深空探测中的激光诱导击穿光谱探测仪

物质成分探测是深空探测领域非常重要的技术领域,激光诱导击穿光谱技术是一种可以非接触式快速获得物质元素成分信息的手段,论文针对2020年我国首次火星探测任务提出的火星表面成分探测仪,阐述了激光诱导击穿光谱技术基本原理,国内外的技术发展现状和趋势,重点围绕火星环境、有效载荷生存性进行了分析,最后论文详细探讨了激光诱导击穿光谱技术中的数据反演和定量化技术。     

基于Web Services的并联机床制造服务系统

针对并联机床加工曲面零件的优势与目前并联机床未得到广泛应用之间的矛盾,开发了并联机床的制造服务系统。该系统将并联机床原有制造系统中的后置处理功能封装成Web services,包括编译、工作空间计算、干涉校验和运动学变换,应用面向服务的架构使并联机床的制造服务与异地制造企业协同工作,并给出了此架构下该系统的工作流程和功能模块。实例说明,应用Web services和面向服务架构的制造服务系统与传统的分布式系统相比,具有易集成性、松耦合性及易操作性,可以为企业减少成本、提高效率。     

一种扩展了价格信息的进程代数

针对目前进程代数缺乏成本建模和分析能力的现状,提出一种扩展了价格信息的进程代数(Price process algebra,PPA).在传值通信系统演算(Calculus of communication systems,CCS)基础上为进程动作和状态扩展价格函数,使用价格迁移系统给出PPA的语义,证明PPA的进程状态扩展累计成本的合理性和完备性,给出构造状态空间的算法并证明该算法的有效性,实例分析说明PPA用于成本建模和分析的可行性.     

地方院校数字图书馆定制化服务建设构想

通过分析数字图书馆定制化、个性化服务的几种方式,探讨地方院校建设数字图书馆定制化功能,提出从信息内容和技术趋势上进行相适应的数字图书馆定制化服务建设构想和建议,促进数字图书馆定制化服务对地方院校的发展。     

基于Web的通用商品报价系统的研究与实现

本文对国内企业现有的商品报价系统的现状进行了分析,并且对现有的商品报价系统进行研究和改进,阐述了基于Web的通用商品报价系统的系统构架及主要功能.     

非叠氮燃气发生剂配方研制进展

介绍了国内外非叠氮燃气发生剂的研制进展。对出现的四唑类、胍类、铝热剂类等非叠氮配方的高氮化合物燃料、氧化剂、黏合剂、工艺助剂等特点和发展做了总结和讨论,指出非叠氮高氮化合物有无毒、燃速范围宽、产气量大、燃温低等优点,正在取代叠氮配方燃气发生剂,得到广泛应用。     

基于多目标决策模型的两栖攻击舰编队编成研究

两栖攻击舰编队编成不能照搬固定的模式,而应根据作战任务和威胁等因素进行合理配置。文章分析了两栖攻击舰编队的作战能力,并在此基础上构建了编成模型的指标体系。运用多目标决策理论,建立了两栖攻击舰编队编成的模型,通过计算得到了针对某作战行动中两栖攻击舰编队的最优编成方案,并将所得到的结果与日常性建制的编队编成进行了比较。     

利用BPMS实现CRP/VMI

当前在市场全球化环境下,需要企业生产多品种少批量产品、缩短订货到交货的周期和产品寿命周期等。因此,很多企业正在加快进行以生产为中心向以客户为中心的企业转型。市场环境的变化需要能及时反映不断变化的客户需求的的实时企业(Real Tim e Enterprise)。本文提出了将自动补充系统BPM用于CRP(Continuous Rep len ishm ent Program)和供应商库存管理(VM I)的实行方案,使整个过程构成网络服务体系,将各程序在实时供给系统中执行主体间的信息传达迟滞时间或等待时间(waiting tim e)最小化。     

CIVA

CIVA (Comet Infrared and Visible Analyser) is an integrated set of imaging instruments, designed to characterize the 360^∘ panorama (CIVA-P) as seen from the Rosetta Lander Philae, and to study surface and subsurface samples (CIVA-M). CIVA-P is a panoramic stereo camera, while CIVA-M is an optical microscope coupled to a near infrared microscopic hyperspectral imager. CIVA shares a common Imaging Main Electronics (IME) with ROLIS. CIVA-P will characterize the landing site, with an angular sampling (IFOV) of 1.1 mrad: each pixel will image a 1 mm size feature at the distance of the landing legs, and a few metres at the local horizon. The panorama will be mapped by 6 identical miniaturized micro-cameras covering contiguous FOV, with their optical axis 60^∘ apart. Stereoscopic capability will be provided by an additional micro-camera, identical to and co-aligned with one of the panoramic micro-camera, with its optical axis displaced by 10 cm. CIVA-M combines two ultra-compact and miniaturised microscopes, one operating in the visible and one constituting an IR hyperspectral imaging spectrometer: they will characterize, by non-destructive analyses, the texture, the albedo, the molecular and the mineralogical composition of each of the samples provided by the Sample Drill and Distribution (SD2) system. For the optical microscope, the spatial sampling is 7 μm; for the IR, the spectral range (1–4 μm) and the spectral sampling (5 nm) have been chosen to allow identification of most minerals, ices and organics, on each pixel, 40 μm in size. After being studied by CIVA, the sample could be analysed by a subsequent experiment (PTOLEMY and/or COSAC). The process would be repeated for each sample obtained at different depths and/or locations.     

Neutral Atmospheres of the Giant Planets: An Overview of Composition Measurements

Measurements of the chemical composition of the giant planets provide clues of their formation and evolution processes. According to the currently accepted nucleation model, giant planets formed from the initial accretion of an icy core and the capture of the protosolar gas, mosly composed of hydrogen and helium. In the case of Jupiter and Saturn (the gaseous giants), this gaseous component dominates the composition of the planet, while for Uranus and Neptune (the icy giants) it is only a small fraction of the total mass. The measurement of elemental and isotopic ratios in the giant planets provides key diagnostics of this model, as it implies an enrichment in heavy elements (as well as deuterium) with respect to the cosmic composition. Neutral atmospheric constituents in the giant planets have three possible sources: (1) internal (fromthe bulk composition of the planet), (2) photochemical (fromthe photolysis ofmethane) and(3) external (from meteoritic impacts, of local or interplanetary origin). This paper reviews our present knowledge about the atmospheric composition in the giant planets, and their elemental and istopic composition. Measurements concerning key parameters, like C/H, D/H or rare gases in Jupiter, are analysed in detail. The conclusion addresses open questions and observations to be performed in the future.