赛佛特星系金属丰度的求解

对于赛佛特星系(文中简称WR星系),作为一种重要的活动星系的类型,求其金属丰度对我们具有重要的意义,本文将详细介绍计算HII区星系金属丰度的方法,并据此计算若干赛佛特星系的金属丰度。     

斜切口喷管的性能计算

本文综述了适应不同用途的,各种结构形式的斜切口喷管的性能计算问题。对在一定条件下,斜切口喷管内流动可简化为一元流的计算作了详细讨论;对二元流及三元流的分析作了简要的介绍。     

圆滑曲线槽的铣切加工

本文详细地介绍了如何利用直线与圆的方程来计算转接小圆弧的中心尺寸,如何计算各段圆弧所对的圆心角;如何精确地计算二直线段的长度;并详细叙述了在普通铣床上用立铣刀加工曲线槽的工艺过程及操作方法。 经实践证明,计算方法正确无误,工艺过程合理,操作简便,取得了良好的效果。     

典型散射体低频特性估计

本文探讨了几种典型金属物体的低频散射问题。介绍了低频散射截面的计算方法；对计算结果进行了分析；并就雷达目标低频散射特性提出了作者的观点。     

利用协方差矩阵研究有限多次点火时轨道转移误差

以低加速度从航天飞机的低地球轨道转移到对地静止轨道,需要有限多次点火。在这种情况下,轨道转移入轨误差的研究变得较为复杂。一般说来,协方差解析法不适用了,必须采用半解析法或数字法。本文经过论证指出,可以在近地点点火段采用半解析法,在远地点点火段采用解析法,从而可以节省大量计算时间。本文给出了近地点点火、远地点点火和轨道滑行段的传递矩阵,也给出了轨道元素协方差转换矩阵。文中还详细介绍了计算机程序的流程图和检验方法。最后给出了一个计算实例。     

超高真空环境冷焊与防冷焊试验现状与建议

国外的冷焊试验从环境压力(真空度)、试件温度、试验接触面的法向压力、试验表面光洁度污染情况以及接触面是否有相对运动等主要影响因素进行分析;同时采用用于冷焊效应研究的环境试验卫星进行空间冷焊试验;在冷焊防护方面也进行了大量飞行试验及地面模拟试验,试验表明三氧化二铝、二氧化锆、三氧化二铬及二硫化钼等薄膜层能有效降低金属面间的摩擦系数,可以防止冷焊效应的发生。国内冷焊试验主要是地面模拟试验,文章对国内各种超高真空冷焊及防冷焊试验设备分别从用途、技术指标和设备组成等几方面作了详细介绍。并对今后这方面的研究方向提出了建议。     

浅谈后勤装备全寿命费用的计算方法

介绍了GJB 1625—93《军事后勤装备全寿命费用计算方法》中规定的三种计算方法——模拟法、参数法、工程法的适用范围,并对每种方法在后勤装备全寿命周期内的有关阶段如何应用作了说明。     

正弦振动试验及结构响应数据处理方法

文章介绍了航天器动力学环境试验中常用的正弦振动试验技术及其试验过程中结构响应测量的数据处理方法,特别就数据处理的4种峰值计算方法作了较详细的阐述.     

载人飞船再入轨道计算及升力控制规律的研究

介绍了载人飞船返回轨道的计算方法,讨论了当前流行的两种飞船再入制导的方法(标准轨道法和预测落点法),并且提出了一种新的预测落点法的纵向制导控制规律。通过仿真计算得到飞船再入的标准轨道,利用两种控制规律进行仿真计算,并对两种制导方法的结果作了比较。     

航天器研制全过程污染控制工程

污染控制体系的完善,控制技术的成熟,对航天器研制至关重要,本文简要说明了污染控制的重要性,以及由于污染造成航天器失效的例子,比较详细地介绍了航天器项目各阶段污染控制的一些方法,最后简要介绍了污染领域的发展方向和急需解决的问题。     

Astrobiologically interesting stars within 10 parsecs of the sun

The existence of life based on carbon chemistry and water oceans relies upon planetary properties, chiefly climate stability, and stellar properties, such as mass, age, metallicity, and galactic orbits. The latter can be well constrained with present knowledge. We present a detailed, up-to-date compilation of the atmospheric parameters, chemical composition, multiplicity, and degree of chromospheric activity for the astrobiologically interesting solar-type stars within 10 parsecs of the Sun. We determined their state of evolution, masses, ages, and space velocities, and produced an optimized list of candidates that merit serious scientific consideration by the future space-based interferometry probes aimed at directly detecting Earthsized extrasolar planets and seeking spectroscopic infrared biomarkers as evidence of photosynthetic life. The initially selected stars number 33 solar-type within the total population (excluding some incompleteness for late M-dwarfs) of 182 stars closer than 10 parsecs. A comprehensive and detailed data compilation for these objects is still lacking; a considerable amount of recent data has so far gone unexplored in this context. We present 13 objects as the nearest "biostars," after eliminating multiple stars, young, chromospherically active, hard x-ray- emitting stars, and low metallicity objects. Three of these "biostars"-- Zeta Tucanae, Beta Canum Venaticorum, and 61 Virginis -- closely reproduce most of the solar properties and are considered as premier targets. We show that approximately 7% of the nearby stars are optimally interesting targets for exobiology.     

卫星自主导航技术发展综述

综述了国外卫星自主导航技术的研究历史和现状 ,简要地介绍了国外的麦氏自主导航系统、星光折射 /星光色散法自主导航系统和基于雷达高度计的自主导航系统的研制情况、特点及导航精度 ,为确立我国研制卫星自主导航系统的技术路线提供参考     

Operation and performance of a second generation, solid state, star tracker, the ASC

The Advanced Stellar Compass (ASC) is a second generation star tracker, consisting of a CCD camera and its associated microcomputer. The ASC operates by matching the star images acquired by the camera with its internal star catalogs. An initial attitude acquisition (solving the lost in space problem) is performed, and successively, the attitude of the camera is calculated in celestial coordinates by averaging the position of a large number of star observations for each image. Key parameters of the ASC for the Ørsted satellite and Astrid II satellite versions are: mass as low as 900 g, power consumption as low as 5.5W, relative attitude angle errors less than 1.4 arcseconds in declination, and 13 arcseconds in roll, RMS, as measured at the Mauna Kea, HI observatories of the University of Hawaii in June 1996.     

A model of habitability within the Milky Way galaxy

We present a model of the galactic habitable zone (GHZ), described in terms of the spatial and temporal dimensions of the Galaxy that may favor the development of complex life. The Milky Way galaxy was modeled using a computational approach by populating stars and their planetary systems on an individual basis by employing Monte Carlo methods. We began with well-established properties of the disk of the Milky Way, such as the stellar number density distribution, the initial mass function, the star formation history, and the metallicity gradient as a function of radial position and time. We varied some of these properties and created four models to test the sensitivity of our assumptions. To assess habitability on the galactic scale, we modeled supernova rates, planet formation, and the time required for complex life to evolve. Our study has improved on other literature on the GHZ by populating stars on an individual basis and modeling Type II supernova (SNII) and Type Ia supernova (SNIa) sterilizations by selecting their progenitors from within this preexisting stellar population. Furthermore, we considered habitability on tidally locked and non-tidally locked planets separately and studied habitability as a function of height above and below the galactic midplane. In the model that most accurately reproduces the properties of the Galaxy, the results indicate that an individual SNIa is ～5.6× more lethal than an individual SNII on average. In addition, we predict that ～1.2% of all stars host a planet that may have been capable of supporting complex life at some point in the history of the Galaxy. Of those stars with a habitable planet, ～75% of planets are predicted to be in a tidally locked configuration with their host star. The majority of these planets that may support complex life are found toward the inner Galaxy, distributed within, and significantly above and below, the galactic midplane.     

卫星控制仿真数据库管理系统软件的自动化测试

介绍了“卫星控制仿真数据库管理系统”软件的自动化测试工作。重点分析了测试脚本生成方法,指出基于记录-回放的测试脚本生成技术的缺陷在于测试脚本与数据及实现细节的耦合。最后,应用基于数据驱动的脚本设计技术和模块化脚本设计思想实现了一个自动化测试脚本框架,解决了测试脚本与数据及实现细节的耦合问题,从而提高了脚本设计质量,降低了脚本维护成本。     

Influence of sensor and actuator errors on impulsive satellite formation control methods

This paper investigates how sensor and actuator errors are impacting formation control accuracy and propellant consumption of a two-satellite formation in a low Earth orbit. Realistic relative navigation errors are implemented, based on the results from the PRISMA mission, as well as realistic actuator uncertainty and actuator constraints. Two impulsive control methods are investigated. The first method is based on a controller that is implemented onboard PRISMA and the second method uses linear programming to arrive at a model predictive controller. The control methods are tested in a simulation environment and are subjected to orbital perturbations and realistic sensor errors and actuator errors. Both control methods are able to maintain the desired relative geometry of a projected circular orbit in the presence of the errors. The PRISMA control method demonstrates lower propellant consumption, while the model predictive controller shows better control accuracy. The results show that, based on the used scenario, sensor errors dominate both the formation control accuracy and propellant consumption. The versatility of the model predictive controller is demonstrated in a challenging formation control scenario including formation maintenance and formation reconfiguration tasks.     

螺栓连接松动的导波监测技术综述

螺栓连接件使结构易于安装或拆卸,同时还可以承受较大的载荷,广泛应用于航空航天结构中。然而,螺栓在复杂服役环境中很容易发生松动,因此准确监测螺栓预紧力对于确保结构的可靠性和安全性具有重要意义。经过多年的发展,基于超声导波的结构健康监测方法逐渐成为螺栓连接松动监测的重要技术手段之一。对典型的螺栓预紧力导波监测方法进行了综述,包括导波能量耗散法、时间反转法、接触声学非线性法和混沌超声法等方法,介绍了这些方法的基本原理和发展现状。同时,通过实验将目前应用较多的导波能量耗散法、时间反转法进行了对比,结果表明时间反转法的监测灵敏度更高。     

基于结构特征的弹道目标雷达识别技术

弹道目标的结构特征反映了目标的本质属性,是识别真假目标最直观的特征之一。分析了弹道目标的结构特征差异,系统归纳了基于结构特征的弹道目标雷达识别方法。根据雷达提取结构特征所采用的信息不同,将这种识别方法分为基于RCS序列的识别方法、基于一维像的识别方法、基于二维像的识别方法以及基于极化信息的识别方法,详细阐述了这四类识别方法的物理基础及其实现途径,分析了它们各自的特点,最后展望了技术发展趋势。