卫星动不平衡方法研究

文章结合在工程中遇到的动不平衡实际问题,根据平衡机的基本工作原理,提出了双平面分别配重、合成计算的解决思路,并在理论上对自旋稳定卫星的双平面配重的动不平衡配重的计算方法进行了分析和研究,验证了配平计算方法的正确性和可行性。最后,根据配重计算方法提出了配重调整的工艺步骤。     

生物皮肤传质的研究

针对皮肤各层结构主要由细胞和细胞间液构成的特点提出了可行的3层多孔介质物理模型,根据不同层的具体特点建立了相应的浓度和能量数学方程.利用浓度方程对模型进行了浓度分析求解,和编程计算了在不同灌流率、传质系数和各层厚度下对浓度的影响.与传质系数实验所得结果相比较,结果一致.      

激光光散射法测定BAG分子量及其分子量分布

介绍了一种用于高能推进剂新型键合剂BAG分子量和分子量分布测定的激光光散射法。给出了该方法的实验原理、实验步骤。该法以合镍化钾的二甲基酰胺溶液溶剂和流动相，凝胶渗透色谱柱为分离体系，实验结果表明：准确度和精密度较好，可作为常规测定BAG分子量及其分布的方法。     

导弹质量矩控制技术发展综述

质量矩技术是近年来导弹控制领域研究的热点问题之一。它是通过调整弹体内部活动质 量块的状态来实现导弹机动飞行的。与传统的气动舵控制方式相比,它具有响应快、气动外 形简单、无舵面烧蚀问题等优点,在大气层内高超声速飞行控制领域具有广阔的应用前景。 简述了质量矩技术的原理及应用领域,回顾了导弹质量矩控制技术的发展历程;从总体 布局、动力学建模、控制系统设计等方面综合分析了质量矩技术的研究现状;提出了一些当 前需要解决的难点问题,供相关人员参考。
     

无阻力卫星发展现状

以无阻力卫星的发展和相关技术为综述对象,首先介绍了无阻力卫星的概念,并比较无阻力卫星中位移模式和加速度计模式的区别和优缺点;其次分析了无阻力卫星的体系结构,将无阻力卫星控制系统分为无阻力控制回路、悬浮控制回路和卫星本体控制回路;然后描述了无阻力卫星中的检测质量、主要硬件的功能与特性,最后列出了无阻力卫星中主要的关键技术。     

一种海洋测高卫星质心在轨估计算法

为了满足海洋测高卫星在轨质心位置精度的要求,提出了一种使用陀螺仪测量数据在轨估算卫星质心位置的算法。该算法利用推力器工作产生外力矩,采用总体最小二乘法,综合考虑了实际推力器推力的误差及陀螺仪的测量误差,由卫星的姿态动力学方程估算得到卫星质心位置。数值仿真证明了该算法的有效性,结果表明质心位置的估计精度在毫米量级,可以满足海洋测高卫星对质心位置精度的需求。     

空间目标轨道信息软件平台的建设

空间目标轨道信息是空间态势感知的重要要素,是空间碰撞预警、空间碎片环境模型和许多空间应用的基础。因而,空间目标轨道确定成为空间态势感知的主要任务之一。文章介绍武汉大学测绘学院正在开发建设的空间目标轨道信息服务软件平台,该平台拥有的主要功能有:利用多源数据的卫星/空间碎片轨道确定(包括初轨确定)与预报、大气质量密度模型精化、空间碰撞预警和半解析法快速精密轨道传播等。文章还针对软件平台功能的研究进展进行了综述,介绍了软件平台发展规划。     

SMESE (SMall Explorer for Solar Eruptions): A microsatellite mission with combined solar payload

The SMESE (SMall Explorer for Solar Eruptions) mission is a microsatellite proposed by France and China. The payload of SMESE consists of three packages: LYOT (a Lyman α imager and a Lyman α coronagraph), DESIR (an Infra-red Telescope working at 35–80 and 100–250 μm), and HEBS (a High Energy Burst Spectrometer working in X- and gamma-rays).     

Evolution of solar wind structures from 0.72 to 1 AU

Understanding the evolution of solar wind structures in the inner heliosphere as they approach the Earth is important to space weather prediction. From the in situ solar wind plasma and magnetic field measurements of Pioneer Venus Orbiter (PVO) at 0.72 AU (1979–1988), and of Wind/Advanced Composition Explorer (ACE) missions at 1 AU (1995–2004), we identify and characterize two major solar wind structures, stream interaction regions (SIRs) and interplanetary coronal mass ejections (ICMEs). The average percentage of SIRs occurring with shocks increases significantly from 3% to 24% as they evolve from 0.72 to 1 AU. The average occurrence rate, radial extent, and bulk velocity variation of SIRs do not change from 0.72 to 1 AU, while peak pressure and magnetic field strength both decrease with the radial evolution of SIRs. Within the 0.28 AU distance from the orbit of Venus to that of Earth, the average fraction of ICMEs with shocks increases from 49% to 66%, and the typical radial extent of ICMEs expands by about a fraction of 1.4, with peak pressure and magnetic field strength decreasing significantly. The mean occurrence rate and expansion velocity of ICMEs do not change from 0.72 to 1 AU.     

Hydrodynamic atmosphere models for hot luminous stars II. Method and improvements over unified models

In a paper submitted to A&A we present the first line blanketed hydrodynamic models of spherically expanding atmospheres of hot stars. This paper is complementary to the submitted paper. Here, we emphasize the advantages and the weak points of our approach and we present additional technical aspects.The models are characterised by a simultaneous solution of the equation of motion, the non-LTE populations of H and He, and radiation transfer in a line blanketed atmosphere. The entire domain from the optically thick photosphere out to the terminal velocity of the wind is treated. The radiative forces are evaluated consistently with the depth-dependent radiation field, taking into account multiple scattering by metal lines and line overlap.