磁悬浮电励磁三相直线同步电机离线参数辨识

建立磁悬浮电励磁三相直线同步电机(MSEETPLSM)的连续时间参数型状态空间方程数学模型,利用前向一阶差分方法将连续时间数学模型离散化成离散时间参数型状态空间方程数学模型,再利用z变换写成递推最小二乘算法标准形式的数学模型。利用递推最小二乘算法在初级转子静止状态下辨识出MSEETPLSM的电阻及自感参数。利用计算机数值仿真软件仿真MSEETPLSM参数的离线辨识算法,得到MSEETPLSM的初级与次级电阻与电感时域辨识曲线,仿真曲线收敛速度较快且辨识精度较高。仿真结果验证了该参数离线辨识算法的有效性。     

航空电子产品印制电路板组件中性清洗技术研究

印制电路板清洗是电子装配中的一个重要环节,它对电子产品的质量和可靠性有着极为重要的作用。通过对印制板清洗原理与影响因素分析,针对性使用优化参数的中性水基清洗剂对印制板组件进行试验,证实该类型清洗剂能够满足航空电子产品在印制板清洗方面的需求。     

某航空发动机应急油路数值分析

利用CFX软件对某航空发动机应急油路内部流动进行模拟,通过计算得到该航空发动机应急油路喷嘴出口压力随引射角度、引射距离、引射压力及喷嘴安装孔直径的变化规律。     

表贴式永磁同步电机永磁体偏心气隙磁场解析

采用分区域的方法对表贴式永磁同步电机磁极偏心的气隙磁场进行推导解析。将求解区域分为永磁体区域、气隙区域、定子槽区域和基于分离变量法利用各区域的边界条件得出相关系数,并在计及永磁体偏心的情况下求解电机气隙磁场。解析模型能够计算电机空载和负载气隙磁场的分布。将解析模型计算结果与有限元分析结果进行对比,发现所建立的解析模型具有较高的准确度。     

电路模拟吸波材料带宽拓展方法探索

电路模拟吸波材料有一定的频率选择特性,电磁波有效损耗的带宽通常比较窄,通过多层电路屏、掺杂电损耗介质、磁损耗介质层组合、磁电损耗组合的方法,对电路模拟结构吸波材料在2~18GHz区间电磁损耗带宽的拓展进行了初步探索。结果证明:四种方法都能够提高电路模拟吸波材料的有效吸波带宽,并能够不同程度地提高材料的吸波效率。多层电路屏、掺杂电损耗介质的多层电路屏、组合磁损耗介质层的多层电路屏、组合磁损耗介质层和电损耗介质的多层电路屏,其反射率≤-5dB的带宽较单层电路屏的1.2GHz分别增加了6.4、10.6、9.6、10.6GHz,最小反射率分别达到-8、-10、-12、-25dB。     

某航空设备模拟电路故障状态分类器设计及仿真

采用传统故障诊断方法对复杂模拟电路进行故障诊断,存在诊断速度慢、故障点难以准确定位等缺点,为此提出基于神经网络理论的故障状态分类器设计方法,以某型飞机自动驾驶仪854C放大器为例,对故障状态分类器进行了分析设计和仿真研究.仿真结果显示:所设计的基于神经网络理论的故障状态分类器实现了对此类航空设备模拟电路故障的快速、准确和有效的识别与定位.     

In-Situ Solar Wind and Magnetic Field Signatures of Interplanetary Coronal Mass Ejections

The heliospheric counterparts of coronal mass ejections (CMEs) at the Sun, interplanetary coronal mass ejections (ICMEs), can be identified in situ based on a number of magnetic field, plasma, compositional and energetic particle signatures as well as combinations thereof. We summarize these signatures and their implications for understanding the nature of these structures and the physical properties of coronal mass ejections. We conclude that our understanding of ICMEs is far from complete and formulate several challenges that, if addressed, would substantially improve our knowledge of the relationship between CMEs at the Sun and in the heliosphere.     

Microwave Diagnostics of Dynamic Processes and Oscillations in Groups of Solar Coronal Magnetic Loops

Low-frequency (LF) modulations of the solar microwave radiation (37 GHz) recorded at the Metsähovi Radio Observatory, are analyzed. Since the intensity of solar microwave radiation, produced by the electron gyrosynchrotron mechanism, is dependent on a value of the background magnetic field [Dulk, G. A.: 1985, Ann. Rev. Astron. Astrophys. 23, 169–224], slow variations of the magnetic field associated with disturbances of the electric current in a radiating source, can modulate the intensity of the microwave radiation. The observed multi-track features of the LF spectra are interpreted as a signature of a complex multi-loop structure of the radiating source. Application of the equivalent electric circuit models of interacting loops allows to explain and reproduce the main dynamical features of the observed LF modulation dynamic spectra.     

Location of Magnetic Reconnection in the Magnetotail

It is a crucial issue to know where magnetic reconnection takes place in the near-Earth magnetotail for substorm onsets. It is found on the basis of Geotail observations that the factor that controls the magnetic reconnection site in the magnetotail is the solar wind energy input. Magnetic reconnection forms close to (far from) the Earth in the magnetotail for high (low) solar wind energy input conditions.With the early Vela spacecraft observations, it was believed that magnetic reconnection started inside the Vela position, likely at 15 R_E. The later ISEE/IRM observations put magnetic reconnection beyond 20 R_E. The Vela event studies were made for highly active conditions, while the ISEE/IRM survey studies were made for moderate or quiet conditions. The finding of the factor that controls the site of magnetic reconnection in the magnetotail resolves the apparent discrepancy among various spacecraft results, and suggests solar cycle variation of the magnetotail reconnection site.     

机载电子显示器接地设计一例

从产品实际应用过程中发现的问题出发，通过试验，阐述了接地设计中“地环路”的影响及其解决方法。