一种高稳定度帆板驱动系统的T-S模糊复合控制器

为减少帆板驱动机构（SADA）对太阳帆板挠性模态的激励作用,以扰动力矩较小的永磁同步电机(PMSM)作为驱动源,提出一种T-S模糊控制与校正网络相结合的控制方法。利用校正网络增加系统的相位裕度和增益,并通过T-S模糊控制器降低系统的超调和非线性摩擦的影响,从而有效抑制太阳帆板的振动。通过圆判据对带有此控制器的驱动系统进行了稳定性证明,很好地解决了模糊控制系统在摩擦扰动下难以进行频域理论分析的缺陷。仿真结果表明,在非线性摩擦等扰动的影响下,该控制方法能够很好地抑制太阳帆板引起的挠性振动,提高系统的速度精度和稳定度,具有较好的动态性能。     

三轴磁强计与太阳电池阵组合的皮卫星姿态确定方法

提出一种组合应用三轴磁强计信号与太阳电池阵列信号,在双矢量定姿的基础上,结合样点卡尔曼滤波(UKF)估计算法,连续输出六维姿态信息的姿态估计方法。数值仿真结果表明:两种测量信息有效组合时,精度水平可以满足皮卫星任务要求。     

平流层飞艇的能源技术和平衡分析

平流层飞艇作为近空间对地观测平台的一种实现方案,主要依靠自身庞大体积产生的静浮力而不像其它飞行器依靠相对空气运动产生升力,所以飞艇能够以较慢的速度飞行甚至能够在空中长期保持定点悬停即相对地面静止。具有长时间在平流层自主飞行的能力,是平流层飞艇设计的一个重要目标。文章对平流层飞艇能源系统的构成、部件及能源平衡分析方法作了介绍。     

太阳帆结构分析

太阳帆是人类向太空发射的一种宇宙探测器。本文推导建立了太阳帆结构分析的理论方程组；利用数值计算方法进行了全结构分析；采用罚函数法，确定了满足各种技术条件下的转速及辐条长度之间的可用范围；同时，在引入某些假设的前提下，得出了方程组的近似理论解。它们为太阳帆强度分析、结构形状保持能力提供了论理基础，也为太阳帆的设计提供了依据。本文最后提供了某实际发射的太阳帆结构的分析结果。本文的分析手段可作为大型柔性结构分析的参考     

行星际扰动与不同级别磁暴强度关系的研究

利用1997-2004年间ACE卫星太阳风观测的时均值数据和相应的Dst指数,针对Dstmin≤-50 nT的磁暴,分析了行星际参数(Bz,Ey,v,Pk,|B|,ε'=vxB2zsin4(θ/2))与Dst指数的相关关系.验证了Ey,Bz与Dst指数的良好相关性;按磁暴强度的不同,发现磁暴强度越大,行星际参数与磁暴强度(Dstmin)的相关性就越好.对于中等磁暴(-100 nT＜Dstmin≤-50 nT),行星际参数与磁暴强度的相关系数不高.如果把磁暴分为两个档次,即-150 nT＜Dstmin≤-50 nT的磁暴和Dstmin≤-150 nT的磁暴,计算结果表明,ε'与Dst指数的相关性是最好的.在诸多行星际参数中,就单一因素来说,Ey对磁暴强度影响最大,Bz对磁暴强度影响次之.      

耐150 ℃太阳翼基板结构胶黏剂性能研究

介绍了一种J-159结构胶黏剂,用于太阳翼基板结构的板-芯胶接,重点进行了胶黏剂的力学性能、真空挥发性能、耐辐照性能研究,同时开展了典型件的制备及热真空循环试验。结果表明,J-159胶黏剂在150℃下各项力学性能保持率均56%,远高于常用的J-47胶黏剂,具有很好的耐高温性能。同时,真空挥发性能和耐带电粒子辐照性能满足航天器空间应用要求,制备的典型件在-105～+150℃热真空循环试验后,外观质量、胶接质量及其他性能均符合指标要求,能够满足卫星太阳翼基板耐150℃及以下空间环境的使用需求。     

太阳闪烁影响下的星际通信链路参数设计

针对太阳闪烁作用于星际通信链路而产生的幅度闪烁、频谱扩展、相位闪烁、时延扩展问题,提出一种适用于星际通信链路的参数设计方法。该方法根据通信链路与太阳的几何关系,计算太阳风中等离子体作用于无线电波的幅度统计特性、时间谱特性,将计算结果作为通信链路的频率选择、传输信号带宽设计、调制方式选择、锁相环路带宽设计的约束条件,并以某空间探测任务为例进行了S、X、Ka三种频段下的信号传输性能仿真分析,结果表明,在太阳闪烁指数m<0.3的情况下,采用Ka频段+8PSK调制相结合的方式,对于太阳闪烁的抵抗能力最强。该方法设计的参数能够降低太阳闪烁对通信链路的影响,可作为工程实际系统设计的参照。     

Modeling the solar cosmic ray event of 13 December 2006 using ground level neutron monitor data

In order to understand the physics under extreme solar conditions such as those producing ground level enhancements of solar cosmic rays, it is important to use accurate and reliable models. The NM-BANGLE Model is a new cosmic ray model which couples primary solar cosmic rays at the top of the Earth’s atmosphere with the secondary ones detected at ground level by neutron monitors during GLEs. This model calculates the evolution of several GLE parameters such as the solar cosmic ray spectrum, anisotropy and particle flux distribution, revealing crucial information on the energetic particle propagation and distribution. The total output of the NM-BANGLE Model is a multi-dimensional GLE picture that gives an important contribution to revealing the characteristics of solar energetic particle events recorded at ground level. In this work, the results of the NM-BANGLE Model application to the recent GLE of 13 December 2006 are presented and discussed. Moreover, a comparison with the extreme event of 20 January 2005 (GLE69) has been realized.     

Proposal of new models of the bottom-side B0 and B1 parameters for IRI

The time series of hourly electron density profiles N(h) obtained from 27 ionosonde stations distributed world-wide have been used to obtain N(h) average profiles on a monthly basis and to extract the expected bottom-side parameters that define the IRI profile under quiet conditions. The time series embrace the time interval from 1998 to 2006, which practically contains the entire solar cycle 23. The Spherical Harmonic Analysis (SHA) has been used as an analytical technique for modeling globally the B0 and B1 parameters as general functions on a spherical surface. Due to the irregular longitudinal distribution of the stations over the globe, it has been assumed that the ionosphere remains approximately constant in form for a given day under quiet conditions for a particular coordinate system. Since the Earth rotates under a Sun-fixed system, the time differences have been considered to be equivalent to longitude differences. The time dependence has been represented by a two-degree Fourier expansion to model the annual and semiannual variations and the year-by-year analyses of the B0 and B1 have furnished nine sets of spherical harmonic coefficients for each parameter. The spatial–temporal yearly coefficients have been further expressed as linear functions of Rz12 to model the solar cycle dependence. The resultant analytical model provides a tool to predict B0 and B1 at any location distributed among the used range of latitudes (70°N–50°S) and at any time that improves the fit to the observed data with respect to IRI prediction.     

Gradient pattern analysis of short solar radio bursts

We analyze the weak component of the localized temporal pattern variability of 3 GHz solar burst observed by the Ondrejov radiospectrograph. A complex, short and weak impulsive sample from the time series was analyzed by applying a method based on the gradient pattern analysis and discrete wavelet decomposition. By analyzing canonical temporal variability patterns we show that the new method can reliably characterize the phenomenological dynamical process of short time series (N ? 10³ measurements) as the radio burst addressed here. In the narrowest sense, by estimating the mutual information distance in the gradient spectra, we show that the fluctuation pattern of the short and weak 3 GHz impulsive solar burst, with energetic amplitudes <350 SFU, is closer to the intermittent and strong MHD turbulent variability pattern.