精密工程中应用的宽范围原子力显微镜的研究

描述了一种用于精密工程中超精密测量的宽范围原子力显微镜．用管状扫描器工作时，测量范围可达２μｍ×２μｍ，能获得原子级的分辨率．当用新开发的定范围工作台扫描时，测量范围可为１４０μｍ×１４０μｍ；分辨率可在１～１００ｎｍ之间调节．     

M—410i型高速堆垛机器人

Ｍ—４１０ｉ型高速堆垛机器人日本公司开发出Ｍ—４１０ｉ高速堆垛机器人．Ｍ—４１０ｉ型高速堆垛机器人每小时输送达１２００次，创世界最高纪录．Ｍ—４１０ｉ型机器人工作范围很大，在宽广的工作范围内放置１．６ｍ方形托盘，其上堆放的工件可高达２．１ｍ。该机器人...     

旋转CVI制备陶瓷基复合材料碳界面层

用旋转ＣＶＩ工艺，通过优化工艺参数，在低压（５ｋＰａ）、高温（１１００℃）、高Ｃ３Ｈ６ 浓度（６２．５ｖｏｌ％ ）以及３．５ｍ ｍ ·ｍ ｉｎ－ １ 碳布旋转线速度条件下，在二维碳布上快速制备了厚度均匀（０．２５μｍ ）、表面规整的致密热解碳界面层。实验结果表明：沉积温度对界面层表面状况有较大的影响；采用减压法与优化沉积炉结构与几何尺寸，能有效防止高温高Ｃ３Ｈ６ 浓度下炭黑的形成。     

测微准直望远镜与零距直角头组合后同轴度误差的测定和消除

一、问题的提出测微准直望远镜与零距直角头组合使用时,使光学视线转折90°,用来建立互相垂直的光学视线或与光学视线垂直的光学平面及若干个互相平行的光学平面等,是最常用的方法。使用这一方法时,人们往往只注意到测微准直望远镜与零距直角头的互换使用,而容易忽视测微准直望远镜与零距直角头组合后,产生了新的光轴与机械轴的同轴度误差。该误差有时远大于测微准直望远镜的光轴与机械轴的     

面向脉冲星深空基准建立的X射线望远镜及发展设想

深空基准是进入、利用和控制太空的基础，X射线望远镜是构建脉冲星深空基准的重要观测设备。首先，论述了脉冲星计时在深空基准建立中的作用，定性分析了毫秒脉冲星空间观测对X射线望远镜的需求，系统总结了X射线望远镜的国内外技术现状及发展趋势；其次，针对X射线毫秒脉冲星观测中脉冲信号弱而非脉冲信号及空间弥散本底较强的特点，提出了利用毫秒脉冲星高分辨率成像观测抑制非脉冲噪声的方法，并初步设计了一种高分辨率低噪声X射线望远镜；最后，分析了不同的脉冲信号流量、非脉冲信号流量、角分辨率及单次镜片反射效率分别对聚焦成像型、聚焦非成像型和准直非成像型X射线望远镜脉冲星观测信噪比的影响，发现聚焦成像型X射线望远镜在弱脉冲信号和强非脉冲信号流量下具有较好的探测能力。同时计算结果表明：在相同条件下，聚焦成像型望远镜对5颗导航脉冲星的探测灵敏度，比美国中子星内部组成探测器（NICER）的X射线计时仪器（XTI）有不同程度的提高。可见，设计的聚焦成像型X射线望远镜，能够有效地提高毫秒X射线脉冲星的观测能力，能为国家综合定位导航授时（PNT）及深空基准体系的建设提供硬件支持。     

采用机头边条改善飞机大迎角横侧气动特性的风洞试验研究

本文就采用机头边条改善飞机大迎角横侧气动特性进行了讨论。着重对机头边条的大小，安位置等对飞机稳定性的影响进行讨论。试验是在气动中心低速所４ｍ＊３ｍ和φ３．２ｍ风洞中进行的。     

极轴式望远镜系统误差修正模型推导

为保证极轴式望远镜轴系测量精度,需要对其系统误差进行修正。在分析极轴式望远镜测角工作原理的基础上,提出了利用欧拉变换方法推导其系统误差修正模型。采用该方法详细推导出望远镜的测角元件误差、极轴误差、纬轴误差、视轴误差等轴系误差模型以及镜筒下沉误差模型,并给出了极轴式望远镜的系统误差修正模型。该误差修正模型与采用球面三角学的方法推导出来的系统误差修正模型完全一致,欧拉变换方法由于只涉及到坐标的旋转与矩阵的计算,更容易理解和掌握。     

一种快速制备C/C材料方法的探索研究

介绍了一种新的Ｃ／Ｃ材料制备方法－－快速化学液气相渗透致密法。利用该技术,采用碳毡作预制体,以两种液态低分子有机物作碳源前驱体沉积时间在３ｈ内,沉积温度在９００℃￣１１００℃范围内可获得密度达１．７４ｇ／ｃｍ＾３的Ｃ／Ｃ材料。碳纤维表面最大沉积速率可达６４μｍ／ｈ,比传统的等温ＣＶＩ沉积速率（０．１μｍ／ｈ￣０．２５μｍ／ｈ）提高了２００倍以上,并初步分析了该技术快速致密多孔预制体的机理。     

单站发射多站接收的空间目标激光测距技术

激光测距作为空间目标测定轨精度最高的技术,对非合作目标的测量精度比微波雷达、光电探测等技术高1～2个数量级,非常有利于非合作目标的精密定位、轨道复核及精确编目,保障在轨空间飞行器的安全。激光在非合作目标表面会发生漫反射,返回光斑弥散、回波微弱,采用大口径望远镜接收系统是必要的。鉴于大口径望远镜研制难度大,提出基于单站发射多站接收的空间目标激光测距新方法,即采用多接收望远镜增加接收面积,实现目标测量能力提升。通过分析单站发射多站接收的激光测距技术特点,基于双望远镜系统开展空间合作目标测量实验,验证了多望远镜接收激光信号的可行性,为该测距技术发展奠定了实验基础。     

大型管中两相爆炸现象的实验研究

介绍了用于研究气－液和气－固悬浮流中加速火焰诱导激波现象的两套实验装置,即长９ｍ,内径０．１４ｍ两侧装有１５套喷雾系统的水平气云火焰加速管和长１２ｍ内径０．１４ｍ两侧装有２０套喷粉系统的水平粉尘火焰加速管,利用上述装置,对铝粉粉尘云和戊烷气雾云两相悬浮流中火焰加速诱导激波现象进行了实验研究,用压电传感器测试管内某点的压力信号和离子探针测试火焰阵面信号,从而得到管内火焰传播的规律和管内压力参数的变化     

The near infrared high resolution imaging camera program of Beijing Observatory

This paper introduces the program of an adaptive optics system using an infrared camera for the near infrared observations based on the 2.16 m telescope of Beijing Observatory. This system consists of 3 parts: (1), the 2.16 m telescope; (2), the adaptive optics system that will be mounted at the coudé focus on an optical table. It will be used to remove the effect of atmospheric turbulence on the imaging observations; (3), the infrared camera with a 512×512 PtSi IR detector array.     

The infrared space observatory

The Infrared Space Observatory (ISO), a programme of the European Space Agency, is an astronomical satellite operating at wavelength from 2.5 to 200 m. It will be launched in 1995.The ISO optical subsystem is a cryogenically cooled telescope with its baffling system (main baffle and sunshade). The telescope, a 60 cm Ritchey-Chrétien type, focuses the beam to the four scientific instruments located in its focal plane. The extremely low temperature, 1.8 K, is provided by the payload module (PLM) cryostat, filled with superfluid He.This paper presents the main choices done for the telescope design together with their rationale and the performances achieved on the flight model (FM) of the telescope. The FM telescope is presently installed inside the payload module, ready for the system final verifications.     

Optimised radiative cooling of infrared space telescopes and applications to possible missions

General principles are outlined for the design of space infrared telescopes intended to cool by radiation to the lowest temperatures attainable without the use of on-board cryogens, and assuming on-orbit cooling after a warm launch. Maximum protection from solar and earth heating, maximum radiating area and efficiency and minimum absorbing area and absorptivity are the obvious basic criteria. The optimised design is a short, fat telescope surrounded by a series of radiation shields, each cooled by its own radiator. Maximising the longitudinal conductivity of the radiation shields and of the telescope tube itself is important both to the on-orbit cooling time and the final achieveable temperature. Realistic designs take between 80 and 200 days to cool to within a few degrees of equilibrium temperatures, depending on the materials used. Great advantages accrue from the use of an orbit distant from earth. Both simple models and detailed simulations suggest that temperatures of 30 to 40 K are attainable in high earth orbits. Placing a radiatively cooled telescope in a halo orbit around the Lagrangian point L2 is a particularly attractive option and significantly lower temperatures can be achieved there than in Earth orbit. Optimised radiative cooling is an important element of the small Japanese mission SMIRT. We suggest that a combination of an ESA Medium-sized Mission with a NASA Explorer to send a 2m+ telescope to an L2 halo orbit would provide a cost-effective and powerful long-duration facility for the early 21st century.     

An Overview of the Instrument Suite for the Deep Impact Mission

A suite of three optical instruments has been developed to observe Comet 9P/Tempel 1, the impact of a dedicated impactor spacecraft, and the resulting crater formation for the Deep Impact mission. The high-resolution instrument (HRI) consists of an f/35 telescope with 10.5 m focal length, and a combined filtered CCD camera and IR spectrometer. The medium-resolution instrument (MRI) consists of an f/17.5 telescope with a 2.1 m focal length feeding a filtered CCD camera. The HRI and MRI are mounted on an instrument platform on the flyby spacecraft, along with the spacecraft star trackers and inertial reference unit. The third instrument is a simple unfiltered CCD camera with the same telescope as MRI, mounted within the impactor spacecraft. All three instruments use a Fairchild split-frame-transfer CCD with 1,024× 1,024 active pixels. The IR spectrometer is a two-prism (CaF₂ and ZnSe) imaging spectrometer imaged on a Rockwell HAWAII-1R HgCdTe MWIR array. The CCDs and IR FPA are read out and digitized to 14 bits by a set of dedicated instrument electronics, one set per instrument. Each electronics box is controlled by a radiation-hard TSC695F microprocessor. Software running on the microprocessor executes imaging commands from a sequence engine on the spacecraft. Commands and telemetry are transmitted via a MIL-STD-1553 interface, while image data are transmitted to the spacecraft via a low-voltage differential signaling (LVDS) interface standard. The instruments are used as the science instruments and are used for the optical navigation of both spacecraft. This paper presents an overview of the instrument suite designs, functionality, calibration and operational considerations.     

Precise Attitude Stabilization of a Large Orbiting Telescope Coupled to a Crew Compartment

Computer simulation results are presented for the planar equations of motion of an attitude-stabilized orbiting telescope passively coupled to a manned service module. This coupling is provided through a set of soft springs and a two-axis gimbal aligned with the telescope center of mass. Principal nonlinearities in the suspension system and the telescope control system are included. The simulation indicates preliminary nary feasibility of this operational mode.     

某型直升机Ti1023钛合金中央件提前疲劳破坏原因分析

简要介绍了某型直升机Ti1023钛合金中央件疲劳提前破坏的情况.本文从原始断口的电镜扫描、材料、加工工艺和熔滴的影响等方面分析,得出了"断口的高应力集中区附近存在熔滴是试验件提前破坏的主要原因,材料的疲劳极限值尚不满足要求也是试验件提前破坏的主要原因"的结论,并给出了改进建议.     

Profile error compensation in precision grinding of ellipsoid optical surface

Optical glass elements with the ellipsoidal surface are used in many critical aerospace instruments, such as satellites, telescope and cameras. Their optical performance is mainly affected by profile accuracy and surface quality. In this paper, a rectangular ellipsoid surface is precisely ground on a BK7 optical glass blank by grating scanning grinding path with a three-axis CNC precision surface grinder. A profile error compensation procedure for ellipsoidal grinding is proposed based on the error analysis about the primary error sources in the XY and YZ projection planes during the grinding process. The mathematical prediction models of the wheel arc profile error, the measurement and wear error of the grinding wheel radiuses are established. By applying the proposed error compensation procedure, the profile accuracy of the ellipsoidal surface was improved from 4 μm to 2 μm in the XY plane, and improved from 15 μm to 5 μm in the YZ plane.     

基于可变滑动窗口与3σ准则的脉冲星信号去噪算法

针对地面接收射电观测脉冲星信号较弱、信噪比较低的问题,提出了基于可变滑动窗口与两层3σ准则的信号去噪算法。该算法引入可变滑动窗口,对信号进行分步连续处理,同时在筛选噪声时使用两层3σ准则算法,解决了噪声遗漏及过度去噪问题。为证明算法可靠性与实用性,利用佳木斯66 m观测站实测数据进行算法验证,针对J1939+2134与J1744—1134脉冲星的实测数据进行分析处理。结果表明,该算法能够对脉冲星数据进行有效去噪,普遍提高信噪比约10dB。     

Optical design and testing of a fast,large aperture,infrared space telescope

An optical design study for a next generation infrared space telescope has been performed. The concept is that of a passively cooled telescope of minium aperture 2.5 metre with an F/1.2 primary and wavelength coverage from = 2 to at least 40 m, and possibly to 100 m. Compactness, low thermal emission from the optics and structure, diffraction limited imaging at = 2 m, and sensitivity to misalignment aberrations and manufacturing errors were the main considerations for this study. Ray tracing results are presented showing the characteristics of the various designs considered. A preliminary investigation of stray light properties is also given. Special emphasis has been placed on the testing of such a fast primary, and optical systems using a lateral shearing interferometer are described for testing both the primary and the primary/secondary combination.     

Orbits for radiatively cooled space telescopes

This paper first outlines the assumed mission requirements for a radiatively cooled space telescope such as EDISON. A summary of relevant characteristics (payload, operating orbit, launcher, lifetime, etc.) for current and proposed cooled telescope missions is then given. This summary includes cryogenic and radiatively cooled missions since in both cases the reduction of heat input to the telescope aperture is a dominant factor in the orbit choice. These missions span the entire range of possibilities from low earth circular, through higher elliptical and circular orbits out to deep space locations such as the Sun-Earth (S-E) libration points and the lunar surface.A full listing of the factors affecting mission selection is then given. The most important points are illustrated by reference to the orbits chosen for ISO, FIRST and SIRTF and those recommended in recent studies of EDISON. Launcher capabilities for direct insertion and the onboard propellant for large velocity changes associated with orbit raising are major constraints in achieving the large payload mass to high orbit which EDISON mission requires. Although it is fairly demanding in launch/boost energy, an orbit about the L2 S-E libration point offers important advantages for a radiatively cooled infrared telescope. Further studies of this orbit and the associated aspects of service module and payload design for the L2 location of EDISON are recommended.