基于DSPN的航天测控系统任务可靠性仿真建模

提出了基于确定与随机Petri网（deterministic and stochastic Petri nets,DSPN）的航天测控系统（tracking,telemetry and command,TT&C）任务可靠性定量分析方法,旨在对相关航天测控方案进行可靠性预计.通过对TT&C系统任务剖面进行时序弧段划分,考虑实际系统中测控单元阶段依赖、单元故障可修以及各单元参与任务起止时间不同等其他建模方法难以处理的复杂因素,建立了“单元层-系统逻辑层-阶段层”3层相互关联的TT&C系统任务可靠性DSPN模型.通过对模型仿真运行,实现了对给定测控方案下TT&C系统任务可靠性定量化评估.分析表明:仿真结果随着仿真次数增加逐渐收敛,与Markov解析方法求得的精确值对比误差控制在1%以内.      

临近空间螺旋桨低雷诺数高效翼型数值分析

针对临近空间翼型边界层变厚更容易发生分离的特点,在修正了湍流模型后,通过分析比较13种低雷诺数翼型的升阻系数得到了比较适合用于临近空间螺旋桨叶素的高效翼型。结果显示,攻角在-6°～8°、8°～14°、14°～22°三种工况下,分别采用SST k-ω、RNG k-ε、Realizable k-ε湍流模型,可以得到与国外实验比较接近的合理结果;工况条件对翼型气动性能好坏的影响很大,翼型S-1223和FX63-137在所研究的工况内都具有较好的气动性能;因此可以选择这两种翼型作为临近空间螺旋桨用高效翼型。     

空间绳系机器人逼近目标协调控制方法

 为了节省空间绳系机器人的末端执行装置在逼近目标卫星过程中推力器所使用的燃料,本文提出一种利用推力器、反作用轮及空间系绳的协调控制方法。首先利用二次型最优控制器(LQR)算法计算出末端执行装置逼近目标所需的理想轨道控制力,然后利用模拟退火算法将所需轨道控制力优化分配到推力器及空间系绳,同时利用时间延迟算法通过反作用轮补偿空间系绳产生的姿态干扰力矩。仿真结果表明,利用该协调控制方法能显著节省末端执行装置上推力器的燃料消耗,有效抑制空间系绳协调控制力产生的姿态干扰,使末端执行装置保持相对稳定的姿态。     

几何非线性机翼本征梁元素模型的高效化改进

 采用Hodges等提出的时间-空间离散化的几何精确非线性本征梁通用模型处理柔性机翼结构动力学问题时,当离散化的节点数增大时,该方法的未知数数量成倍地增长,而且方程组是严重病态的,因此数值模拟计算的速度非常缓慢。针对机翼中最常见的悬臂梁结构,根据空间离散化的边界条件,提出了空间缩聚法把空间离散差分方程缩聚为常系数矩阵格式,得到了只与时间相关的微分方程组,进一步推导得到了该方程组的雅可比矩阵,因而大大减少了方程组的数量以及求解过程的循环和迭代步数。采用Gear方法分别求解了原始的本征梁元素模型和本文提出的缩聚模型,结果表明空间缩聚模型在相同条件下可提高运算速度约5.1倍,而且对不同类型的外载荷都具有较好的通用性、稳定性和高效性。     

空间绳系机器人抓捕后复合体姿态协调控制

针对空间绳系机器人对目标抓捕后的复合体姿态稳定控制问题进行了研究.首先,对复合体进行动力学建模,并对其动力学特性进行了分析;然后,考虑复合体的特点、空间绳系机器人燃料有限以及自身姿态控制力的限制,分别设计了系绳主动拉力与推力器推力协调控制器和基于滑模变结构的全推力控制器,并设计了其切换条件,利用两种控制器切换对姿态进行稳定控制;最后,利用仿真实验验证了所提方法的正确性.仿真结果表明,系绳拉力和推力器协调控制方法能够实现对姿态的稳定控制,并且有效地节省姿态控制过程中的燃料消耗.     

临近空间高超声速目标滑跃式轨迹Sine-AIMM跟踪算法

针对单一的Sine模型算法无法与临近空间高超声速目标滑跃式轨迹准确匹配,现有的交互多模型(IMM)算法跟踪效果也不够理想的问题,提出一种基于多重贝叶斯准则的自适应交互式多Sine模型(Sine-AIMM)临近空间高超声速滑跃式目标跟踪算法.算法采用多个Sine模型对滑跃式轨迹进行匹配,并利用多重贝叶斯准则在线调整各模型...     

Space weather: its effects and predictability

Terrestrial technology is now, and increasingly, sensitive to space weather. Most space weather is caused by solar storms and the resulting changes to the Earth's radiation environment and the magnetosphere. The Sun as the driver of space weather is under intense observation but remains to be adequately modelled. Recent spacecraft measurements are greatly improving models of solar activity, the interaction of the solar wind with the magnetosphere, and models of the radiation belts. In-situ data updates the basic magnetospheric model to provide specific details of high-energy electron flux at satellite orbits. Shock wave effects at the magnetopause can also be coarsely predicted. However, the specific geomagnetic effects at ground level depend on the calculation of magnetic and electric fields and further improvements are needed. New work on physical models is showing promise of raising geomagnetic and ionospheric predictability above the synoptic climatological level. This revised version was published online in August 2006 with corrections to the Cover Date.     

Type II Solar Radio Bursts: Theory and Space Weather Implications

Recent data and theory for type II solar radio bursts are reviewed, focusing on a recent analytic quantitative theory for interplanetary type II bursts. The theory addresses electron reflection and acceleration at the type II shock, formation of electron beams in the foreshock, and generation of Langmuir waves and the type II radiation there. The theory's predictions as functions of the shock and plasma parameters are summarized and discussed in terms of space weather events. The theory is consistent with available data, has explanations for radio-loud/quiet coronal mass ejections (CMEs) and why type IIs are bursty, and can account for empirical correlations between type IIs, CMEs, and interplanetary disturbances. This revised version was published online in August 2006 with corrections to the Cover Date.     

Real-Time Specifications of the Geospace Environment

We report the recent progress in our joint program of real-time mapping of ionospheric electric fields and currents and field-aligned currents through the Geospace Environment Data Analysis System (GEDAS) at the Solar-Terrestrial Environment Laboratory and similar computer systems in the world. Data from individual ground magnetometers as well as from the solar wind are collected by these systems and are used as input for the KRM and AMIE magnetogram-inversion algorithms, which calculate the two-dimensional distribution of the ionospheric parameters. One of the goals of this program is to specify the solar-terrestrial environment in terms of ionospheric processes, providing the scientific community with more than what geomagnetic activity indices and statistical models provide. This revised version was published online in August 2006 with corrections to the Cover Date.     

Modelling of the electromagnetic field in the interplanetary space and in the Earth's magnetosphere

A magnetohydrodynamic model of the solar wind flow is constructed using a kinematic approach. It is shown that a phenomenological conductivity of the solar wind plasma plays a key role in the forming of the interplanetary magnetic field (IMF) component normal to the ecliptic plane. This component is mostly important for the magnetospheric dynamics which is controlled by the solar wind electric field. A simple analytical solution for the problem of the solar wind flow past the magnetosphere is presented. In this approach the magnetopause and the Earth's bow shock are approximated by the paraboloids of revolution. Superposition of the effects of the bulk solar wind plasma motion and the magnetic field diffusion results in an incomplete screening of the IMF by the magnetopause. It is shown that the normal to the magnetopause component of the solar wind magnetic field and the tangential component of the electric field penetrated into the magnetosphere are determined by the quarter square of the magnetic Reynolds number. In final, a dynamic model of the magnetospheric magnetic field is constructed. This model can describe the magnetosphere in the course of the severe magnetic storm. The conditions under which the magnetospheric magnetic flux structure is unstable and can drive the magnetospheric substorm are discussed. The model calculations are compared with the observational data for September 24–26, 1998 magnetic storm (Dst _min=−205 nT) and substorm occurred at 02:30 UT on January 10, 1997. This revised version was published online in August 2006 with corrections to the Cover Date.