调频激光干涉绝对距离测量技术及其信号处理

最最的绝对距离测量方法是非相干飞行时间测量法。随后，在小数重合法的基础上，产生了多波长干波绝对距离测量技术。随着半导体激光器的发展，８０年代又出现了调频干涉绝对距离测量方法，并很快成为一种新的测长技术。本文在综述绝对距离技术及方法的基础上，着重介绍了调频激光干涉绝对距离测量技术的一些新发展及其几种不同的信号处理。     

光滑通道内格栅湍流特性实验

为了更好地模拟实际涡轮叶片内冷通道的流动换热，采用格栅对光滑通道内湍流度进行控制。并通过实验的方法对不同格栅尺寸激发的湍流度进行测量。实验中，在边长为80mm×80mm的方形通道中，放置了3种不同尺寸的格栅，利用热线风速仪，得到了通道雷诺数为5000~30000范围内的格栅后下游湍流特性。研究发现:流体通过该格栅后，气流在流经格栅后较短距离内就获得了4.5%的湍流度，同时湍流度沿程呈现衰减趋势，雷诺数对湍流度的影响较小。湍流积分时间尺度与雷诺数呈负相关的关系。      

基于激光扫描的移动机器人实时轨迹测量系统

 设计了一种移动机器人实时轨迹测量系统，主要包括激光扫描仪、数据采集计算机、无线通讯网络和数据处理显示软件4个部分。测量系统采用两台激光扫描仪从不同高度测量机器人身上安装的标志杆的位置，将测量数据经过位置识别和坐标系对准后，传输到一台计算机上进行融合，采用卡尔曼滤波器消除测量随机误差，绘制出机器人的运动轨迹。实验结果表明，测量系统可以在较大的测量范围内实现厘米级测量精度和目标分辨率的轨迹测量，为移动机器人的设计开发和导航控制等研究领域提供了良好的实验测试平台。     

光纤表面粗糙度测量中探头的精密定位

介绍了光纤表面粗糙度测量原理及探头定位的实验装置．叙述了如何采用单片机控制步进电机带动探头运动来确定最佳定位距离，从而实现精密自动定位．该装置的使用不仅使光纤测量仪的输出只反映已加工表面的变化，提高测量精度，而且大大提高了测量效率，缩短了测量时间．     

空间目标的空基红外测量技术

地基红外测量系统由于受大气衰减和天空背景的影响,对空间目标的探测能力有限。针对此问题,提出了采用空基红外测量系统实现空间目标红外特性测量的设想,通过从决定红外测量系统探测能力的信噪比和调制对比度2个方面出发,推导出了红外测量系统作用距离公式。并利用大气传输软件计算了长波红外在不同高度下的大气透过率、天空背景,理论分析给出了不同高度的空基红外测量系统对不同辐射面积空间目标的探测距离。仿真结果表明,当空基平台高度大于10km时,长波红外不仅可以观测到光照区内的低轨空间目标,而且还可以观测到阴影区内辐射面积不小于40m~2的低轨空间目标。     

球形破片飞行速度衰减过程实验研究

通过二级轻气炮发射方式、激光无阻测量方法测量了不同材料、不同直径的球形破片在不同初速条件下长距离(最大距离达120m)飞行时的速度衰减规律.试验结果表明:在同一初速条件下,球形破片长距离飞行时的衰减系数为常数;破片飞行空气阻力系数与破片初速有关,在战斗部设计关心的范围内(1.2 km/s～2.2 km/s),阻力系数与初速成线性关系.     

反射激波冲击单模界面的不稳定性实验研究

激波诱导流体界面失稳问题广泛存在于惯性约束核聚变、超燃冲压发动机、武器内爆等工程应用中，相关研究具有重要意义。本文在改进的水平激波管中开展入射激波及其反射激波诱导单模气体界面失稳的实验研究，采用线约束肥皂膜技术生成较为理想的空气/六氟化硫（air/SF₆）单模气体界面，借助高速纹影技术捕捉激波冲击界面后的详细不稳定性演化过程，重点关注反射距离对不稳定性发展的影响（反射距离定义为初始界面和激波管尾端固壁的距离）。研究发现，在一定反射距离范围内，反射激波作用后的扰动增长率几乎为一个恒定值，与反射距离无关（即与反射激波作用前的扰动振幅及增长率无关），随着反射距离的进一步增大，扰动增长率降低。通过实验测量值与理论预测值的对比，发现Mikaelian模型和Charakhch’an模型（采用合适的经验系数）均能对反射激波作用界面后的扰动增长率给予有效预测，且这两种模型的经验系数都依赖于反射激波作用前的界面演化状态，如果反射距离的改变引起/（不引起）界面演化状态的变化，则需要/（不需要）改变经验系数的值。     

机场助航灯光光强动态检测系统

提出了一种机场助航灯光光强动态检测方法，该方法可以替代原有的人工巡检方式，实现快速、准确的在线检测灯光强度，发现灯光故障，保证飞机安全起降与滑行。系统采用安装在车体上的经余弦校正和v（λ）校正的条形照度传感带在水平面内动态扫描助航灯光发光截面，利用车载多普勒测距雷达测量距离，计算相应的光强值，并进而获得等光强图。为了保证系统的可靠性和测量精度，系统中采用了视频导航系统来保证检测车沿助航灯光中心线行驶，利用灯光定位传感器来消除测距雷达测量距离的累积误差。试验表明了该方法的可行性和检测精度。     

测量爆燃到爆震转捩距离的离子探针技术研究

为了测量爆震管中从爆燃到爆震转捩距离,研制了一套基于对比电路的离子探针系统。通过该系统测量爆震管中火焰传播速度的轴向分布,确定了爆燃到爆震的转捩距离。系统结构简单,造价低廉,可用于高温环境下测量。运用该系统测量的乙炔与氧气混合气从爆燃到爆震转捩的距离,其结果与采用高频响的压力传感器系统的测量结果一致。      

双预膜式Hartmann哨超声波喷嘴设计及特性实验研究

为了满足先进航空发动机燃烧系统对燃油雾化质量的要求,设计了一种双预膜式Hartmann哨超声波喷嘴,采用激光粒度分析仪和高速相机对其进行了实验研究,得到了其流量特性和雾化特性。研究结果表明:在满足流量要求下,索太尔平均直径SMD为4.2μm～9μm,气液比ALR为0.27～0.54,液滴尺寸分布集中,均匀性好;在测量范围内,SMD基本不受测量位置到喷嘴出口距离的影响;油压和共振腔到喷嘴出口距离是影响SMD大小的主要因素;雾化角度随油压的变化较小;共振腔到喷嘴出口距离是影响雾化角度的主要因素,雾化角度为135°～180°。     

大尺寸蜗轮齿距累积误差的检测及数据处理

介绍了１种作为工厂机床检修中大尺寸蜗轮距累积误差的检测装置和检测方法，以及用计算机快速准确地进行数据处理。     

An Overview of Results From rpi on Image

The Radio Plasma Imager (RPI) on the Imager for Magnetopause-to-Aurora Global Exploration (IMAGE) spacecraft was designed as a long-range magnetospheric radio sounder, relaxation sounder, and a passive plasma wave instrument. The RPI is a highly flexible instrument that can be programmed to perform these types of measurements at times when IMAGE is located in key regions of the magnetosphere. RPI is the first radio sounder ever flown to large radial distances into the magnetosphere. The long-range sounder echoes from RPI allow remote sensing of a variety of plasmas structures and boundaries in the magnetosphere. A profile inversion technique for RPI echo traces has been developed and provides a method for determining the density distribution of the plasma from either direct or field-aligned echoes. This technique has enabled the determination of the evolving density structure of the polar cap and the plasmasphere under a variety of geomagnetic conditions. New results from RPI show that the plasmasphere refills in slightly greater than a day at L values of 2.8 and that ion heating is probably playing a major role in the overall density distribution along the field-line. In addition, RPI's plasma resonance observations at large radial distances over the polar cap provided in situ measurements of the plasma density with an accuracy of a few percent. For the first time in the magnetosphere, RPI has also observed the plasma D resonances. RPI's long antennas and its very low noise receivers provide excellent observations in the passive receive-only mode when the instrument measures the thermal plasma noise as well as natural emissions such as the continuum radiation and auroral kilometric radiation (AKR). Recent passive measurements from RPI have been compared extensively with images from the Extreme Ultraviolet (EUV) imager on IMAGE resulting in a number of new discoveries. For instance, these combined observations show that kilometric continuum can be generated at the plasmapause from sources in or very near the magnetic equator, within a bite-out region of the plasmasphere. The process by which plasmaspheric bite-out structures are produced is not completely understood at this time. Finally, RPI has been used to successfully test the feasibility of magnetospheric tomography. During perigee passages of the Wind spacecraft, RPI radio transmissions at one and two frequencies have been observed by the Waves instrument. The received electric field vector was observed to rotate with time due to the changing density of plasma, and thus Faraday rotation was measured. Many future multi-spacecraft missions propose to use Faraday rotation to obtain global density pictures of the magnetosphere.     

The Galileo Dust Detector

The Galileo Dust Detector 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 system, to investigate their physical and dynamical properties as functions of the distances to the Sun, to Jupiter and to its satellites, to study its interaction with the Galilean satellites and the Jovian magnetosphere. Surface phenomena of the satellites (like albedo variations), which might be effects of meteoroid impacts will be compared with the dust environment. Electric charges of particulate matter in the magnetosphere and its consequences will be studied; e.g., the effects of the magnetic field on the trajectories of dust particles and fragmentation of particles due to electrostatic disruption. The investigation is performed with an instrument that measures the mass, speed, flight direction and electric charge of individual dust particles. It is a multicoincidence detector with a mass sensitivity 10⁶ times higher than that of previous in-situ experiments which measured dust in the outer solar system. The instrument weighs 4.2 kg, consumes 2.4 W, and has a normal data transmission rate of 24 bits s^-1 in nominal spacecraft tracking mode. On December 29, 1989 the instrument was switched-on. After the instrument had been configured to flight conditions cruise science data collection started immediately. In the period to May 18, 1990 at least 168 dust impacts have been recorded. For 81 of these dust grains masses and impact speeds have been determined. First flux values are given.     

水平冲击下头排乘员损伤及保护姿势研究

为研究水平冲击下不同参数对于头排乘员损伤的影响及不同保护姿势的保护效果。首先进行水平16g动态冲击试验，建立相应的数值模型，验证模型有效性；其次通过正交试验设计进行参数研究，揭示头排座椅间距、安全带刚度、隔板刚度、安全带固定点位置对于乘员损伤的影响；最后研究直立式、抱脚式、手顶式3种姿势对于头排乘员的保护效果。结果表明头排座椅间距以及隔板刚度对乘员头部损伤影响显著；头排乘员头部、颈部、股骨、胫骨损伤对安全带材料特性及安全带固定点位置不敏感；抱脚式、手顶式保护姿势均对头排乘员头部有较好的保护效果。在水平冲击下采用头部前倾的抱脚式保护姿势可使头排乘员头部、颈部、股骨及胫骨损伤均小于限定值。     

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.     

The Multi-Needle Langmuir Probe System on Board NorSat-1

On July 14th, 2017, the first Norwegian scientific satellite NorSat-1 was launched into a high-inclination (98^°), low-Earth orbit (600 km altitude) from Baikonur, Kazakhstan. As part of the payload package, NorSat-1 carries the multi-needle Langmuir probe (m-NLP) instrument which is capable of sampling the electron density at a rate up to 1 kHz, thus offering an unprecedented opportunity to continuously resolve ionospheric plasma density structures down to a few meters. Over the coming years, NorSat-1 will cross the equatorial and polar regions twice every 90 minutes, providing a wealth of data that will help to better understand the mechanisms that dissipate energy input from larger spatial scales by creating small-scale plasma density structures within the ionosphere. In this paper we describe the m-NLP system on board NorSat-1 and present some first results from the instrument commissioning phase. We show that the m-NLP instrument performs as expected and highlight its unique capabilities at resolving small-scale ionospheric plasma density structures.     

基于Labview的谐振式微光学陀螺锁频环路设计

谐振式微光学陀螺(RMOG) 是通过检测基于Sagnac效应产生的谐振频率差来测量旋转角速度的一种新型光学传感器。针对RMOG检测电路信号质量差、功能单一,无法兼容不同光路结构的问题,提出了基于虚拟仪器的RMOG数字控制方案,利用Labview编程的灵活性,完成了锁频环路的设计并进行了实验验证,实验结果表明1h陀螺锁频精度为0.03 °/s。1 h的输出精度为1.4 °/s。     

The Lightning And Radio Emission Detector (LRD) instrument

The Lightning and Radio Emission Detector (LRD) instrument will be carried by the Galileo Probe into Jupiter's atmosphere. The LRD will verify the existence of lightning in the atmosphere and will determine the details of many of its basic characteristics. The instrument, operated in its magnetospheric mode at distances of about 5, 4, 3, and 2 planetary radii from Jupiter's center, will also measure the radio frequency (RF) noise spectrum in Jupiter's magnetosphere. The LRD instrument is composed of a ferritecore radio frequency antenna ( 100 Hz to 100 kHz) and two photodiodes mounted behind individual fisheye lenses. The output of the RF antenna is analyzed both separately and in coincidence with the optical signals from the photodiodes. The RF antenna provides data both in the frequency domain (with three narrow-band channels, primarily for deducing the physical properties of distant lightning) and in the time domain with a priority scheme (primarily for determining from individual RF waveforms the physical properties of closeby-lightning).     

Development and Effects of Turbulence in Connection with CIRs

We present an overview of the properties of magnetohydrodynamic turbulence within corotating interaction regions (CIRs) and its effects on energetic particles. We stress the importance of both the population of fluctuations in the inner heliosphere and the changing local environment in determining their properties at larger heliospheric distances. We present observations from two typical CIRs, one at 0.3 AU before compression regions have formed and the other well developed at 5.1 AU, and discuss the properties of fluctuations within them and show that it is possible to distinguish different regions of the CIR on the basis of the turbulence itself. The strength of the turbulence varies strongly within and close to the CIRs, explaining changes in the mean free path of energetic particles of several orders of magnitude with implications for the modulation of cosmic rays and for diffusive acceleration of particles. The mechanisms by which turbulent fluctuations within interaction regions scatter energetic particles are briefly discussed on a theoretical basis. This revised version was published online in August 2006 with corrections to the Cover Date.     

Ultrasound assisted solidification process of ternary Cu–Sn–Sb alloy

It is well-known that the application of ultrasound during liquid to solid transitions for alloys can refine the solidification microstructure and thus improves the mechanical properties. How-ever, most published work focuses on single phase dendritic growth, whereas little has been con-ducted on the multiphase alloys with complicated phase transformations during solidification. In this work, the solidification process of ternary Cu40Sn45Sb15 alloy was realized within intensive ultra-sonic field with a resonant frequency of 20 kHz and ultrasound power from 0 W to 1000 W. The ultrasound refines the size of the primary e(Cu3Sn) intermetallic compound by two orders of mag-nitudes. If the ultrasound power increases to 1000 W, g(Cu6Sn5) phase nucleates and grows directly from parent liquid phase without the occurrence of peri-eutectic reaction on the top of the alloy sam-ple where the ultrasound intensity is sufficiently high. These microstructural variations lead to the enhancement of compressive strength and elasticity modulus of ternary Cu40Sn45Sb15 alloy.