自调节模拟低通滤波器的研究

通过对有源低通滤波器，频率／电压转换器AD650及其变容二极管的特性分析，提出由信号频率来自调节有源低通滤波器截止频率的新设计方案，并对其可行性进行了分析和研究。     

XMM-Newton temperature maps for five intermediate redshift clusters of galaxies

We have analyzed XMM-Newton archive data for five clusters of galaxies (redshifts 0.223–0.313) covering a wide range of dynamical states, from relaxed objects to clusters undergoing several mergers. We present here temperature maps of the X-ray gas together with a preliminary interpretation of the formation history of these clusters.     

基于A320飞机横航向控制律架构的LQ设计

前缘缝翼、襟翼活动面及其支承结构的疲劳试验是民用飞机取证前要开展的一项重要工作。在试验中采用主动驱动和随动加载方法加载,不仅能缩小试验规模,同时可提高试验精度。国内某型机采用此技术成功进行了前缘缝翼、襟翼及其悬挂结构的疲劳试验。从试验件及其支承设计、系统构成和载荷与运行三方面,介绍了一种适用于大中型固定翼飞机前缘缝翼和襟翼的疲劳试验技术。     

Extragalactic observations and future missions

We briefly review some questions of extragalactic astrophysics and cosmology that would most benefit from future missions outside the Earth's atmosphere in the IR and submillimeter. These include the formation and early evolution phases in galaxies and the probably related question of quasar formation; the observation of Active Galactic Nuclei embedded in thick dusty structures (torii) and its impact on the still debated unified model of AGN activity; the observability of radiation processes occurring at very highz through background measurements; the investigation of the large scale structure and velocity field in the distant universe; and studies of the interstellar medium in galaxies. Some more emphasis is given on the galaxy formation problem, because we believe that IR-mm sensitive observations will be crucial to its final solution.     

行星际航天器主动热控系统模糊控制

对行星际航天器主动热控系统进行了研究。以“火星探路者”号为例，在其机械泵式单相液体循环冷却系统设计布局的基础上，使用更高换热效率、更低压力降的分形微管道网络换热器传递电子设备散发的热量，利用模糊控制策略对系统进行控制。通过合理的简化和假设，应用集总参数法建立系统动态特性模型，进行仿真研究。结果表明此主动热控系统能对航天器电子设备温度进行有效控制。     

主动控制式对接机构对接预捕获阶段的仿真

介绍了主动控制式对接机构对接的基本操作过程，并以具有六个作动阻尼器的主动接制式对接机构为例，对对接预捕获阶段作了详细的研究。 该阶段两对接飞行器的运动方程，给出了作动／阻尼器为满足捕获条件所需达到的长度的计算方法，设计了控制回路，在此基础上作了数值仿真。仿真结果表明，建立的数学模型是正确的，设计的控制系统控制效果良好。     

细长体双自旋卫星消旋主动章动控制动力学解耦的系统仿真

细长体双自旋卫星自旋部分的能量耗散会导致卫星章动运动的发散。利用消旋体的惯性积在动力学上的耦合作用,使消旋电机的轴向力矩通过耦合,产生横向力矩来阻尼章动,称之为消旋主动章动控制（ＤＡＮＣ）［１］。本文提出一种利用动力学解耦的仿真方案,用单轴平台进行细长体双自旋卫星消旋和章动控制的系统试验,验证了系统的可行性。     

柔性多体卫星自抗扰控制系统的研究

设计了一种新型的姿态控制器一姿态自抗扰控制器。采用简化了的刚体动力学模型，即把柔性太阳帆板与柔性天线等的振动都看作外干扰，对象的不确定性、未建模动态与外干扰的总量都由自抗扰控制器估计出，再用该估计总量实现动态反馈补偿。该姿态控制器，只需控制输入转换矩阵的估计值，无需精确的卫星动力学模型。改变星体转动惯量或设置干扰力矩情况下的数学仿真表明，所设计的自抗扰控制器具有较小的稳态误差、较快的动态响应及对干扰有较强的抑制能力。     

Global value of Hubble constant

Multiaperture photometry in V (5500Å), r (6738Å) and IV (10500Å) of 52 spirals in nearby clusters Virgo, Fornax and Grus and farther clusters Cancer, Zw 74-23 and Peg I in the redshift range up to 6000 Km s⁻¹ was combined with HI width to derive three independant distances for each galaxy in these clusters.The plot between the mean distance of each cluster and its redshift, indicates the Hubble ratios of distant clusters Cancer, Zw 74-23 and Peg I are about 77 Km s⁻¹ Mpc⁻¹. Further, the Hubble ratios of distant clusters vary only from 76.3 to 78.9 Km s⁻¹ Mpc⁻¹ while those of nearby clusters Virgo, Fornax and Grus vary through a large range of 58.5 to 83.5 Km s⁻¹ Mpc⁻¹. We interpret these data by postulating a systematic motion toward Virgo for the Local Group.The best value for the global Hubble constant from farther and nearby clusters is derived as 74.3± 4 Km s⁻¹ Mpc⁻¹ and an average value of 289±60 Km s⁻¹ for the infall velocity of the Local Group toward Virgo is also derived.     

The X-ray evolution of galaxies: implications for future X-ray observatories

The X-ray evolution of the luminosity of normal galaxies is primarily driven by the evolution of their X-ray binary populations. The imprints left by a cosmological evolution of the star formation rate (SFR) will cause the average X-ray luminosity of galaxies to appear higher in the redshift range 1–3. As reported by White and Ghosh [ApJ, 504 (1998) L31] the profile of X-ray luminosity with redshift can both serve as a diagnostic probe of the SFR profile and constrain evolutionary models for X-ray binaries. In order to observe the high redshift (z>3) universe in the X-ray band, it is necessary to avoid confusion from foreground field galaxies. We report on the predictions of these models of the X-ray flux expected from galaxies and the implications for the telescope parameters of future deep universe X-ray observatories.