Future of Space Astronomy: A global Road Map for the next decades

The use of space techniques continues to play a key role in the advance of astrophysics by providing access to the entire electromagnetic spectrum from radio to high energy γ rays. The increasing size, complexity and cost of large space observatories places a growing emphasis on international collaboration. Furthermore, combining existing and future datasets from space and “ground based” observatories is an emerging mode of powerful and relatively inexpensive research to address problems that can only be tackled by the application of large multi-wavelength observations. While the present set of astronomical facilities is impressive and covers the entire electromagnetic spectrum, with complementary space and “ground based” telescopes, the situation in the next 10–20 years is of critical concern. The James Webb Space Telescope (JWST), to be launched not earlier than 2018, is the only approved future major space astronomy mission. Other major highly recommended space astronomy missions, such as the Wide-field Infrared Survey Telescope (WFIRST), the International X-ray Observatory (IXO), Large Interferometer Space Antenna (LISA) and the Space Infrared Telescope for Cosmology and Astrophysics (SPICA), have yet to be approved for development.     

Relativistic electron fluxes and dose rate variations during April–May 2010 geomagnetic disturbances in the R3DR data on ISS

Space radiation has been monitored successfully using the Radiation Risks Radiometer-Dosimeter (R3D) installed at the ESA EXPOSE-R (R3DR) facility outside of the Russian Zvezda module of the International Space Station (ISS) between March 2009 and January 2011. R3DR is a Liulin type spectrometer–dosimeter with a single Si PIN detector 2 cm² of area and 0.3 mm thick. The R3DR instrument accumulated about 2 million measurements of the absorbed dose rate and flux of 10 s resolution. The total external and internal shielding before the detector of R3DR device is 0.41 g cm⁻². The calculated stopping energy of normally incident particles to the detector is 0.78 MeV for electrons and 15.8 MeV for protons. After the Coronal Mass Ejection (CME) at 09:54 UTC on 3 April 2010, a shock was observed at the ACE spacecraft at 0756 UTC on 5 April, which led to a sudden impulse on Earth at 08:26 UTC. Nevertheless, while the magnetic substorms on 5 and 6 of April were moderate; the second largest in history of GOES fluence of electrons with energy >2 MeV was measured. The R3DR data show a relatively small amount of relativistic electrons on 5 April. The maximum dose rate of 2323 μGy day⁻¹ was reached on 7 April; by 9 April, a dose of 6600 μGy was accumulated. By the end of the period on 7 May 2010 a total dose of 11,587 μGy was absorbed. Our data were compared with AE-8 MIN, CRESS and ESA-SEE1 models using SPENVIS and with similar observations on American, Japanese and Russian satellites.     

组合航天器转动惯量在轨两步辨识标定

在轨辨识转动惯量参数是主动航天器与非合作空间目标构成组合体后实现高精度姿态控制的重要前提,文章提出了一种两步在轨辨识组合航天器转动惯量参数的方法。第一步以航天器本体坐标系滚动轴转动惯量为基准将转动惯量矩阵归一化,得到特殊的转动惯量比矩阵,建立与其相关的姿态动力学模型,提出了基于扩展卡尔曼滤波的在轨辨识算法,基于星上陀螺角速率测量信息在100s左右辨识出所有转动惯量比参数,克服了由于模型简单导致转动惯量信息辨识不完整的缺点;第二步基于第一步辨识得到的转动惯量比参数,采用最小二乘算法辨识得到滚动轴转动惯量值,计算量小,消耗能量少。最后给出仿真算例,辨识精度基本在1|之内,验证了方法的有效性。     

月尘环境效应及地面模拟技术

介绍了月球尘的特点及其对探月活动的影响。在分析月球尘环境及其对月面探测器污染、磨损、阻塞、静电效应的基础上,对月球尘环境模拟技术、月球尘扬尘及其运动学和动力学规律、月球尘效应防护及试验评价方法等研究方向和重点提出了一些初步看法。针对研究内容的需求,梳理出一台完整的月球尘地面模拟试验设备应具备真空、温度、太阳风、太阳紫外、月球尘、月面电场、月面磁场等环境因素。在此基础上,设计了一种月球尘地面模拟试验装置方案,并对月球尘环境效应试验方法进行了初步讨论。为月球探测后期任务条件保障建设及相关研究工作提供参考。     

单轴台的大角度姿态快速机动联合控制方法

为验证小卫星大角度姿态快速机动与高精度稳定控制能力,基于单轴气浮台硬件仿真环境,提出了一种利用推力器与飞轮组合的联合控制策略.采用相平面控制技术与有限时间控制理论设计控制器,利用推力器实现无超调的快速机动控制,利用飞轮实现有限时间内的高精度稳定控制,使单轴台在有限时间内快速高精度稳定于目标姿态.物理仿真结果表明:该方法在有限时间内完成单轴台快速稳定控制的同时,可有效避免机动过程中的超调现象,且能有效规避推力器的频繁开关与飞轮的过快饱和等问题.     

直接敏感地平的空天飞行器惯性/天文组合方法

传统的惯性/天文位置组合导航系统中,由于天文定位观测输出耦合了水平观测平台基准误差,往往存在系统噪声与量测噪声不完全独立的问题.针对此问题,分析了利用天文观测量修正惯性系下陀螺漂移的原理,提出了一种直接敏感地平进行天文解析定位及组合滤波的空天飞行器自主导航定位方案,并建立了相应的组合滤波模型.所提出的方法采用星敏感器和陀螺仪构造惯性基准,并在此基础上进行基于红外地平仪的天文定位解算,最后进行惯性/天文组合定位.该方案充分利用了星光敏感器在惯性系下姿态测量精度高的优点,并使惯性/天文组合定位滤波中状态噪声和观测噪声完全独立,仿真结果验证了该定位方法的有效性.     

抗辐射模拟CMOS集成电路研究与设计

为研究宇宙辐射环境中航天器里的模拟互补金属氧化物半导体(Complementary Metal Oxide Semiconductor,CMOS)集成电路性能和各种效应,并在辐射效应所产生机制的基础上,从设计和工艺方面提出了模拟CMOS集成电路主要抗辐射加固设计方法.在宇宙环境中,卫星中的模拟CMOS集成电路存在CMOS半导体元器件阈值电压偏离、线性跨导减小、衬底的漏电流增加和转角1/f噪声幅值增加.所以提出了3种对模拟CMOS集成电路进行抗辐射加固的方法:1)抗辐射模拟CMOS集成电路的设计;2)抗辐射集成电路版图设计;3)单晶半导体硅膜(Silicon on Insulator,SOI)抗辐射工艺与加固设计.根据上面的设计方法研制了抗辐射加固模拟CMOS集成电路,可以取得较好的抗辐射效果.     

绳驱动拟人臂机器人的动力学建模及张力分析

与传统的机械臂相比,绳驱动拟人臂机器人采用串并混联的结构形式,模拟了人手臂肌肉的并联驱动方式,但是,绳索的引入也增加了动力学分析的难度.将绳驱动拟人臂机器人视为基座、大臂、小臂和末端四连杆串联机构,采用迭代牛顿-欧拉法建立动力学方程的递推形式,考虑绳驱动的冗余特性和绳索的单方向受力性,提出基于动态最小预紧力的张力分配算法,求解出各绳索的驱动力.与未进行张力分配的方法及基于静态最小预紧力的方法相比,所提出的算法可使各绳索驱动力根据动态最小预紧力进行实时调节,满足了不同工作条件下机构的刚度要求.     

一种改进的多目标粒子群优化算法

为了增强多目标粒子群优化算法的收敛性与多样性,提出一种改进的多目标粒子群算法.采用Kent映射对种群进行初始化,并将目标空间均匀划分为若干扇形区域;基于一种新的多样性和收敛性判定标准,选取合适的收敛性最优解和多样性最优解,并提出一种改进的粒子群更新公式进行全局搜索;采用聚类算法对外部种群与坐标轴夹角进行分析,维护外部种群.通过标准测试函数的仿真实验,与多目标优化算法基本MOPSO(Multi-objective Particle Swarm Optimization Algorithm)和NSGA-II(Nondominated Sorting Genetic Algorithm II)进行对比,结果表明了该改进算法的有效性.