国防科工委科技与质量司高志强司长在航空行业5个专业标技委成立大会上的讲话(摘要)

同志们 :　　首先 ,我代表国防科工委科技与质量司对航空行业 5个专业标技委的成立表示热烈的祝贺 !对各位院士、各位专家在百忙之中来参加这个大会表示衷心的感谢 !同时也对秘书处 ,特别是对 30 1所做的大量工作表示谢意 !这个大会既是标技委成立大会 ,也是研究部署标技委今后工作的大会。我认为开好这个会 ,对我们航空行业的标准化工作 ,具有非常重要的意义。下面 ,我谈 3点意见 ,供大家参考。1　要认清形势。即要充分认识航空标准化工作的特殊重要性及其面临的形势和要求　　应该说在整个国防科技工业标准化工作中 ,航空标准化工作具有重…     

《武器装备研制管理译丛》前四集出版

为了配合型号综合标准化工作以及各行业研究应用系统工程管理标准,国防科工委军用标准化中心组织翻译了《武器装备研制管理译丛》。该译丛对借鉴国外武器装备研制管理经验,保障武器装备的高效能、高战备完好性和保障性、高效费比和低风险有重要参考价值。目前,该译丛的前四集已经出版。这四集是:     

信息与动态

2005年8月3日至5日,国防科技工业标准化“十一五”规划项目论证初审会在北京举行,会议由国防科工委科技与质量司主持,国防科技工业标准化研究中心负责此次会议的筹备和组织工作。国防科工委科技与质量司技术基础处的有关领导到会并讲话。会议的主要任务是:对各行业提交的国防科技工业标准化“十一五”规划项目(共320个)逐项进行审查并提出修改意见。来自核、航天、航空、船舶、兵器五大行业的120余名业内专家,按行业、专业工程和通用项目划分为8个组。各组专家按照科工委提出的要求,对提交初审的项目进行了技术把关,对经各行业论证的部分存…     

国防科工委标准化规章宣贯会在京召开

为贯彻国防科工委“科工法学[2000]851号文”和“科工技字[2000]758号文”的要求,受国防科工委科技质量司的委托,国防科工委标准化研究中心于12月14日到15日在京召开了“国防科工委标准化规章制度宣贯会”。有关集团公司标准化管理机构、标准化技术归口单位共计57人参加了会议。国防科工委科技质量司技术基础处岳峰处长主持了宣贯会。首先,高志强司长向与会代表传达了江泽民主席关于建立竞争机制、评价机制、监督机制、激励机制,以及新时期改革思想“寓军于民、大力协调、自主创新”十二字方针的精神,并指出在朱基总理提出加强行业规划、…     

领导重视,严格人选,服务型号,高效动作--航空电子标技委3年工作总结

国防科工委航空电子电气和武器系统标准化技术委员会(以下简称标技委)在国防科工委的领导下,在国防科技工业标准化研究中心、中国航空工业第一、第二集团公司及中国航空综合技术研究所的大力支持下,本着促进航空电子电气和武器系统标准化工作的发展、充分发挥专家作用的宗旨,积极开展了标准立项评审、标准送审稿审查、技术咨询和学术交流等活动.     

2007年度报道要点

根据国防科工委、总装备部和中国一航、中航二集团“十一五”的标准化与质量工作重点和发展目标,本刊拟定了2007年度报道要点:“十一五”期间标准化工作、质量管理与可靠性工程管理工作研究课题的方法与举措;高新技术应用的标准化理论研究、思路与措施;     

总结经验 抓住机遇 加速航空工业标准化的发展

总结经验抓住机遇加速航空工业标准化的发展编者的话该文系航空工业总公司张彦仲副总经理在全国第四次军用标准化工作会议上的发言。本刊略有删节。军用标准化自国防科工委归口统一管理以来，发展飞速，面貌发生了根本的变比。现就第三次军用标准化工作会议以来航空工业标...     

《航空标准化与质量》2006年度报道要点

根据国防科工委、总装备部和中国一航、中航二集团“十一五”开局年的标准化与质量工作重点和发展目标,本刊拟定了2006年度报道要点,供广大作者投稿时参考。1.标准化工作、质量管理与可靠性工程管理工作“十一五”发展框架与举措,开局之年的目标与任务。2.“十五”期间促进标准化工作、质量与适航性管理工作和可靠性工程管理工作可持续发展的经验。3.在经济全球化环境下,标准化和质量管理政策、理论研究。4.高新技术应用的标准化理论研究、思路与措施。5.集团/企业推广、应用“用户满意度测评模型”的经验、典型做法与体会。6.产品全寿命周…     

热烈祝贺第四次全国军用标准化工作会议胜利召开

热烈祝贺第四次全国军用标准化工作会议胜利召开大会会场军用标准化成就展示会开幕式国防科工委怀国模副主任作工作报告国防科工委谢光副主任参观军用标准化工作成就展览航空工业总公司张彦仲副总经理在大会上发言大会向先进工作者颁奖（本刊　摄）１９９４年１０月１８日...     

贯彻《若干意见》搞好型号研制标准化工作

根据国防科工委发布的《关于加强国防科技工业技术基础工作的若干意见》 ,简述了标准化对武器装备型号研制的重要性 ;重点叙述了如何以系统“三坐标”管理思想为指导 ,搞好型号研制标准化工作 ,并进一步提出了只有依靠广大工程技术人员的共同努力 ,才能搞好型号标准化工作。     

ICP-AES法测定纯铜中的Bi,Sb,As,Fe,Ni,Pb,Sn,Zn,Ag的方法

研究了ICP-AES法测定纯铜中的Bi,Sb,As,Fe,Ni,Pb,Sn,Zn和Ag等9个元素的分析方法.进行了基体元素铜对9个分析元素的光谱干扰研究,选择了合适的分析谱线,同时测定了分析方法的检出限.     

A survey of the outer planets Jupiter,Saturn, Uranus,Neptune, Pluto,and their satellites

A survey of current knowledge about Jupiter, Saturn, Uranus, Neptune, Pluto, and their satellites is presented. The best available numerical values are given for physical parameters, including orbital and body properties, atmospheric composition and structure, and photometric parameters. The more acceptable current theories of these bodies are outlined with thorough referencing offering access to the details. The survey attempts to cover the literature through May 1, 1972. Prepared Under Contract No. NAS7-100 National Aeronautics and Space Administration.     

Collapse,equilibrium, and fragmentation of rotating,adiabatic clouds

Numerical calculations of the collapse of adiabatic clouds from uniform density and rotation initial conditions show that when restricted to axisymmetry, the clouds form either near-equilibrium spheroids or rings. Rings form in the collapse of low thermal energy clouds and have = T/ ¦W¦ 0.43. When the axisymmetric constraint is removed and an initial m=2 density variation is introduced, clouds either collapse to form near-equilibrium ellipsoids or else fragment into binary systems through a bar phase. Ellipsoids form in the collapse of high thermal energy clouds and have 3 0.27. The results are consistent with the critical values of for instabilities in Maclaurin spheroids, and suggest that protostellar clouds may undergo a dynamic fragmentation in the nonisothermal collapse regime.National Academy of Sciences — National Research Council Resident Research Associate.     

Modeling of Venus, Mars, and Titan

Increased computer capacity has made it possible to model the global plasma and neutral dynamics near Venus, Mars and Saturn??s moon Titan. The plasma interactions at Venus, Mars, and Titan are similar because each possess a substantial atmosphere but lacks a global internally generated magnetic field. In this article three self-consistent plasma models are described: the magnetohydrodynamic (MHD) model, the hybrid model and the fully kinetic plasma model. Chamberlain and Monte Carlo models of the Martian exosphere are also described. In particular, we describe the pros and cons of each model approach. Results from simulations are presented to demonstrate the ability of the models to capture the known plasma and neutral dynamics near the three objects.     

Origin,age, and composition of meteorites

This paper attempts to bring together and evaluate all significant evidence on the origin of meteorites.The iron meteorites seem to have formed at low pressures. Laboratory evidence shows that the absence of a Widmanstätten pattern in meteorites with > 16% Ni cannot be attributed to high pressures, but to supercooling or an unusually fast cooling rate for these meteorites, which prevented the development of a pattern. The presence of tridymite in the Steinbach siderophyre provides further, direct proof that the Widmanstätten pattern can form at pressures less than 3 kb. Neither diamond, nor cliftonite, nor cohenite are reliable pressure indicators in meteorites. Diamonds were formed by shock while cliftonite may have been derived from a cubic carbide such as Fe₄C. Cohenite is apparently stabilized by kinetic rather than thermodynamic factors. Several lines of evidence suggest that the irons come from more than one parent body, perhaps as many as four.The frequency of pallasites is perfectly consistent with an origin in the transition zone between core and mantle of the parent body. Hybrid meteorites such as Brenham are not necessarily derived from the metal-silicate interface, but probably resulted from dendrite growth in the solidifying melt.Ordinary chondrites definitely are equilibrium assemblages rather than chance conglomerates. According to the best available evidence, Prior's rules seem to be valid. The metal particles in chondrites differentiated into kamacite and taenite in their present location, rather than in a remote earlier environment. Trace element abundances in ordinary and carbonaceous chondrites suggest that these meteorites accreted from two types of matter: an undepleted fraction that separated from its complement of gases at low temperatures, and a depleted fraction that lost its gases at high temperatures. These two fractions of primitive meteoritic matter are tentatively identified with the matrix and chondrules-plus-metal, respectively. New restrictive limits are placed on the iron-silicate fractionation in chondrites. No direct evolutionary path exists that connects the currently accepted solar abundances of Fe and Ni and the observed Fe/Si and Ni/Si ratios in chondrites. Apparently the solar abundance of iron is in error. The iron-silicate fractionation seems to have occurred while chondritic matter was in a more strongly reduced state than its present one.The U-He and K-Ar ages of hypersthene chondrites are systematically shorter than those of bronzite chondrites. Short ages are correlated with shock effects, and it seems that the hypersthene chondrites suffered reheating and partial-to-complete outgassing 0.4 AE ago. The cosmic-ray exposure ages of all classes of meteorites cluster distinctly, indicating that the meteorites were produced in a few discrete major collisions rather than by a quasi-continuum of smaller ones. The dates of the principal breakups are: irons, 0.6 and 0.9 AE; aubrites, 45 m.y.; bronzite chondrites, 4 m.y.; hypersthene chondrites, 0.025, 3, 7–13, and 16–31 m.y. All four clusters of hypersthene chondrites show evidence of severe outgassing 0.4 AE ago, which implies that most or all hypersthene chondrites come from the same parent body.As already noted by Signer and Suess, two distinct types of primordial gas occur in meteorites. Differentiated meteorites always contain unfractionated gas, while relatively undifferentiated meteorites contain fractionated gas. The former component is invariably associated with shock effects, and seems to have been derived from the solar wind. The latter component is correlated with other volatiles and seems to be a truly primitive constituent of meteoritic matter. Isotopic anomalies in the fractionated gas suggest that meteoritic matter was irradiated with 10¹⁷ protons/cm² at a very early stage of its history.There is very little doubt that most, if not all, meteorites come from the asteroid belt rather than from the moon. The orbits and geocentric velocities of stony meteorites resemble those of the Apollo asteroids (most of which are former members of the asteroid belt that have strayed into terrestrial space), but disagree strongly with the calculated orbits and velocities for lunar ejecta. Öpik's conclusions about the difficulty of accelerating lunar debris to escape velocity represent a further argument against a lunar origin of stony meteorites.The most likely parent bodies of the meteorites are the 34 asteroids which cross the orbit of Mars. Collisional debris from these objects will remain in Mars-crossing orbits, and perturbations by Mars will inject some fraction of this material into terrestrial space. Most of the Mars asteroids, comprising 98% of the mass and 92% of the cross-section, belong to three Hirayama families (Phocaea, Desiderata, and Aethra), and an additional, previously unrecognized family. These families were apparently produced by disruption of parent asteroids ca. 104, 105, and 46 km in diameter. The size distribution and light curves of asteroids indicate that the larger asteroids are original accretions, rather than collision fragments. There is no reason to believe that the meteorites ever resided in bodies larger than Ceres (d = 770 km).Various theories on the origin of the meteorites are critically reviewed in the light of the preceding evidence. Wood's theory, which postulates a high-temperature and a low-temperature variety of primordial matter, is in best accord with the evidence. Apparently the asteroids accreted from varying proportions of these two types of material, and were then heated by extinct radioactivity produced in the early irradiation.     

Chemistry,accretion, and evolution of Mars

The high FeO concentrations measured by VIKING for the Martian soils correspond to all probability to a FeO-rich mantle. In general, the VIKING XRF-data indicate a mafic crust with a considerably smaller degree of fractionation compared to the terrestrial crust.In recent years evidence has been collected which points towards Mars being the parent body of SNC-meteorites and, hence, these meteorites have become a valuable source of information about the chemistry of Mars. Using element correlations observed in SNC-meteorites and general cosmochemical constraints, it is possible to estimated the bulk composition of Mars. Normalized to Si and Cl, the mean abundance value for the elements Ga, Fe, Na, P, K, F, and Rb in the Martian mantle is found to be 0.35 and thus exceeds the terrestrial value by about a factor of two. Aside pressure effects and the H₂O poverty, the high P and K content of the Martian mantle may lead to magmatic processes different from those on Earth.The composition of the Earth's mantle can successfully be described by a two component model. Component A: highly reduced and almost free of all elements more volatile than Na; component B: oxidized and containing all elements in Cl-abundances including volatile elements. The same two components can be used as building blocks for Mars, if one assumes that, contrary to the inhomogeneous accretion of the Earth, Mars accreted almost homogeneously. The striking depletion of all elements with chalcophile character indicates that chemical equilibrium between component A and B was achieved on Mars which lead to the formation of significant amounts of FeS which, on segregation, extracted the elements according to their sulphide-silicate partition coefficients. While for the Earth a mixing ratio AB = 8515 was derived, the Mars ratio of 6040 reflects the higher concentrations of moderately volatile elements like Na, K, and sulphur on Mars. A homogeneous accretion of Mars could also explain the obvious low abundances of water and primordial rare gases.     

ICP-OES法测定钛合金中稀土元素Y,La,Pr,Sm,Ce,Gd和Nd

进行了用电感耦合等离子体发射光谱法(ICP-OES)法测定钛合金中稀土元素Y,La,Pr,Sm,Ce,Gd和Nd的研究.研究样品的溶解,待测稀土元素分析谱线的选择,钛合金基体及共存元素对稀土元素测量的影响等,确定了待测稀土元素的分析线,校准曲线采用基体匹配消除基体效应的影响,对仪器测量条件进行优化.进行了加入回收实验.精密度和准确度结果表明:本方法快速、准确,可以满足钛合金中的稀土元素的测定要求,RSD<4%,回收率98%～105%.