On the station keeping of a solar sail in the elliptic Sun–Earth system

In this work we focus on the dynamics of a solar sail in the Sun–Earth Elliptic Restricted Three-Body Problem with solar radiation pressure. The considered situation is the motion of a sail close to the L₁ point, but displacing the equilibrium point with the sail so that it is possible to have continuous communication with the Earth. In previous works we derived a station keeping strategy for this situation but using the Circular RTBP as a model.     

Results of solar observations by the CORONAS-F payload

The CORONAS-F mission experiments and results have been reviewed. The observations with the DIFOS multi-channel photometer in a broad spectral range from 350 to 1500 nm have revealed the dependence of the relative amplitudes of p-modes of the global solar oscillations on the wavelength that agrees perfectly well with the earlier data obtained in a narrower spectral ranges. The SPIRIT EUV observations have enabled the study of various manifestations of solar activity and high-temperature events on the Sun. The data from the X-ray spectrometer RESIK, gamma spectrometer HELICON, flare spectrometer IRIS, amplitude–temporal spectrometer AVS-F, and X-ray spectrometer RPS-1 have been used to analyze the X- and gamma-ray emission from solar flares and for diagnostics of the flaring plasma. The absolute and relative content of various elements (such as potassium, argon, and sulfur) of solar plasma in flares has been determined for the first time with the X-ray spectrometer RESIK. The Solar Cosmic Ray Complex monitored the solar flare effects in the Earth’s environment. The UV emission variations recorded during solar flares in the vicinity of the 120-nm wavelength have been analyzed and the amplitude of relative variations has been determined.     

Effects on winter circulation of short and long term solar wind changes

Indices of the North Atlantic Oscillation and the Arctic Oscillation show correlations on the day-to-day timescale with the solar wind speed (SWS). Minima in the indices were found on days of SWS minima during years of high stratospheric aerosol loading. The spatial distribution of surface pressure changes during 1963–2011 with day-to-day changes in SWS shows a pattern resembling the NAO. Such a pattern was noted for year-to-year variations by Boberg and Lundstedt (2002), who compared NAO variations with the geo-effective solar wind electric field (the monthly average SWS multiplied by the average southward component, i.e., negative Bz component, of the interplanetary magnetic field). The spatial distribution of the correlations of geopotential height changes in the troposphere and stratosphere with the SWS; the geo-effective electric field (SWS∗Bz); and the solar 10.7 cm flux suggests that solar wind inputs connected to the troposphere via the global electric circuit, together with solar ultraviolet irradiance acting on the stratosphere, affect regional atmospheric dynamics.     

Sunspot cycle 23 descent to an unusual minimum and forecasts for cycle 24 activity

The decay phase of the sunspot cycle 23 exhibited two unusual features. First, it lasted too long. Second, the interplanetary magnetic field intensity at earth orbit reached the lowest value since in situ measurements in space began in October 1963. These physical anomalies significantly altered the early forecasts for the sunspot activity parameters for cycle 24, made by several colleagues. We note that there was a significant change in the solar behavior during cycle 22. We discuss the observed trends and their effect on our empirical solar activity forecast technique, leading to our prediction for cycle 24 parameters; cycle 24 will be only half as active as cycle 23, reaching its peak in May 2013. We speculate on the possible implications of this outcome on future earth climate change and the ensuing socio-economic consequences.     

陆基无线电授时系统信号分析与解算

时间应用的广泛性以及授时战的提出,使国家更加重视授时服务体系的完备性以及灵活性。为顺应授时战要求,从我国整体授时体系出发,简单介绍授时系统的工作原理,从多方面对比各类授时系统;主要分析了我国陆基无线电授时系统的发播程序以及信号格式等,对BPM短波呼号以及时码结构进行补充与修正,并讲解对陆基无线电授时信号的解算过程,利用实际试验验证解算方法的可行性;最后根据我国目前授时体系的现状以及授时战的要求,给出应对授时战的技术路线,对未来我国授时体系发展方向提出建议。     

永磁同步电机驱动太阳翼扰动力矩建模与仿真

建立太阳翼驱动机构(SADA)永磁同步电机的电磁方程,并利用固定界面模态综合法建立SADA驱动太阳翼耦合系统的振动方程;设计模拟柔性负载,对SADA驱动该柔性负载的扰振力矩进行仿真分析。结果表明,SADA驱动柔性负载运行过程中所产生扰振力矩主要由两个原因引起：1)电流噪声引起的力矩波动;2)控制参数选取不当引起的转角波动。     

软件无线电的可重构流处理器体系结构

 针对软件无线电中存在通用数字信号处理器（DSP）计算能力不足以及专用基带处理器缺乏扩展性的问题,提出了一种新的处理器：面向软件无线电的可重构流处理器及相应的专用指令集。仿真证明,该处理器的可重构设计具备指令集扩展能力,可以对多种无线通信标准甚至是新的通信标准提供支持;面向软件无线电的流体系结构和专用指令集保证了对多种高速无线基带信号的实时处理,运算能力是通用DSP的5~13倍。该处理器为软件无线电中的硬件设计难题提供了一种新的解决途径。     

APU 转子爆破对防火墙影响的研究

APU是安装在民用飞机上的辅助动力装置,是飞机上重要的部件,因此必须考虑APU 转子爆破时小碎片对飞机安全的影响。通过有限元软件LS-DYNA,分别模拟了APU 转子爆破时小碎片对APU 防火墙以及3种不同厚度加强板的冲击计算。根据数值计算结果,选择合适的加强板方案,既能防止防火墙碰撞区被小碎片击穿,同时付出的重量代价又较小。通过对APU 防火墙增加加强板,确保APU 转子爆破时飞机的安全 性,满足AC20-128A 的设计要求。     

深空探测器无线电干涉测量开源数据处理系统构建及试验

为更好地开展深空无线电干涉测量试验,基于DiFX(Distributed FX,分布式FX型相关处理)、SPICE(Spacecraft Planet Instrument Camera-matrix Events,航天器行星仪器照相机矩阵事件)、HOPS(Haystack Observatory Postprocessing System,Haystack克天文台后处理系统)及AIPS(Astronomical Image Processing System,天文图像处理系统)等开源软件,搭建了一套可用于深空探测器信号相关处理的无线电干涉测量数据处理系统。首先介绍了该系统的整体架构及组成,然后介绍了系统各组成模块的功能及工作原理,最后利用该系统对嫦娥三号着陆器开展了观测试验,并对观测数据进行了处理。试验结果表明,该系统能成功实现深空航天器信号的相关处理、条纹拟合,以及时延解算等功能,有望为我国嫦娥五号任务及火星探测任务数据处理提供支持。     

Modelling of galactic Carbon in an asymmetrical heliosphere: Effects of asymmetrical modulation conditions

Observations of galactic cosmic rays (GCRs) from the two Voyager spacecraft inside the heliosheath indicate significant differences between them, suggesting that in addition to a possible global asymmetry in the north–south dimensions (meridional plane) of the heliosphere, it is also possible that different modulation (turbulence) conditions could exist between the two hemispheres of the heliosphere. We focus on illustrating the effects on GCR Carbon of asymmetrical modulation conditions combined with a heliosheath thickness that has a significant dependence on heliolatitude. To reflect different modulation conditions between the two heliospheric hemispheres in our numerical model, the enhancement of both polar and radial perpendicular diffusion off the ecliptic plane is assumed to differ from heliographic pole to pole. The computed radial GCR intensities at polar angles of 55° (approximating the Voyager 1 direction) and 125° (approximating the Voyager 2 direction) are compared at different energies and for both particle drift cycles. This is done in the context of illustrating how different values of the enhancement of both polar and radial perpendicular diffusion between the two hemispheres contribute to causing differences in radial intensities during solar minimum and moderate maximum conditions. We find that in the A > 0 cycle these differences between 55° and 125° change both quantitatively and qualitatively for the assumed asymmetrical modulation condition as reflected by polar diffusion, while in the A < 0 cycle, minute quantitative differences are obtained. However, when both polar and radial perpendicular diffusion have significant latitude dependences, major differences in radial intensities between the two polar angles are obtained in both polarity cycles. Furthermore, significant differences in radial intensity gradients obtained in the heliosheath at lower energies may suggest that the solar wind turbulence at and beyond the solar wind termination shock must have a larger latitudinal dependence.