T-1A型高精度绝对重力仪

高精度绝对重力仪用于测量地球表面的重力加速度（g,常用值9.81 m/s2）,在精密计量、大地测量、地球物理、资源勘探等领域具有广泛应用。近年来,清华大学自主研制完成T-1与T-1A型高精度绝对重力仪,采用新型的自由落体装置、激光干涉测量技术和信号处理方法,可实现微伽量级不确定度的精密重力测量。本文主要介绍T-1A型高精度绝对重力仪的系统技术和测试结果,经过进一步工程化改进,该仪器有望实际应用于重力计量、地震研究等领域。     

Challenges in the Measurement and Data-Processing Chain of the LISA Mission

The LISA Mission (Laser Interferometer Space Antenna) is currently under mission formulation with a launch date planned in 2020. The purpose of the mission is the observation of gravitational waves at frequencies between 0.1 mHz and 1 Hz by measuring distance fluctuations between inertial reference points, represented by cubic proof masses. In order to provide a sufficient sensitivity of the instrument, distance fluctuations between two inertial reference points must be measured with a strain accuracy of around 10^?20 Hz^?1/2. This is achieved by setting up a laser interferometer with a base-length of 5?10⁶ km and a path-length measurement noise in the order of 10 pm?Hz^?1/2. For a correct evaluation of the data on the ground, it is essential that the science data telemetry preserves all required frequency domain information. That is, any on-board data-processing and down-sampling must be done with great care in order not to introduce aliasing or other artifacts into the data stream. As an additional complication, most of the optical metrology data is dominated by laser phase noise which is about eight orders of magnitude larger than the required instrument sensitivity. However, by applying a method called “time-delayed interferometry” during the ground data processing, this laser phase noise can be eliminated from the data. This method has already been demonstrated in a detailed simulation environment, but it requires a very careful filtering, synchronization, and interpolation of the individual data streams. Last but not least, a calibration of system parameters is necessary in many areas of the LISA measurement system. The system design must therefore ensure that all data required for these calibrations is available on-ground in a quality that allows a successful computation of the calibration coefficients within a reasonable time-frame. The data streams do not only include data from the optical metrology system, but also from the drag-free and attitude control system which are used to derive other information, such as the charge state of the proof mass. This yields a strong coupling between the different disciplines since data that is only used for housekeeping purposes in other missions becomes an essential part of the science data stream for the LISA mission. This paper gives an overview of the LISA measurement and data-processing chain. It highlights the most challenging areas that have been identified so far and describes the intended solution methods.     

Geodetic Methods for Calibration of GRACE and GOCE

It is beyond doubt that calibration and validation are essential tools in the process of reaching the goals of gravity missions like GRACE and GOCE and to obtain results of the highest possible quality. Both tools, although general and obvious instruments for any mission, have specific features for gravity missions. Therefore, it is necessary to define exactly what is expected (and what cannot be expected) from calibration and what from validation and how these tools should work in our case. The general calibration and validation schemes for GRACE and GOCE are outlined. Calibration will be linked directly to the instrument and the measurements whereas validation will be linked to data derived from the original measurements. Calibration includes on-ground, internal, and external calibration as well as error assessment. The calibration phase results in corrected measurements along with an a posteriori error model. Validation of e.g. calibrated measurements or geoid heights means checking against independent data to assess whether there are no systematic errors left and/or whether the error model describes the true error reasonably well. Geodetic methods for calibration typically refer to external calibration and error assessment, and will be illustrated with an example. This revised version was published online in August 2006 with corrections to the Cover Date.     

Dynamic Modelling of the Hipparcos Attitude

We present a new method for a high-accuracy reconstruction of the attitude for a slowly spinning satellite. This method, referred to as the fully-dynamic approach, explores the possibility to describe the satellite's attitude as that of a rigid body subject to continuous external torques. The method is tried out on the Hipparcos data and is shown to reduce the noise for the along-scan attitude reconstruction for that mission by about a factor two to three. The dynamic modelling is expected to give a more accurate representation of the satellite's attitude than was obtained with a pure mathematical modelling. As such, it decreases the degrees of freedom in the a posteriori reconstruction. Some of the decrease is obtained through accumulating and subsequently implementing information on high frequency components in the solar radiation torques, which show to be systematic and predictable. This could be expected, as they are primarily linked to the external geometry and optical properties of the satellite. In the context of an astrometric mission, the methods presented here can only be applied as a final iteration step: the star positions that are used to reconstruct the attitude are also part of the scientific objectives of the mission. An estimate for the potential of a re-reduction of the Hipparcos data using the fully-dynamic model for the attitude reconstruction was obtained from test reductions of the first 24 months of mission data. Improvement of the accuracies of the astrometric parameters for all stars brighter than Hp=9.0 appears possible. The noise on the astrometric parameters for these stars was affected significantly by the along-scan attitude noise, which dominated for stars brighter than Hp=4.5. The possible improvement for stars brighter than about Hp=4.5 may, after iterations, be as much as a factor three. The reduced noise levels also allow a more accurate calibration and monitoring of instrument parameters, leading potentially to a better understanding of the instrument and the scientific data obtained with it. This revised version was published online in August 2006 with corrections to the Cover Date.     

数控机床几何误差测量研究现状及趋势

数控机床作为现代制造加工业的"工业母机",是衡量国家制造业的重要标志。随着技术的发展,对机床加工精度的要求越来越高。因此,我国数控机床精度和精度保持性面临着严峻的挑战,如何快速准确测量数控机床的各种误差成为该领域的一个研究热点和重点。首先从测量仪器角度以及测量策略研究角度回顾了数控机床激光干涉测量、激光跟踪测量、空间体积误差测量、球杆仪测量、平面光栅测试、R-Test、标准件测试等主要几何误差综合测量方法,并对热误差、力误差等相关研究做了简要回顾。在此基础上,分析了当前数控机床误差测量面临的主要挑战以及下一步的发展趋势,为国产数控机床误差测量方法与技术发展提供了建议。     

Galileo radio science investigations

The radio science investigations planned for Galileo's 6-year flight to and 2-year orbit of Jupiter use as their instrument the dual-frequency radio system on the spacecraft operating in conjunction with various US and German tracking stations on Earth. The planned radio propagation experiments are based on measurements of absolute and differential propagation time delay, differential phase delay, Doppler shift, signal strength, and polarization. These measurements will be used to study: the atmospheric and ionospheric structure, constituents, and dynamics of Jupiter; the magnetic field of Jupiter; the diameter of Io, its ionospheric structure, and the distribution of plasma in the Io torus; the diameters of the other Galilean satellites, certain properties of their surfaces, and possibly their atmospheres and ionospheres; and the plasma dynamics and magnetic field of the solar corona. The spacecraft system used for these investigations is based on Voyager heritage but with several important additions and modifications that provide linear rather than circular polarization on the S-band downlink signal, the capability to receive X-band uplink signals, and a differential downlink ranging mode. Collaboration between the investigators and the space-craft communications engineers has resulted in the first highly-stable, dual-frequency, spacecraft radio system suitable for simultaneous measurements of all the parameters normally attributed to radio waves.     

一种新型测距仪的研制

介绍了一种在中，小范围内，采用激光定位，超声测距的新型测量仪器，该仪器以单片微处理器为核心，对不同的测量距离，采用不同频率的超声波，结合信号处理方法，从而实现０．６～１４ｍ范围内高精度实时测量目标距离，其测量相对误差优于１％。     

基于自抗扰理论的小型四旋翼飞行器姿态控制

针对四旋翼飞行器的强耦合性、非线性、易受外界干扰等控制难点,研究利用自抗扰控制器对四旋翼飞行器进行姿态控制的技术问题。通过牛顿-欧拉方程建立四旋翼飞行器动力学模型,将不确定性、耦合及参数摄动等干扰作为"总和干扰",利用扩张状态观测器进行估计并动态反馈补偿,再利用非线性反馈抑制补偿残差,进行四旋翼飞行器姿态控制仿真实验。结果表明:在存在模型参数摄动和外界扰动的情况下,扩张状态观测器很好地实时估计和补偿了四旋翼飞行器的总和干扰,基于自抗扰的四旋翼飞行器姿态控制系统具有较好的动态品质、稳态精度以及较强的鲁棒性。     

Ф300mm大口径平面等厚干涉仪波面数字化技术改造

介绍了把Ф300 mm口径平面等厚干涉仪改造为移相式数字平面干涉仪的基本情况。改造后的仪器采用液面基准的系统误差校准方法,在Ф300 mm口径时的最大允许误差为76 nm（PV值）,测量重复性为4 nm,满足相关使用要求。     

原子干涉陀螺仪关键技术及进展

原子作为一种微观粒子,具有波粒二象性.利用粒子的波动性,可以产生类似于光波的Sagnac效应,由此实现基于原子波干涉的原子干涉陀螺仪.其中原子干涉有内态干涉和物质波干涉两种.在围成相同面积的情况下,原子干涉陀螺仪的灵敏度将比光学陀螺仪高出10个量级以上,适宜于水下和空间等长时间惯性导航的应用.本文详细地论述了原子干涉陀...     

纳米力学测试系统位移传感器校准装置

介绍了用激光干涉方法对纳米力学测试系统位移传感器进行校准的方法,并建立了校准装置;采用平衡式光学系统设计,干涉系统的抗干扰能力得到了显著提高,通过零位移测量实验对装置的稳定性进行了验证;用校准装置对TriboIndenter纳米力学测试系统的位移传感器进行了校准实验,测量不确定度分析结果表明该系统测量压头位移的准确度可以达到纳米量级。     

A Smart Low-Power Meteorological System

A new low-power instrument to measure meteorological parameters has been developed. The instrument is based on an intelligent data cruncher concept: Fast sensor data rates are stored and process to yield a variety of answers for each parameter, at slower data rates, as appropriate. Special methods are used to achieve these results with an average current drain of under one mA, including sensors. Sampling rates and processing algorithms are designed to correct for swaying ocean-deployed buoys. A modular approach to design allows many types of sensors to be accommodated and permits data dissemination to a variety of destinations; data is available for real-time transmission or for internal archiving. The Weather Station's high-capacity internal data storage system, coupled with its fast data acquisition rates, enable the instrument to be used for air turbulence measurements.     

基于RTX子系统的导弹试验实时测控系统

导弹试验实时测控系统是空空导弹制导系统半实物仿真试验平台的主要设备之一,服务于新型导弹的研制、试验、优化和评估。系统采用RTX实时开发技术,克服了Windows系统实时性差的局限性,解决了测控系统实时与非实时任务兼容处理难的问题,实现了空空导弹半实物仿真试验的实时仿真和实时测控。系统利用RTX子系统的开放性,重新开发了所用仪器板卡在RTX环境下的驱动程序,实现了应用程序的设备无关性,提高了导弹试验验证的有效性和系统性。     

椭圆振动切削加工的同步控制研究

利用椭圆振动切削加工的回转体表面微织构是在机床主轴旋转、平台进给和装置椭圆振动的联合运动下得到的,机床主轴转动与装置位移输出如果不能保持完全的实时同步,会造成微织构加工的偏差。为了解决这一问题,提出了一种新的基于转角的同步控制方法,该方法在主轴的对位基准处实现装置正弦信号的复位,以修正转速漂移造成的加工位置误差,并通过判断主轴角度信号实时输出对应幅值电压来实时同步信号输出和机床旋转运动。基于LabVIEW FPGA搭建同步控制模块,经试验验证,利用该方法加工的矩形阵列微织构轴向排列与中轴线平行,与周向排列的夹角和仿真结果的偏差不超过0.1°,织构深度随转角的不同发生预设的变化,因此,同步控制方法具有实时同步控制椭圆振动切削装置的能力。     

滚转弹两框架导引头的前馈补偿技术

针对弹体滚转情况下两框架平台式导引头的伺服控制问题,基于导引头运动学和动力学,建立了导引头稳定回路模型。结合弹体滚转条件下的导引头输入指令和输出视线角速率关系,构建了视线闭环回路。针对偏航、俯仰通道间的解耦控制问题,推导出解耦条件,要求两通道由失调角到光轴转动角速度的传递函数相同。仿真分析了该模型在视线角输入以及弹体姿态扰动输入时,弹体滚转对导引头跟踪精度产生的影响,并由此提出了滚转角速度前馈补偿控制方案。结果表明,采用结合滚转角前馈补偿控制的两框架平台式导引头方案可以满足滚转弹的制导精度要求。     

Laser Interferometer for High Sensitivity Measurements on Transient Phase Objects

A He-Ne laser beam is sent through a common path differential interferometer and the interference signal is detected by a p-i-n photodiode. Weak phase objects can be examined because optical path changes can be resolved to 0.1 ? with a time resolution of about 20 ns. Examples for different gas-dynamic investigations show good results and demonstrate the wide field of application for this type of laser interferometer.     

基于动基座重力梯度仪的导弹主动段飞行状态估计

弹道导弹主动段由于惯导系统工具误差和扰动引力的影响,使得导弹关机点状态参数偏离标准关机状态参数,大大影响了导弹的命中精度.为此,提出了基于动基座重力梯度仪的导弹主动段飞行状态估计方案,利用动基座重力梯度仪测得的导弹实际位置引力梯度信息,采用卡尔曼滤波方法,修正导弹当前的飞行状态.通过初步仿真,证明该方法理论上是可行的.     

高频振荡器噪声分析

 本文将高频振荡器视为具有深度正反馈噪声放大器。对它分析,给出正弦波信号的谱、等效带宽及相位噪声谱;同时还提出诸如高频振荡器内部产生的随机游走噪声形成机理等新看法。     

基于自适应Kalman滤波的导引头随动系统设计

主要研究导引头随动系统中探测器信号处理延迟的影响及其补偿控制算法。提出了一种自适应Kalman滤波延迟补偿方案,利用Kalman滤波的预测能力得到当前时刻视线角的估计值,进而得到此时的跟踪误差的估计值,取代被延迟的探测器输出进行闭环控制。考虑到导引头探测器的低更新频率、非等间隔量测等工程特点,又对上述滤波算法进行了一系列改进。仿真表明方法可以明显提高导引头在弹体扰动情况下的跟踪精度。     

Prospects for space stellar astrometry

Astrometry is the major astronomical technique to measure distances, masses and motions of stars. Dividing astrometric techniques into five types according to the size of the field in which a single instrument can produce measurements, the present achievements of the Earth-based astrometry are described. The astrometric activities such as measurements of star diameters, double star relative positioning or stellar parallaxes, search for invisible companions, photographic plate reduction, visual and photoelectric meridian and astrolable astrometry are reviewed. Then, the methods used to construct a quasi-inertial celestial reference frame and to materialize it by a fundamental catalogue are presented and discussed. A much better definition of an absolute reference frame is made possible by VLBI, but the problem of extending it to stellar positions is not yet satisfactorily resolved.The limitations of the ground based astrometry are: the atmospheric turbulence and refraction, Earth's motions and the impossibility to view the entire sky with a single instrument. These limitations are discussed and it is shown how astrometry from space can overcome them. A priori, a gain of two orders of magnitudes in accuracy for all types of astrometry is expected, but at this new level of precision, new effects and limitations will appear, as already shown in the studies of the approved programs.Then, the ESA astrometric satellite HIPPARCOS presently under development is presented. The satellite and the payload are described as well as the observing procedures. Several limitations, specific to space borne instrumentation and to the milliarc second accuracy expected have been identified. However the main limitation in precision remains the photon noise. The data reduction methods are sketched. The data downlinked at a rate of 20 kilobits per second have to be used with an equal weight all over the 21/2 years of observation. They are expected to yield a mean accuracy of 2 milliarc seconds in position and parallax and 2 m.a.s. per year in proper motion for most of the 100000 stars of the program (M _b < 9). Stars to be observed by HIPPARCOS have to be carefully selected. The main fields in which the results of HIPPARCOS will be used are listed from the proposals made by the scientific community. The task of constructing the HIPPARCOS input catalogue from these proposals is presented.Another feature of the ESA astrometric satellite is the use of the HIPPARCOS star-mapper as a photometric and position survey of the sky. This experiment, called TYCHO, should give at least 400000 star positions with accuracies of the order of 0.03 to 0.15 depending upon the magnitudes. Two colour instantaneous magnitudes should also be obtained to 0.1–0.4 mag. precision.Several Space-Telescope on-board instruments are also capable to make small field astrometric observations. Accurate imaging is possible with the Wide Field and the Faint Object cameras. Lunar occultations will be performed with the High Speed photometer. But the main astrometric mode of the Space Telescope will be the use of the Fine Guidance Sensors to measure the relative positions of stars to ±0.002. It is described together with its main scientific applications.The establishment of an absolute reference frame is subsequently discussed. Plans using simultaneously VLBI, HIPPARCOS, and Space Telescope observations are described. They consist in linking the HIPPARCOS stellar system to quasars via radio-stars or stars in the vicinity of optical quasars.Finally, several space astrometry proposals are described: long focus space astrometry and two versions of space interferometry.