电火花成型机数控系统的研究

通过研究开放式数控系统的体系结构，结合开放式的运动控制器，开发了基于PC的四轴联动电火花数控系统，本研究通过采用神经模糊控制智能技术，并结合数据库，依据放电间隙状况对电火花成型加工过程进行实时控制，保证加工过程处于优化状态，文中还详细研究了高精度双闭环控制以实现工件的高精度加工。     

轴向载荷下复合材料元件吸能能力的试验研究

试验研究了三种结构形式的复合材料元件在轴向准静态载荷下的压溃过程和能量吸收能力。通过组试件在轴向准静态载荷下的压溃试验，研究复合材料的缓冲吸能机理，对吸能能力进行了定义，并对试件的峰值截荷、持续压溃载荷和吸能能力等作了定量分析。     

金属零件的一种快速成型制造方法

金属零件的快速制造是快速成型技术的最终目标之一,也是当今快速成型领域的一大研究热点。本文在介绍快速成型技术的一个重要分支－选区激光烧结的基础上,提出了一种基于小功率激光快速成型系统的金属零件成型工艺。这种方法首先烧结金属与有机粘结剂的混合粉末,生成“绿件”,而后除粘、熔渗金属,最终得到致密的金属件。最后,文中给出了加工实例,并对这种工艺的影响因素进行了详细的分析与讨论。     

基于聚束照射SAR成像算法的条带SAR数据处理

为实现聚束照射合成孔径雷达（SAR）与条带模式SAR成像算法上的统一，本文利用两种模式之间的内在联系，将条带模式SAR数据分块处理，等效成聚束模式数据。然后，用聚束照射SAR成像算法实现条带数据的成像处理。针对具体数据，文中还对成像区大小的选择作了分析，并推导出成像长度与滤波器带宽应当满足的关系式。包场数据的处理严格证实了理论分析并验证了本文运用的方法。     

飞机穿越微下击暴流风切变的智能控制

在应用模糊逻辑建模与辨识方法建立微下击暴流风切变模型的基础上，根据恒定俯仰姿态改出微下击暴流的飞行引导策略，提出了一种改出微下击暴流风切变的模糊反馈控制系统，并将遗传算法应用于该模糊逻辑控制器的设计。结果表明，本文提出的建模方法能够更真实地反映出飞机穿越微下击暴流风场的动态特性；采用模糊逻辑控制器，可使得飞机在穿越微下击暴流风场时具有较好的改出性能；另外，遗传算法的应用对已设计的模糊逻辑控制器进行了优化，进一步改善了飞机穿越微下击暴流的性能。     

基于批生产的逐段式车间作业调度算法

探讨了离散作业型（Job shop）车间中的作业调度的分阶段模型，并根据离散作业调度的阶段性提出了基于作业状态空间的逐段式车间作业调度算法，通过对一个实际车间作业调度仿真比较，此算法运算速度比最短加工时间（SPT）和最少工作量剩余（LWR）算法快，其调度结果在实际作业车间具有可执行性。     

一种新颖组合变换器拓扑研究与应用

基于电源模块并联和串联的思想，提出了一种新颖双管正激组合变换器拓扑，克服了双管正激变换器副边二极管电压应力过高，输出电压和电流脉动大，只能应用于输出中低压场合的缺点，具有副边二极管电压应力低，可靠性高，原边开关管电流应力低，输出电压和电流脉动小，磁芯元件体积小等优点，本文对该新颖组合变换器进行分析，仿真和实验，表明适合应用于输入中，高电压，输出高压，大电流场合，并成功应用于某型飞机6KVA逆变器前级变换器，各项技术指标均符合设计要求。     

快速可重构信息系统的框架研究(英文)

变化和重构是快速可重构信息系统 (RRIS)的两个核心概念 ,RRIS对变化的适应或演化能力使它优于传统信息系统。本文首先提出 RRIS的体系结构 ,然后以 RRIS框架为重点 ,讨论框架的定义、分类及设计 ,研究框架的构成、构成元素 (业务构件 )的设计及构件如何在构架的组织下协调地安插在 CORBA的软总线上 ,实现类似硬件IC的即插即用。构件在框架上即插即用的灵活机制及热点构件 (反映变化 )的灵活运用 ,提高了框架的可扩展性、可定制性 ,从而提高了 RRIS适应变化的可重构性。     

Interplanetary shocks and sudden impulses during solar maximum (2000) and solar minimum (1995–1996)

In this work a study is performed on the correlation between fast forward interplanetary shock parameters at 1 Astronomical Unit and sudden impulse (SI) amplitudes in the H-component of the geomagnetic field, for periods of solar activity maximum (year 2000) and minimum (year 1995–1996). Solar wind temperature, density and speed, and total magnetic field, were taken to calculate the static pressures (thermal and magnetic) both in the upstream and downstream sides of the shocks. The variations of the solar wind parameters and pressures were then correlated with SI amplitudes. The solar wind speed variations presented good correlations with sudden impulses, with correlation coefficients larger than 0.70 both in solar maximum and solar minimum, whereas the solar wind density presented very low correlation. The parameter better correlated with SI was the square root dynamic pressure variation, showing a larger correlation during solar maximum (r = 0.82) than during solar minimum (r = 0.77). The correlations of SI with square root thermal and magnetic pressure were smaller than with the dynamic pressure, but they also present a good correlation, with r > 0.70 during both solar maximum and minimum. Multiple linear correlation analysis of SI in terms of the three pressure terms have shown that 78% and 85% of the variance in SI during solar maximum and minimum, respectively, are explained by the three pressure variations. Average sudden impulse amplitude was 25 nT during solar maximum and 21 nT during solar minimum, while average square root dynamic pressure variation is 1.20 and 0.86 nPa^1/2 during solar maximum and minimum, respectively. Thus on average, fast forward interplanetary shocks are 33% stronger during solar maximum than during solar minimum, and the magnetospheric SI response has amplitude 20% higher during solar maximum than during solar minimum. A comparison with theoretical predictions (Tsyganenko’s model corrected by Earth’s induced currents) of the coefficient of sudden impulse change with solar wind dynamic pressure variation showed excellent agreement, with values around 17 nT/nPa^1/2.     

Great solar bursts of October 19, 22 and 23, 1989

Itapetinga measurements at 48 GHz with the multibeam technique are used to determine the relative position of solar burst centroid of emission with high spatial accuracy and time resolution. For the Great Bursts of October 19,22, 1989, with a large production of relativistic particles, and October 23, it is suggested that, at 48 GHz, the bursts might have originated in more then one source in space and time. Additionally the October 19 and 22 Ground Level Events exhibited very unusual intensity-time profiles including double component structures for the onset phase. The Bern observatory spectral radio emission data show a strong spectral flattening typical for large source inhomogeneties. The interpretation for this is that large solar flares are a superposition of a few strong bursts (separated both in space and time) in the same flaring region.