基于摄影测量技术的航天发动机装配过程几何参数测量方法研究

当前我国航天发动机装配过程几何参数的测量方法为专业人员操作激光跟踪仪或全站仪逐点位进行测量,此类方法存在测量效率低的缺点。针对此问题,提出了一种高效的基于摄影测量技术的航天发动机装配过程几何参数测量方法,对该测量方法的测量原理进行了介绍,详细说明了这一方法各测量环节实现的测量目的,最后通过实测数据计算工业数字摄影测量技术在此类应用中的系统准确度,证明了该测量方法的可行性。     

参数不确定空间机械臂关节轨迹跟踪的增广自适应控制方案

讨论了载体位置与姿态均不受控制的漂浮基两杆空间机械臂系统的控制问题.系统动力学分析的结果表明,结合系统动量及动量矩守恒关系得到的系统动力学方程将为系统惯性参数的非线性函数.证明了借助于增广变量法,即通过适当扩展系统的控制输入与输出可以得到一组控制方程,它们可以表示为一组适当选择的惯性参数的线性函数.以此为基础,针对机械臂末端载荷参数未知的情况,设计了关节空间轨迹跟踪的增广自适应控制方案.此控制方案的显著优点在于不需要测量漂浮基的位置及移动的速度、加速度.仿真运算证实了方法的有效性.     

两类空间目标的非参数姿态判别方法

在详细分析空间轨道目标窄带雷达特性的基础上,利用非参数统计学的随机游程检验理论对空间目标的稳定方式进行判别,从而实现对绕质心旋转和非旋转这两类目标的分类识别。     

空间机器人的目标捕获自适应控制

首先推导了基座姿态受控空间机器人系统运动学关系,得到了广义雅可比矩阵。根据目标的运动来规划机械臂末端在惯性空间的期望轨迹。对机器人动力学和运动学关系式进行线性参数比,分别对动力学待估参数和运动学待估参数设计在线修正律,在关节空间采用自适应控制。对于存在动力学参数不确知的机器人系统,算法保证了系统的渐近稳定,在成目标捕获任务的同时,控制基座姿态保持在期望范围之内。以平面两关节空间机器人系统为对象进行了仿真,结果表明了算法的可行性和有效性。     

Mars Phobos and Deimos Survey (M-PADS) – A martian Moons orbiter and Phobos lander

We describe a Mars ‘Micro Mission’ for detailed study of the martian satellites Phobos and Deimos. The mission involves two ∼330 kg spacecraft equipped with solar electric propulsion to reach Mars orbit. The two spacecraft are stacked for launch: an orbiter for remote investigation of the moons and in situ studies of their environment in Mars orbit, and another carrying a lander for in situ measurements on the surface of Phobos (or alternatively Deimos). Phobos and Deimos remain only partially studied, and Deimos less well than Phobos. Mars has almost always been the primary mission objective, while the more dedicated Phobos project (1988–89) failed to realise its full potential. Many questions remain concerning the moons’ origins, evolution, physical nature and composition. Current missions, such as Mars Express, are extending our knowledge of Phobos in some areas but largely neglect Deimos. The objectives of M-PADS focus on: origins and evolution, interactions with Mars, volatiles and interiors, surface features, and differences. The consequent measurement requirements imply both landed and remote sensing payloads. M-PADS is expected to accommodate a 60 kg orbital payload and a 16 kg lander payload. M-PADS resulted from a BNSC-funded study carried out in 2003 to define candidate Mars Micro Mission concepts for ESA’s Aurora programme.     

Lower ionosphere response to external forcing: A brief review

There are two ways of external forcing of the lower ionosphere, the region below an altitude of about 100 km: (1) From above, which is directly or indirectly of solar origin. (2) From below, which is directly or indirectly of atmospheric origin. The external forcing of solar origin consists of two general factors – solar ionizing radiation variability and space weather. The solar ionization variability consist mainly from the 11-year solar cycle, the 27-day solar rotation and solar flares, strong flares being very important phenomenon in the daytime lower ionosphere due to the enormous increase of the solar X-ray flux resulting in temporal terminating of MF and partly LF and HF radio wave propagation due to heavy absorption of radio waves. Monitoring of the sudden ionospheric disturbances (SIDs – effects of solar flares in the lower ionosphere) served in the past as an important tool of monitoring the solar activity and its impacts on the ionosphere. Space weather effects on the lower ionosphere consist of many different but often inter-related phenomena, which govern the lower ionosphere variability at high latitudes, particularly at night. The most important space weather phenomenon for the lower ionosphere is strong geomagnetic storms, which affect substantially both the high- and mid-latitude lower ionosphere. As for forcing from below, it is caused mainly by waves in the neutral atmosphere, i.e. planetary, tidal, gravity and infrasonic waves. The most important and most studied waves are planetary and gravity waves. Another channel of the troposphere coupling to the lower ionosphere is through lightning-related processes leading to sprites, blue jets etc. and their ionospheric counterparts. These phenomena occur on very short time scales. The external forcing of the lower ionosphere has observationally been studied using predominantly ground-based methods exploiting in various ways the radio wave propagation, and by sporadic rocket soundings. All the above phenomena are briefly mentioned and some of them are treated in more detail.     

Induction of genomic instability after an acute whole-body exposure of mice to Fe ions

The purpose of this study was to evaluate dose–response relationships for the in vivo induction of micronuclei (MN) as a measure of both initial radiation damage and the induction of genomic instability. These measurements were made in mouse blood erythrocytes as a function of radiation dose, radiation quality, time after irradiation, and the genetic background of exposed individuals. Blood samples were collected from two strains of mouse (CBA/CaJ and C57BL/6J) at different times up to 3 months following a whole-body exposure to various doses of 1 GeV/amu ⁵⁶Fe ions (0, 0.1, 0.5 and 1.0 Gy, at the dose rate of a 1 Gy/min) or ¹³⁷Cs gamma rays (0, 0.5, 1.0 and 3.0 Gy, at the dose rate of 0.72 Gy/min). Blood-smear slides were stained with acridine orange (AO). The frequencies of MN were measured in mature normochromatic-erythrocytes (MN-NCEs) and in immature polychromatic-erythrocytes (MN-PCEs). Effects of both types of radiation on erythropoiesis were also evaluated. As a measure of cell progression delay, a dose-dependent decrease in numbers of PCEs was observed at day 2 post-exposure in both strains, regardless of radiation quality. Subsequently, the levels of PCEs increased in all exposed mice, reaching control levels (or higher) by day 7 post-exposure. Further, at day 2 after the exposure, there was no increase in the frequency of MN-PCEs in CBA/CaJ mice exposed to ⁵⁶Fe ions while the frequency of MN-PCEs elevated as a function of dose in the C57BL/6J mice. At day 4, there was no dose related increase in MN-NCEs in either strain of mouse exposed to ¹³⁷Cs gamma rays. Additionally, at the early sacrifice times (days 2 and 4), ⁵⁶Fe ions were slightly more effective (per unit dose) in inducing MN-NCEs than ¹³⁷Cs gamma rays in CBA/CaJ mice. However, there was no increase in the frequency of MN-NCEs at late times after an acute exposure to either type of radiation. In contrast, both types of radiation induced increased MN-PCEs frequencies in irradiated CBA/CaJ mice, but not C57BL/6J mice, at late times post-exposure. This finding indicates the potential induction of genomic instability in hematopoietic cells of CBA/CaJ mice by both types of radiation. The finding also demonstrates the influence of genetic background on radiation-induced genomic instability in vivo.     

Using high-energy proton fluence to improve risk prediction for consequences of solar particle events

The potential for exposure to large solar particle events (SPEs) with high energy levels is a major concern during interplanetary transfer and extra-vehicular activities (EVAs) on the lunar and Mars surface. Previously, we have used data from the last 5 solar cycles to estimate percentiles of dose to a typical blood-forming organ (BFO) for a hypothetical astronaut in a nominally shielded spacecraft during a 120-d lunar mission. As part of this process, we made use of complete energy spectra for 34 large historical SPEs to calculate what the BFO mGy-Eq dose would have been in the above lunar scenario for each SPE. From these calculated doses, we then developed a prediction model for BFO dose based solely on an assumed value of integrated fluence above 30 MeV (Φ₃₀) for an otherwise unspecified future SPE. In this study, we reasoned that since BFO dose is determined more by protons with higher energies than by those with lower energies, more accurate BFO dose prediction models could be developed using integrated fluence above 60 (Φ₆₀) and above 100 MeV (Φ₁₀₀) as predictors instead of Φ₃₀. However to calculate the unconditional probability of a BFO dose exceeding a pre-specified limit (“BFO dose risk”), one must also take into account the distribution of the predictor (Φ_30,Φ₆₀, or Φ₁₀₀), as estimated from historical SPEs. But Φ₆₀ and Φ₁₀₀ have more variability, and less available historical information on which to estimate their distributions over many SPE occurrences, than does Φ₃₀. Therefore, when estimating BFO dose risk there is a tradeoff between increased BFO dose prediction at a given energy threshold and decreased accuracy of models for describing the distribution of that threshold over future SPEs as the threshold increases. Even when taking the second of these two factors into account, we still arrived at the conclusion that overall prediction improves as the energy level threshold increases from 30 to 60 to 100 MeV. These results can be applied to the development of approaches to improve radiation protection of astronauts and the optimization of mission planning for future space missions.     

利用栅网控制空间等离子体环境效应模拟中的等离子体参数

通常采用ECR等离子体源产生的等离子体的温度和密度都比较大,通过附加适当目数的栅网,并在栅网上加一定的偏置电位来对等离子体参数,尤其是温度、密度进行调整,满足空间等离子体环境模拟要求.本文利用14目、25目的栅网,对己有的地面实验室空间等离子体环境进行了改进,得到了更加接近空间等离子体参数的一个地面模拟环境.     

空间站废水的处理及管理

长期载人飞行的空间站需要大量的用水,为解决由此引起的巨大的维持飞行的运行费用,需要实现水的再生与闭路循环.如何针对空间站废水的特征,解决废水的处理与利用问题,并建立合理的水循环体系是这一工作的关键.文中分析、比较了空间站废水的处理方法,设计了空间站水管理整合方案,并多方面探讨和验证这一方案的合理性和可行性.