基于多边形的积木式大圆锥端面直径测量

介绍了一种根据与被测圆锥表面有关联的多边形测量大圆锥端面直径的方法。通过磁铁现场组装各测量单元,可以实现任意大圆锥包括锥孔的端面直径测量。测量装置具有结构简单、体积小、成本低及测试容易等特点。由于各测量单元的平均化作用,当测量小锥度端面直径时,测量误差仅为（０ ．００５＋ １ ×１０－５ Ｄ） ｍｍ 。     

空间扫描

空间扫描美航宇局２０００年将用超级气球进行空间实验该气球比３０层大楼还要高，宽超过９０ｍ，能把大约１３５０ｋｇ重的科学仪器送入３５ｋｍ高，在空间可停留１００天。利用气球进行实验成本低廉，仅需１００万美元。其实验仪器可回收并多次使用。预计气球飞行任务将...     

1MΩ～100GΩ高值电阻器高精度的校准方法

高阻计、数字源表等仪器在半导体行业有着广泛的应用。但目前市场上1MΩ~100GΩ高值电阻器准确度(±1.0×10-3~±1.0×10-2)无法满足高阻计、数字源表等仪器电阻参数的溯源需求。本文提出了一种高精度的高值电阻器的校准方法,该方法由两个多功能校准源和指零仪组成的比较电桥实现。根据校准方法组建了1MΩ~100GΩ测量系统,测量结果的不确定度为3.0×10-5~8.0×10-4,可满足市场上绝大部分高阻测量仪器的校准需求。     

激光测量大直径方法的研究

大型工件内外径测量点的瞄准和定位是大直径测量中的一个关键技术，也是国内外未能很好解决的测量问题。提出了一种利用激光光线瞄准大型工件内外径测量点的新方法和使用双频激光干涉仪测量大直径的原理。该方法利用激光准直仪出射的高稳定光线，经单个测量头中的五角棱镜反射后，先后瞄准吸附在被测工件直径两端点上的两个磁性定位块上的光电接收器，使用双频激光干涉仪直接测量出这两个光电接收器中心之间的距离，通过简单的几何计算得到被测直径大小。还对系统的测量误差进行了简要的分析，并给出了１０００ｍｍ量块和Φ５００ｍｍ直径对比的实验结果。理论分析和实验结果表明：测量系统的相对测量误差小于５×１０￣（－６）。     

一种高g值冲击标准校准裝置

本文介绍了高g值冲击标准校准装置的原理和方法,详细分析了该装置的误差来源及其合成方法,并给出了实验结果。该装置的不确定度为U_(95％)=±3％。(200～2×10~5m/S~2),U_(95％)=±5％(3×10~5m/S~2)。用该装置对美国ENDEVCO公司的2270标准加速度计进行幅值线性度校准,其校准值与出厂值完全一致。     

高频高稳恒温晶体振荡器设计

本文采用低频高稳振荡与低噪声倍频相结合的方法，并进行精密控温设计，研制了一种高频高稳恒温晶体振荡器，输出频率为100MHz，短期频率稳定度可以实现2.68E-13/s，2.54E-12/100s，老化率优于7E-11/d，谐波优于-50dBc。经随机振动、冲击和温度冲击等环境试验考核，晶振试验前后频率变化均小于±5E-9，可以很好地满足多领域应用对高频高稳定信号源的需求，可靠性高，有利于简化系统构成，缩小设备体积。     

现代小卫星的新创举——立方体纳型卫星

小卫星中最不引人注意的皮型卫星(Picosat),1999年重新被定义为立方体星(CubeSat),即质量为1kg、体积约为10cm×10cm×10cm的正立方体星。由若干颗立方体星可以组成纳型卫星(Nanosat)。近几年来,这2种卫星得到飞速发展,并且在分布式空间系统中获得了非常成功的应用。例如:采用50～100颗立方体星,每颗质量8kg,可以实现全球覆盖,同时还可以获得高空间分辨率(2～3m)和高时间分辨率(重访时间15～45min),其经济成本仅为1亿多美元,相当于目前1颗对地观测大卫星的价钱。     

CCD星敏感器光学系统设计

介绍ＣＣＤ星敏感器用光学系统设计的参数选择,光学系统的设计光谱范围０．４８、０．８５μｍ;焦距为７５ｍｍ,Ｆ／１．４４,视场８．５°。该系统为复杂化的Ｐｅｔｚｖａｌ结构形式;以点列图能量集中度和能量重心偏评价光学系统的成像质量。所选用的ＣＣＤ芯片像元尺寸为２３μｍ×２３μｍ,像元数３８４×２８８,全视场内混色光点列图能量重心偏最大值１．６μｍ,对应于４．３９角秒。     

一种实用的高中频输出集成混频器

本文介绍一种高中频输出的微波集成平衡混频器。在C波段,中频输出在250～400兆赫通带内,混频器的前中放单边带整机噪声系数(包括前中放噪声系数≤2分贝)可达7～7.5分贝。由于中频频率较高,又有一定的中频带宽要求,因此在设计混频器电路时作了某些特殊考虑。全部电路制作在30×40×1毫米~3的陶瓷基片上。通过环境试验条件考核,电性能稳定,结构可靠。     

电弧加热发动机的实验研究

介绍一种低功率电弧加热发动机系统的实验研究。该系统包括电源，点火系统，推进剂供给系统，发动机本体和一些测量设备。用氮和氩对不同的喷口喉道直径（０．６ｍｍ～１ｍｍ），不同的质量流率（２０ｍｇ／ｓ～１００ｍｇ／ｓ），不同的电源电压（８０Ｖ～１５０Ｖ）进行了性能研究。所有试验都是在直径为１ｍ，长为１．６ｍ的真空室内进行的     

Properties of the high area-to-mass ratio space debris population at high altitudes

In the framework of its space debris research activities ESA established an optical survey program to study the space debris environment at high altitudes, in particular in the geostationary ring and in the geostationary transfer orbit region. The Astronomical Institute of the University of Bern (AIUB) performs these surveys on behalf of ESA using ESA’s 1-m telescope in Tenerife. Regular observations were started in 1999 and are continued during about 120–140 nights per year. Results from these surveys revealed a substantial amount of space debris at high altitudes in the size range from 0.1 to 1 m. Several space debris populations with different dynamical properties were identified in the geostationary ring. During the searches for debris in the geostationary transfer orbit region a new population of objects in unexpected orbits, where no potential progenitors exist, was found. The orbital periods of these objects are clustered around one revolution per day; the eccentricities, however, are scattered between 0 and 0.6. By following-up some of these objects using the ESA telescope and AIUB’s 1-m telescope in Zimmerwald, Switzerland, it was possible to study the properties of this new population. One spectacular finding from monitoring the orbits over time spans of days to months is the fact that these objects must have extreme area-to-mass ratios, which are by several orders of magnitudes higher than for ‘normal-type’ debris. This in turn supports the hypothesis that the new population actually is debris generated in or near the geostationary ring and which is in orbits with periodically varying eccentricity and inclination due to perturbations by solar radiation pressure. In order to further study the nature of these debris, multi-color and temporal photometry (light curves) were acquired with the Zimmerwald telescope. The light curves show strong variations over short time intervals, including signals typical for specular reflections. Some objects exhibit distinct periodic variations with periods ranging from 10 to several 100 s. All this is indicative for objects with complicated shapes and some highly reflective surfaces.     

高频大电压标准器

主要阐述了该标准器的基本原理,从理论上对结构补偿法进行了分析和数学推导,当R/Z_o=1.9～2.0之间时,具有最小的交直流差。设计了匹配的同轴热电转换标准器;进行了误差分析;给出了试验结果,说明该标准器交直流差的重复性和复现性是好的。     

Very high energy gamma-ray sources

A brief review of very high energy gamma-ray astronomy achievements is presented. The results of observations of the Crab nebula, the Cygnus X-3, Vela pulsar, radiogalaxy Centaurus A and 2CG 195+4 show that all these objects are the sources of very high energy gamma-quanta. The most powerfull source is Cygnus X-3. Its gamma-ray luminosity is no less than 3·10³⁷ erg.s⁻¹. The upper limit of quanta energy is no less than 10¹⁶eV. All sources are variable in different time scales, from milliseconds up to years. The nature of all these sources is not known yet, but known ones are pulsars.     

高压高剪切率下密封环缝隙流体动态润滑特性

为减少高压高剪切率下热效应对密封环缝隙流体润滑性能的影响,以密封环缝隙流体剪切速度梯度、壁面剪切应力和油膜温升表征摩擦副润滑性能,采用RNG k-ε湍流模型,通过Workbench建立流-固-热多场模型,计算得到不同主轴转角下缝隙流动形态变化规律和温升前后油膜厚度变化量、不同L型槽内外径比及长径比下流速流型分布规律、壁面剪切应力、温度分布和热变形量。研究结果表明:密封环L型槽黏性底层随剪切速度增大而增厚,油膜厚度随运动周期增加而变薄;当L型槽内外径比小于1.07时,随比值减小密封环壁面剪切应力不断增大,最大变化率为7%;密封环L型槽长径比在0.19时平均壁面剪切应力达到最大,当长径比继续增大时,油膜区剪切速度梯度逐渐减小,油膜温升和热变形亦随之减小。研究结果可为马达优化以减少能量损失和改善密封环润滑条件提供理论指导和依据。      

高频大功率GXN—50型霓虹灯电子电源的研制

ＧＸＮ－５０型霓虹灯电子电源是为负载提供高频交流电压电流的电源设备，是一种专用大功率霓虹灯电源。该产品采用先进的电子技术，节能效率高，带负载能力强（比传统电源高４倍以上），并采用超音技术，用特制的电子开关代替价格昂贵的机械继电器，因而无任何噪声，灯光变化采用程序控制，变换方式灵活，工作稳定可靠。该电源体积小、重量轻，并设计了过压过流保护电路，具有抗干扰能力强等特点。     

Flight performance of a high resolution,high data rate solar ultraviolet telescope and spectrograph

The High Resolution Telescope and Spectrograph (HRTS) instrument has been flown three times on sounding rockets and has dramatically demonstrated the value of high resolution (spectral, spatial, and temporal) coupled with wide spectral and spatial coverage. Through the use of film as a detector, the HRTS can capture a large spectral and spatial range simultaneously. Because of the high spectral and spatial resolution, each exposure contains 10 million data points. After digitizing, this equates to a data collection rate of four megabits per second for a 20 second exposure. Because of the large film format, a set of HRTS exposures has recorded complete profiles of over 2800 emission lines simultaneously at 1000 different locations on the Sun. These emission lines originate in temperature regimes ranging from the temperature minimum to the corona. This allows a statistical analysis of temperature, pressure, density and velocity in many layers of the solar atmosphere.     

Production of high fidelity lunar agglutinate simulant

As space faring nations consider manned and unmanned missions to the Moon, there is a growing need to develop high fidelity lunar regolith simulants that can accurately reproduce the properties and behavior of lunar regolith. Such simulants will be employed to verify the performance of equipment, mechanisms, structures and processes to be used on the lunar surface. One of the significant limitations of current terrestrial-based simulants, such as the popular mare simulant, JSC-1A, is the lack of agglutinates. This paper investigates the production of a lunar mare agglutinate simulant based on JSC-1A. A modified plasma processing technique was used to expose the JSC-1A regolith simulant to high temperatures and transform it to predominantly a glassy phase. Detailed characterization results are presented to confirm that the agglutinate simulant material produced during this investigation reasonably satisfies the primary requirements of an agglutinate simulant such as amorphous/crystalline content, particle size, morphology, vesicular structure, chemistry, and presence of nanophase elemental Fe.     

关于大电流测试问题的研究

采用电流比较仪,AD交直流标准电阻,高准确度数字多用表组成校验系统,解决大电流测试问题.     

High resolution science with high redshift galaxies

We summarize the high-resolution science that has been done on high redshift galaxies with Adaptive Optics (AO) on the world’s largest ground-based facilities and with the Hubble Space Telescope (HST). These facilities complement each other. Ground-based AO provides better light gathering power and in principle better resolution than HST, giving it the edge in high spatial resolution imaging and high resolution spectroscopy. HST produces higher quality, more stable PSF’s over larger field-of-views in a much darker sky-background than ground-based AO, and yields deeper wide-field images and low-resolution spectra than the ground. Faint galaxies have steadily decreasing sizes at fainter fluxes and higher redshifts, reflecting the hierarchical formation of galaxies over cosmic time. HST has imaged this process in great structural detail to z  6, and ground-based AO and spectroscopy has provided measurements of their masses and other physical properties with cosmic time. Last, we review how the 6.5 m James Webb Space Telescope (JWST) will measure First Light, reionization, and galaxy assembly in the near–mid-IR after 2013.     

一种仪器用高准确度MCXO

针对频率计等仪器中使用温补晶振的特殊情况提出并实现了一种软件数据补偿的特殊ＭＣＸＯ。其补偿原理与传统的方式有所不同，它不是对振荡器进行补偿控制，而是根据温度的变化以数据方式不断修改晶体振荡器的频率标称值来达到提高准确度的目的，当该振荡器被用作标准来测量其它信号或用它产生标准时间信号时，都以其准确的频率为基础进行运算和处理。所以，这种ＭＣＸＯ不但远比同类ＭＣＸＯ简单，而且在构成系统中获得的准确度也高得多