有/无铁芯轴向磁通风力发电机性能研究

针对有、无铁芯轴向磁通风力发电机哪种更适合在微风地区使用,对比分析了有铁芯和无铁芯发电机在不同转速时的效率、转矩特性及电能质量。通过对发电机基本参数的确定,建立有、无铁芯发电机3D有限元模型,对比有、无铁芯风力发电机的运行特性,并通过实验平台验证3D有限元计算结果。研究结果表明：发电机在额定运行状态下,磁钢用量相同时,有铁芯发电机效率比无铁芯发电机效率高4.2%,但有铁芯发电机存在齿槽转矩,发电机运行平稳性差;在磁钢用量及电枢绕组匝数相同时,无铁芯发电机效率比有铁芯发电机效率高0.3%且启动力矩更小;当磁通量相同时,无铁芯发电机效率比有铁芯发电机效率高5.7%,综上所述无铁芯发电机更适合在微风低速下运行。     

单向电永磁作动器结构优化与动态特性分析

针对电磁作动器的使用要求,设计出一种具有能耗低、吸力大及响应快等特点的新型单向电永磁作动器。结合有限元仿真软件,利用有限元法研究作动器的结构参数如铁芯齿形结构、平面结构、无永磁结构、铁芯的倾斜角度及衔铁位移（气隙厚度）等因素对作动器电磁吸力和响应速度的影响。结果表明,电磁吸力随着作动衔铁位移的增加而大幅度减小;倾角结构的铁芯设计能使作动器性能达到最佳,且铁芯的倾斜角度为50°时,电磁吸力有最大值3071N。     

压力敏感元件新材料的实验研究

对非晶态的和局部晶化的Ni68Si15B17合金薄带和其他一些非晶态的合金薄带,以及对康铜丝,做了受拉力时电阻变化率的测量比较,并做了电阻随温度的变化以及其他一些测量。从比较中看出,非晶态Ni68Si15B17合金具有的特性可能使它成为优良的压力敏感元件的新材料,尤其适于制作飞行器中的传感元件。     

罐车转向时液体晃动的仿真分析

采用VOF模型对罐车转向时液体晃动进行了数值模拟,对单室受力及侧倾力矩进行了计算.计算结果表明,无防波板时,随向心加速度增加,竖直、水平方向受力峰值及侧倾力矩均变大;随充液比增加,竖直方向受力峰值增大,水平方向受力峰值与侧倾力矩峰值先增大后减小;带防波板时,竖直、水平方向受力峰值减小,当防波板面积大于纵剖面积30%时防波板面积的增加能显著改善罐体受力;侧倾力矩峰值先增大后减小,在防波板面积等于纵剖面积30%时达到最大值,当防波板面积大于纵剖面积40%时防波板面积增加能提高防晃效果.     

激光束频率混叠误差分析

研究了激光外差干涉仪中存在的频率混叠现象、误差形成机理和变化规律。重点研究了共光路外差干涉仪中引起频率混叠的两个因素：激光光源的椭圆偏振元和Ｗｏｌｌａｓｔｏｎ棱镜的安装方位角误差，以及上述两因素引起的频率混叠误差的大小及变化规律。对进一步提高共光路外差干涉测量准确度具有现实意义。     

非晶态(Fe_(0.5)Ni_(0.5))_(80-x)Cr_xP_(14)B_6合金的内禀磁性和热稳定性的研究

对Cr含量变化对非晶态(Fe_(0.5)Ni_(0.5))_(80-x)Cr_xP_(14)B_6(x=0,1,2,3,4,6,10)合金薄带样品的内禀磁性和热稳定性进行了研究。对所得的随着Cr含量增加,样品的磁性原子的平均磁矩(?)和居里温度T_c的减少,热稳定性的提高等结果进行了讨论。当Cr含量x=4at％时,样品表现出一些特殊性质;而当x>4at％和<4at％时,样品的磁性和热稳定性的变化不尽相同。     

图解太阳系小天体（4）

<正>小行星带天体小行星带是太阳系中位于火星和木星轨道之间的一片环状区域,核心部分轨道半径介于2.06至3.27天文单位之间,质量中心大约在轨道半径2.8天文单位处。小行星带内绝大部分天体离心率都小于0.4、轨道倾角小于30°。典型值分别为离心率0.07、轨道倾角小于4°,因此,大部分小行星轨道都基本位于黄道面附近,且轨道接近圆形。这里拥有太阳系内已知数量最多的小天体,据估计直径在1千米以上的小天体数量达到100万颗以上,     

用频装备带内多频电磁辐射阻塞干扰效应预测方法

为解决用频装备复杂电磁环境效应准确评估的技术难题，从电磁辐射信号耦合传输的基本理论出发，推导揭示了射频前端线性不良和动态范围不足分别是导致用频装备电磁辐射效应对带内多频电磁辐射干扰场强有效值、幅值敏感的本质原因。在此基础上建立了2类用频装备的带内多频连续波电磁辐射效应模型，提出了通过正弦调幅波(调制深度100%)、单频连续波电磁辐射临界干扰场强有效值之比(E_ame/E_sine)确定受试装备电磁辐射敏感类型的方法。E_ame/E_sine>0.9时，受试装备对干扰场强有效值敏感，0.612 < E_ame/E_sine < 0.9时，受试装备对干扰场强幅值敏感。通信电台带内双频、三频电磁辐射效应试验验证表明:所提建模预测方法的误差小于10%，能够有效预测用频装备带内多频连续波电磁辐射效应。      

作为通用逼近子的模糊系统及其逼近性质

针对模糊控制系统提出通用逼近子与通用控制器概念。探讨模糊系统作为通用逼近子所具备的一些性质,较全面地综述了这一领域的最新研究成果。归纳由各种常用模糊推理方法生成的模糊推理系统,其中模糊推理的Ｔ－模运算主要包括乘积、取小、有界积与强制积运算。提出ｎ元Ｔ－模概念并讨论其基本性质,在此基础上导出各种模糊推理系统的统一数学描述。利用模糊基本函数形式化描述模糊系统的方法,比较了它们的结构特征,以及由此导出的     

变截面毛细通道中气泡的运动特性分析

为了确定复合材料成型过程中气泡的运动条件,利用变截面毛细模拟通道实验系统,研究了气泡在变截面毛细管中的运动行为,分析了气泡长度、毛细管半径及液体种类对气泡垂直穿出行为的影响,并从理论角度推导出气泡穿出的临界压力方程.研究结果表明,气泡垂直穿出变截面毛细通道所需要的临界压力差,随气泡长度和毛细管半径的增大而减小,液体种类对其也有明显影响,实验结果与理论计算值基本吻合.该研究结果将为复合材料成型中工艺参数的优化提供实验依据.      

REM measurements aboard Mir during 1995

Measurements of the South Atlantic Anomaly (SAA) made with the Radiation Environment Monitor (REM) aboard Mir from November 1994 to February 1996 are presented. During this period an increase of the SAA radiation by ≈25% is observed, which coincides with a lowering of the radio solar flux. Radio solar flux is one of the parameters controlling the earth's atmospheric distribution and with it the absorption of inner radiation belt protons forming the SAA. Due to the altitude gradient of the atmospheric density, the proton fluxes in the SAA are anisotropic (loss cone, east-west effect). The measured distribution can be accounted for by basic models.     

空间粒子辐射对卫星中集成芯片的影响

本文分析了在“风云一号(B)”气象卫星环境中各种粒子辐射在集成芯片临界体积中产生的能量沉积, 即LET(线性能量传输);得到了银河宇宙线1≤Z≤28、银河宇宙线异常成分(C、N、O、Ne、Ar、Fe)、内辐射带质子等产生的LET, 计算了其分别产生的单粒于事件(SEU)翻转率。      

Inner radiation belt source of helium and heavy hydrogen isotopes

Nuclear interactions between inner zone protons and atoms in the upper atmosphere provide the main source of energetic H and He isotopes nuclei in the radiation belt. This paper reports on the specified calculations of these isotope intensities using various inner zone proton intensity models (AP-8 and SAMPEX/PET PSB97), the atmosphere drift-averaged composition and density model MSIS-90, and cross-sections of the interaction processes from the GNASH nuclear model code. To calculate drift-averaged densities and energy losses of secondaries, the particles were tracked in the geomagnetic field (modelled through IGRF-95) by integrating numerically the equation of the motion. The calculations take into account the kinematics of nuclear interactions along the whole trajectory of trapped proton. The comparison with new data obtained from the experiments on board RESURS-04 and MITA satellites and with data from SAMPEX and CRRES satellites taken during different phases of solar activity shows that the upper atmosphere is a sufficient source for inner zone helium and heavy hydrogen isotopes. The calculation results are energy spectra and angular distributions of light nuclear isotopes in the inner radiation belt that may be used to develop helium inner radiation belt model and to evaluate their contribution to SEU (single event upset) rates.     

机器人修形磨削工具坐标系的精确标定方法

针对目前机器人修形磨削系统中接触轮姿态标定精度低影响磨削精度的问题,提出了一种实验测量的工具坐标系标定方法,姿态标定精度达0.05°.首先总结了通用静态标定法的不足之处,提出了新标定方法的构思并且理论证明了该方法的正确性.介绍了实验系统的组成,并在机器人砂带磨削系统上做了磨削实验.采集了磨削处的实验数据,分析实验数据,获得接触轮的实际偏转角,把偏转角补偿到磨削路径的工具坐标系上,最后完成了工具坐标系补偿后的重复性实验,证明了该方法的可行性和准确性.     

Theoretical modelling of X-ray fluorescence signals for different lunar compositions and dependence on solar activity

We present a forward modelling technique for calculating the surface X-ray spectra for a variety of lunar terrains. Our calculations considered variations in solar fluxes from solar quiescent condition to large flare activity (M1 flare), and expected elemental concentrations in the target, as well as yield, instrumental, and viewing geometry parameters for X-ray induced fluorescence from the lunar surface. Additionally, we present estimates of anticipated XRF signals from prominent K_α lines observable by a collimated 14 cm² X-ray detector from a 100 km lunar orbit with ∼20 km spatial resolution. Our results show that Mg, Al and Si characteristic K_α lines can be observed for all solar conditions. The Ca K_α lines line can be differentiated from a fixed background during more energetic solar conditions such as C1 and M1 flares, whereas Ti and Fe lines are identifiable only during C1 and M1 solar flare conditions for Apollo 12 site composition. Both the K_α X-ray intensity ratios of Mg/Si and Al/Si correlate well with concentration ratios of Mg/Si and Al/Si, respectively, for B1 and M1 solar conditions. The K_α X-ray intensity ratios of Fe/Si and Ca/Si correlates with concentration ratios of Fe/Si and Ca/Si, respectively, for M1 solar condition. In principle, the modelling technique outlined here can be used to determine absolute elemental abundances (Mg, Al, Si, Ca, Ti and Fe) from X-ray spectra measured during recent and future lunar missions.     

基于NOAA卫星数据的辐射带质子投掷角分布研究

利用NOAA-12卫星数据对空间环境平静时期太阳同步轨道处辐射带质子投掷角分布进行了研究. 根据投掷角分布的经验公式,计算出90°投掷角的质子方向强度和各向异性指数n. 质子投掷角分布按n的取值范围可分为三类,即90°峰值分布、平顶分布和蝴蝶形分布. 观测证实,对于辐射带质子,三种分布类型均存在并且具有明显的空间区域特征. 在内辐射带边缘地区90°峰值分布占主要优势;在外辐射带高L值区域,90°峰值分布明显减少,平顶分布和蝴蝶形分布逐渐增多. 针对90°峰值分布,研究了质子强度各向异性的区域分布特征,对于内辐射带区域,n值随L值的增大而增大,对于外辐射带,n值表现为逐渐下降的趋势. 为了研究质子投掷角分布对磁地方时的依赖关系,分析了能量为250～800keV的质子在两个不同磁地方时范围的投掷角分布规律. 结果显示,在内辐射带,质子强度的投掷角分布相对稳定,随磁地方时的变化并不显著;而在外辐射带的高L值区域,质子强度的投掷角分布随磁地方时变化明显,与磁地方时之间有明显的依赖关系.      

Inner magnetosphere variations after solar proton events. Observations on Mir space station in 1989-1994 time period.

Measurements on board the Mir space station have been used to study the dose rate and the particle flux distribution in the inner magnetosphere. The measurements have been performed with the Bulgarian-Russian dosimeter-radiometer Liulin. The paper concentrates on the dynamics of the observed "new" and "second" maxima which were created after Solar Proton Events (SPE) in the 1989-1994 time. The "second" belt was first observed after the SPE on October 20, 1989, and the last observation was after the SPE on February 20, 1994. The creation of the "new" belt is a unique phenomena seen in the Liulin data set after the SPE on March 23, 1991 and relates to the magnetic storm on March 24. The new belt fully disappears in the middle of 1993.     

Low altitude dose measurements from APEX, CRRES and DMSP

Dosimeter data taken on the APEX (1994–1996), CRRES (1990–1991) and DMSP (1984–1987) satellites have been used to study the low altitude (down to 350 km) radiation environment. Of special concern has been the inner edge of the inner radiation belt due to its steep gradient. We have constructed dose models of the inner edge of the belt from all three spacecraft and put them into a personal computer utility, called APEXRAD, that calculates dose for user-selected orbits. The variation of dose for low altitude, circular orbits is given as a function of altitude, inclination and particle type. Dose-depth curves show that shielding greater than 1/4 in Al is largely ineffectual for low altitude orbits. The contribution of outer zone electrons to low altitude dose is shown to be important only for thin shields and to have significant variation with magnetic activity and solar cycle.     

太阳周期活动对低高度内辐射带高能质子的影响

利用NOAA-15卫星1998年到2011年近13年的高能质子全向通量观测资料, 分析了一个太阳活动周内, 低高度内辐射带高能质子通量的分布变化特性及其物理原因, 比较了观测结果与AP8模型的不同. 研究表明, 低高度内辐射带高能质子通量与太阳活动水平的反相关关系与磁壳参数L值及磁场B值有关; L值越低, B值越大的空间点, 其高能质子通量与太阳活动水平的反向相关性越明显. 高能质子通量随太阳活动水平的变化存在明显滞后现象, L值越高、 B值越小的空间点, 滞后现象就越明显, 滞后严重时可以达到一年左右的时间; 这种滞后现象反映出低高度内辐射带高能质子的源与损失达到平衡是一个中长期过程. 通过与AP8模型计算结果的比较分析可以看出, 利用AP8模型时, 仅考虑地磁场长期变化对质子通量的影响可能会夸大低高度内辐射带局部高能质子通量的增强.