constituent of cometary emission; its analysis is one of the major objectives of ESA’s Rosetta mission to comet 67P/Churyumov-Gerasimenko (C–G). Several instruments aboard Rosetta are dedicated to studying various aspects of dust in the cometary coma, all of which require a certain level of exposure to dust to achieve their goals. At the same time, impacts of dust particles can constitute a hazard to the spacecraft. To conciliate the demands of dust collection instruments and spacecraft safety, it is desirable to assess the dust environment in the coma even before the arrival of Rosetta. We describe the present status of modelling the dust coma of 67P/C–G and predict the speed and flux of dust in the coma, the dust fluence on a spacecraft along sample trajectories, and the radiation environment in the coma. The model will need to be refined when more details of the coma are revealed by observations. An overview of astronomical observations of 67P/C–G is given, because model parameters are derived from this data if possible. For quantities not yet measured for 67P/C–G, we use values obtained for other comets, e.g. concerning the optical and compositional properties of the dust grains. One of the most important and most controversial parameters is the dust mass distribution. We summarise the mass distribution functions derived from the in-situ measurements at comet 1P/Halley in 1986. For 67P/C–G, constraining the mass distribution is currently only possible by the analysis of astronomical images. We find that both the dust mass distribution and the time dependence of the dust production rate of 67P/C–G are those of a fairly typical comet.     

GEMS at the Galactic Cosmic-Ray Source

Galactic cosmic rays probably predominantly originate from shock-accelerated gas and dust in superbubbles. It is usually assumed that the shock-accelerated dust is quickly destroyed by sputtering. However, it may be that some of the dust can survive bombardment by the high-metallicity gas in the superbubble interior, and that some of that dust has been incorporated into solar system materials. Interplanetary dust particles (IDPs) contain enigmatic submicron components called GEMS (Glass with Embedded Metal and Sulfides). These GEMS have properties that closely match those expected of a population of surviving shock-accelerated dust at the GCR source (Westphal and Bradley in Astrophys. J. 617:1131, 2004). In order to test the hypothesis that GEMS are synthesized from shock-accelerated dust in superbubbles, we plan to measure the relative abundances of Fe, Zr, and Mo isotopes in GEMS using the new Resonance Ionization Mass Spectrometer at Argonne National Laboratory. If GEMS are synthesized from shock-accelerated dust in superbubbles, they should exhibit isotopic anomalies in Fe, Zr and Mo: specificially, enhancements in the r-only isotopes ⁹⁶Zr and ¹⁰⁰Mo, and separately in ⁵⁸Fe, should be observed. We review also recent developments in observations of GEMS, laboratory synthesis of GEMS-like materials, and implications of observations of GEMS-like materials in Stardust samples.     

Spatial distribution and orbital properties of interplanetary dust at high latitudes

Although the interplanetary dust cloud is assumed to be mainly concentrated in the ecliptic plane, there is a component of dust particles on highly inclined orbits that forms the out-of-ecliptic distribution. The ULYSSES mission for the first time makes this component accessible to in-situ, detection. Evidence for this dust component is also provided from the analysis of the Zodiacal light brightness and especially from the spherical shape of the solar F — corona. An obvious source for an out-of-ecliptic dust population is the activity of comets on high eccentric, highly inclined orbits. We discuss the dynamical conditions of particles under the influence of the radiation pressure when released from the comet and discuss their input to the dust cloud based on brightness analysis and in-situ results.     

The Cassini Cosmic Dust Analyzer

The Cassini-Huygens Cosmic Dust Analyzer (CDA) is intended to provide direct observations of dust grains with masses between 10⁻¹⁹ and 10⁻⁹ kg in interplanetary space and in the jovian and saturnian systems, to investigate their physical, chemical and dynamical properties as functions of the distances to the Sun, to Jupiter and to Saturn and its satellites and rings, to study their interaction with the saturnian rings, satellites and magnetosphere. Chemical composition of interplanetary meteoroids will be compared with asteroidal and cometary dust, as well as with Saturn dust, ejecta from rings and satellites. Ring and satellites phenomena which might be effects of meteoroid impacts will be compared with the interplanetary dust environment. Electrical charges of particulate matter in the magnetosphere and its consequences will be studied, e.g. the effects of the ambient plasma and the magnetic field on the trajectories of dust particles as well as fragmentation of particles due to electrostatic disruption.The investigation will be performed with an instrument that measures the mass, composition, electric charge, speed, and flight direction of individual dust particles. It is a highly reliable and versatile instrument with a mass sensitivity 10⁶ times higher than that of the Pioneer 10 and 11 dust detectors which measured dust in the saturnian system. The Cosmic Dust Analyzer has significant inheritance from former space instrumentation developed for the VEGA, Giotto, Galileo, and Ulysses missions. It will reliably measure impacts from as low as 1 impact per month up to 10⁴ impacts per second. The instrument weighs 17 kg and consumes 12 W, the integrated time-of-flight mass spectrometer has a mass resolution of up to 50. The nominal data transmission rate is 524 bits/s and varies between 50 and 4192 bps.This revised version was published online in July 2005 with a corrected cover date.     

管道相连泄爆容器中粉尘爆炸的实验研究

采用管道相连容器进行了工业规模的粉尘爆炸实验,目的是研究粮食粉尘在管道相连的加工和输送工业设备中发生粉尘爆炸时火焰和爆炸压力的传播过程及粉尘的Kst值对爆炸的影响。实验装置为一个气力输送系统,由两个不同体积的容器通过管道连接构成。采用粮食工业上具有代表性的两类粉尘进行了粉尘爆炸测试,爆炸从一个容器中通过管道传播到另一个容器中并引发了随后的二次爆炸,测试了不同位置的火焰和压力信号。实验结果表明：即使在起爆容器采取了泄爆措施,管道中没有粉尘喷入的情况下,粉尘爆炸火焰也可沿管道传播达30m并引发二次爆炸;随着粉尘爆炸指数的增大,初始爆炸的猛烈程度增强,火焰传播速度加快,二次爆炸的猛烈程度也随之增强。     

旋翼诱发砂尘环境及其对直升机的危害

 用直升机模型进行试验研究,制造了“直升机”在地面附近不同高度悬停及不同桨盘载荷下诱发砂尘环境,考察了旋翼诱发砂尘对直升机的实际危害,测定了某些指定部位的砂尘浓度与作用力及砂尘粒度分布情况。理论分析,计算了机身周围旋翼诱导流场,并经实验检验了直升机旋翼诱发砂尘浓度、粒度分布规律及作用力的近似估算方法。     

涡旋管砂尘分离效率计算方法

本文介绍了直升机发动机进气防砂装置核心元件-涡旋管的砂尘分离效率计算方法.在柱坐标系中推导出了砂尘在涡旋管中运动的三维动力学方程,并通过数值计算方法,成功地解决了砂尘在涡旋管中运动轨迹的求解问题,得出了涡旋管砂尘分离效率计算方法和计算结果,试验数据表明,该计算方法是可行的.     

粉尘爆炸与爆炸危险度评价

分析了粉尘爆炸的分类、条件、特性、因素、爆炸极限和最小点火能,重点介绍了粉尘爆炸的机理。在此基础上,采用Fuzzy评价的方法,建立了发生粉尘爆炸的危险度评价模型。