基于激光反射层析法的换能器声场测量技术及仿真研究

换能器的辐射声场分布能够直接反映出换能器声学性能的好坏,若不能精确测量出换能器的辐射声场,则会对换能器的诊断和评估造成严重影响。从理论仿真的角度出发,推导了运用激光反射层析法重建换能器辐射声场的理论公式,着重利用推导出的理论公式对激光反射层析法进行了仿真计算。结果表明激光反射层析法能够精确地重建出换能器的辐射声场分布及声场中的声压量值,这为换能器的声场重建及声压测量提供了一种可行的方法。     

小型磁悬浮CMG高速转子动框架效应前馈补偿与实验

磁悬浮控制力矩陀螺是航天器快速姿态控制与快速机动的新型空间执行机构。由于动框架效应,框架转动输出力矩反作用于飞轮转子,会导致磁轴承的径向载荷和控制电流发生改变。为抑制动框架效应对磁浮转子的影响,在分析力矩输出时高速磁浮转子受力特性的基础上,采用角速率前馈控制策略实现对动框架效应引发的力矩扰动的有效抑制,并在所研制的75Nms立式小型磁悬浮控制力矩陀螺上进行了整机输出特性测试。试验结果表明：该方法能在保证磁浮转子高速稳定的前提下有效抑制动框架效应,满足整机力矩输出的要求。     

石英挠性加速度计温度特性测试与建模

为分析石英挠性加速度计在不同温度条件下的特性和规律,对加速度计两个主要参数偏值K₀和标度因数K₁的温度特性测试方法进行研究。根据变温速率和保温时间建立了加速度计的静态和动态温度曲线,并在不同的温度条件下对两只加速度计样品进行测试。利用最小二乘法对测量得到的加速度计温度特性进行建模,并提出通过温度特性曲线评判加速度计性能优劣的基本方法。最后将温度特性模型应用到系统精度补偿上,并取得了较好的效果。     

质子交换炉温度场均匀性分析与优化

针对质子交换炉的温度场均匀性问题,结合质子交换炉的结构特点,基于FLUENT用户自定义函数（UDF）开发了质子交换炉炉温控制算法,并在此基础上提出了多种加热控温方案;利用FLUENT软件对不同方案下的质子交换炉温度场进行仿真,分析不同控温方式下炉内温度场均匀性与传感器位置布置、加热丝布置高度的关系,找到最佳方案。结果表明:采用三段控温、3个传感器位置分别布置在3段加热丝中间、加热丝布置高度4倍于均匀温区长度时炉内温度场均匀性最好,均匀温区内最大偏差为0.03℃;对于既定结构的立式炉体,增加加热丝布置高度、优化设计传感器布置方案和炉体控温方式可以提高温度场均匀性。该方法为同类电加热炉温度场均匀性的优化设计提供了思路。      

磁悬浮控制敏感陀螺转子前馈解耦内模控制

磁悬浮控制敏感陀螺以洛伦兹力磁轴承（LFMB）为力矩器驱动转子偏转。针对磁悬浮控制敏感陀螺转子径向转动自由度间存在耦合的问题以及转子偏转高精度快响应要求,提出一种前馈解耦内模控制方法。根据洛伦兹力磁轴承的工作原理建立了转子偏转动力学模型,并设计了前馈解耦矩阵实现转子径向偏转解耦,在此基础上,采用二自由度内模控制器（2-DOF IMC）对转子进行高精度快响应偏转控制。MATLAB仿真结果表明所提出的控制方法可有效实现对陀螺转子偏转的完全解耦,且转子偏转响应时间较交叉PID算法减少57.1%,受0.1sin（2πt）°正弦信号扰动影响产生的偏转波动幅值较交叉PID算法减少76%。      

A study of a long duration B9 flare-CME event and associated shock

We present and discuss here the observations of a small long duration GOES B-class flare associated with a quiescent filament eruption, a global EUV wave and a CME on 2011 May 11. The event was well observed by the Solar Dynamics Observatory (SDO), GONG H$\alpha$, STEREO and Culgoora spectrograph. As the filament erupted, ahead of the filament we observed the propagation of EIT wave fronts, as well as two flare ribbons on both sides of the polarity inversion line (PIL) on the solar surface. The observations show the co-existence of two types of EUV waves, i.e., a fast and a slow one. A type II radio burst with up to the third harmonic component was also associated with this event. The evolution of photospheric magnetic field showed flux emergence and cancellation at the filament site before its eruption.     

口径近场的特征谱

 提出口径近场特征谱的概念,以描述口径设计近场特征。特征谱包括角域谱和时域谱,分别定义为口径近场区空域场和频域场在角域和时域的变换。理论分析和计算结果表明,特征谱可以在角域和时域上分离有限大口径的直达波和绕射波,因而可以用来描述口面尺寸、形状和场分布等条件改变时绕射场的相对变化,这对紧缩场设计具有参考价值。基于口面场卷积法,计算、比较了限度为5 m×5 m圆口径和方口径近场在X波段特征谱分布。并导出：口径近场角谱为口径场角谱和网络响应函数角谱的乘积,网络响应函数等效于一个空间角谱滤波器。     

非均匀磁化等离子体层的电磁特性分析

基于分层传播原理提出了一种计算电磁波在非均匀磁化等离子体层中反射率和吸收率的模型,并数值分析了等离子体密度与碰撞频率,以及背景磁场强度对电磁波的反射和吸收特性的影响.研究表明:该法所得结果与文献的传播矩阵(SMM)法一致.数值分析发现:低密度高碰撞频率等离子体可减少等离子体层对入射波的功率反射;高密度高碰撞频率等离子体可改善其对入射波的功率反射宽频带吸收特性;背景磁场强度可明显改变等离子共振吸收频段.     

Magnetospheric electric field variations caused by storm-time shock fronts

On January 20, 2005 there was an X 7.1 solar flare at 0636 UT with an accompanied halo coronal mass ejection (CME). The resultant interplanetary shock impacted earth ∼36 h later. Near earth, the Advanced Composition Explorer (ACE) spacecraft observed two impulses with a staircase structure in density and pressure. The estimated earth-arrival times of these impulses were 1713 UT and 1845 UT on January 21, 2005. Three MINIature Spectrometer (MINIS) balloons were aloft on January 21st; one in the northern polar stratosphere and two in the southern polar stratosphere. MeV relativistic electron precipitation (REP) observed by all three balloons is coincident (<3 min) with the impulse arrivals and magnetospheric compression observed by both GOES 10 and 12. Balloon electric field data from the southern hemisphere show no signs of the impulse electric field directly reaching the ionosphere. Enhancement of the balloon-observed convection electric field by as much as 40 mV/m in less than 20 min during this time period is consistent with typical substorm growth. Precipitation-induced ionospheric conductivity enhancements are suggested to be (a) the result of both shock arrival and substorm activity and (b) the cause of rapid (<6 min) decreases in the observed electric field (by as much as 40 mV/m). There is poor agreement between peak cross polar cap potential in the northern hemisphere calculated from Super Dual Auroral Radar Network (SuperDARN) echoes and horizontal electric field at the MINIS balloon locations in the southern hemisphere. Possible reasons for this poor agreement include (a) a true lack of north–south conjugacy between measurement sites, (b) an invalid comparison between global (SuperDARN radar) and local (MINIS balloon) measurements and/or (c) radar absorption resulting from precipitation-induced D-region ionosphere density enhancements.