有限大平板中圆孔的应力集中计算

本文应用广义变分原理,给出了含圆孔的有限大平板应力集中的计算公式。並对矩形板单向均匀拉伸和剪切两种情况进行了数值计算,将计算结果绘成了曲线。     

小卫星动平衡研究--质心不对中对姿态的影响

首先定性分析质心不对中对星体动力学特性的影响，然后由拉格朗日第二类方程导出引力场下星体运动方程的矩阵表达式，最后以50kg级长方体3轴稳定小卫星为例，分析不同初角速度和不同时间历程情况下质心不对中对星体运动姿态的影响，并分析其对星体运动稳定性的影响．本文研究为同类品种小卫星的构型设计、姿态控制系统设计以及制定卫星动平衡精度提供依据。     

基于中值滤波和参考点的风洞压敏涂料试验图像处理技术

提出了一种结合图像中值滤波和试件参考点的风洞压敏涂料（PSP）试验图像数据处理方法。与通常用校准箱获取校准曲线进而得到PSP试验试件表面压力或压力系数（Cp）的方法不同，该方法通过空心中值滤波技术恢复PSP光强比图像中测压孔处的光强比数据，结合若干参考点处常规测压技术实测所得Cp值，获得Cp值和PSP图像光强比数据的关系曲线，进而得到整个试件表面的Cp值数据，该方法获得的数据结合了风洞试验诸多因素对试验结果的影响。利用MATLAB对PSP技术试验图像数据进行了处理，并将PSP方法获得的Cp值与常规测压方法获得的Cp值进行了比较，得到的结果显示，笔者采用的方法获得的Cp值与常规测压方法获得的Cp值吻合较好。该方法为PSP图像数据的处理提供了一种新的方法，具有较大的发展潜力和应用价值。     

Proposal for a United Nations Basic Space Technology Initiative

The United Nations Programme on Space Applications, implemented by the United Nations Office for Outer Space Affairs, promotes the benefits of space-based solutions for sustainable economic and social development. The Programme assists Member States of the United Nations to establish indigenous capacities for the use of space technology and its applications. In the past the Programme has primarily been focusing on the use of space applications and on basic space science activities. However, in recent years there has been a strong interest in a growing number of space-using countries to build space technology capacities, for example, the ability to develop and operate small satellites. In reaction to this development, the United Nations in cooperation with the International Academy of Astronautics has been organizing annual workshops on small satellites in the service of developing countries. Space technology related issues have also been addressed as part of various other activities of the Programme on Space Applications. Building on these experiences, the Office for Outer Space Affairs is now considering the launch of a new initiative, preliminarily titled the United Nations Basic Space Technology Initiative (UNBSTI), to promote basic space technology development. The initiative would be implemented in the framework of the Programme on Space Applications and its aim would be to help building sustainable capacities for basic space technology education and development, thereby advancing the operational use of space technology and its applications.     

Evolution of the temporal and the spectral properties in 2010 and 2011 outbursts of H 1743-322

The Galactic black hole candidate H 1743-322 exhibited two X-ray outbursts in rapid succession: one in August 2010 and the other in April 2011. We analyze archival data of this object from the PCA instrument on board RXTE (2–25 keV energy band) to study the evolution of its temporal and spectral characteristics during both the outbursts, and hence to understand the behavioral change of the accretion flow dynamics associated with the evolution of the various X-ray features. We study the evolution of QPO frequencies during the rising and the declining phases of both the outbursts. We successfully fit the variation of QPO frequency using the Propagating Oscillatory Shock (POS) model in each of the outbursts and obtain the accretion flow parameters such as the instantaneous shock locations, the shock velocity and the shock strength. Based on the degree of importance of the thermal (disk black body) and the non-thermal (power-law) components of the spectral fit and properties of the QPO (if present), the entire profiles of the 2010 and 2011 outbursts are subdivided into four different spectral states: hard, hard-intermediate, soft-intermediate and soft. We attempt to explain the nature of the outburst profile (i.e., hardness-intensity diagram) with two different types of mass accretion flow.     

小卫星动平衡灵敏度分析

基于线性规划灵敏度分析技术和小卫星质心对中计算平台 ,分析质心偏差(Rc)、允许质心偏差 (Rc0 )、单个配重允许值 (wb)、卫星总质量 (Mc)对总配重 (W )的影响。分析表明 ,在允许配重位置确定的情况下 ,Rc0 ∝ 1 /Mc;Rc0 ∝wb;单个配重允许值低时 ,偏心增大显著增加总配重 ;偏心大时 ,放宽单个配重允许值可以有效降低总配重。分析结论同样适用于其他航天器和一般机械产品     

微小卫星姿态控制系统半物理仿真设计及验证

针对利用反作用飞轮作为执行机构的微小卫星姿态控制系统,详细讨论了基于dSPACE实时仿真机、单轴气浮转台、星载计算机及陀螺和反作用飞轮实物的卫星姿态控制系统半物理仿真的方案设计;并利用该系统对仅用反作用飞轮的卫星姿态大角度机动控制模式进行了半物理仿真验证。仿真结果表明根据陀螺和反作用飞轮现有精度,设计的大角度姿态机动控制算法能够满足分系统技术要求,同时验证了半物理仿真系统方案设计合理、可靠。     

小卫星故障诊断与处理技术

介绍一种简单有效的故障诊断及处理技术，它将小卫星的故障分为分系统级，系统级和系统外部级三种，并由星务管理软件处理系统级故障，在每个循环周期都对遥测参数进行采集和监测，故障发生时，根据故障的优先级，选择并恢复具有最高优先级的故障。该技术在某小卫星中应用，能有效满足系统控制周期的限制和系统可靠性要求。     

区域观察小卫星星座重构方法研究

在对地观测任务中，经过优化设计的卫星星座通常具有较强的适应能力。但是，当星座中某颗卫星失效或地面需求发生变化时，就需要进行星座重构，以恢复或增强对部分地区的观察能力。提出了小卫星区域观察组网的方法，重点探讨了在应急情况下区域观察小卫星星座的重构问题，研究了节省能量的卫星轨道机动方法，特别提出了保持轨道属性和星座基本构形的预置量机动方法，分析了应急机动星座重构的几种情况，给出了每种情况的星座重构策略。     

Dark energy,co-evolution of massive black holes with galaxies,and ASTROD-GW

The detection of low frequency band (100 nHz–100 mHz) and very low frequency band (300 pHz–100 nHz) gravitational waves (GWs) is important for exploration of the equation of state of dark energy and the co-evolution of massive black holes (MBHs) with galaxies. Most galaxies are believed to have a massive black hole in the galactic core. In the formation of these black holes, merging and accretion are the two main processes. Merging of massive black holes generate GWs which could be detected by space GW detectors and Pulsar Timing Arrays (PTAs) to cosmological distances. LISA (Laser-Interferometric Space Antenna) is most sensitive to the frequency band 1 mHz–100 mHz, ASTROD-GW (ASTROD [Astrodynamical Space Test of Relativity using Optical Devices] optimized for Gravitational Wave detection) is most sensitive to the frequency band 100 nHz–1 mHz and PTAs are most sensitive to the frequency band 300 pHz–100 nHz. In this paper, we discuss the sensitivities and outlooks of detection of GWs from binary massive black holes in these frequency bands with an emphasis on ASTROD-GW. The GWs generated by the inspirals, merging and subsequent ringdowns of binary black holes are standard sirens to the cosmological distance. Using GW observations, we discuss the methods for determining the equation of state of dark energy and for testing the co-evolution models of massive black holes. ASTROD-GW is an optimization of ASTROD to focus on the goal of detection of GWs. The mission orbits of the 3 spacecraft forming a nearly equilateral triangular array are chosen to be near the Sun-Earth Lagrange points L3, L4 and L5. The 3 spacecraft range interferometrically with one another with arm length about 260 million kilometers. With 52 times longer in arm length compared to that of LISA, the strain detection sensitivity is 52 times better toward larger wavelength. The scientific aim is focused for gravitational wave detection at low frequency. The science goals include detection of GWs from MBHs, and Extreme-Mass-Ratio Black Hole Inspirals (EMRI), and using these observations to find the evolution of the equation of state of dark energy and to explore the co-evolution of massive black holes with galaxies.