基于神经网络的电机智能保护器研究

介绍了一种电机智能保护装置系统，分析了对电动机进行各类保护的原理，并且针对过载保护．提出一种基于人工神经网络的电动机长期过载运行温升预测的算法，将这种算法应用于实际的保护中．有效地弥补了不能用数学模型精确描述电机运行中发热和散热过程的缺陷。实验证明，在样本足够多的情况下，这种方法是切实可行的。     

基于模糊聚类的模糊神经网络在非定常气动力建模中的应用

建立了一种基于模糊聚类的模糊神经网络模型.该模型利用模糊聚类技术确定系统的模糊空间和模糊规则数,利用BP算法调整模糊神经网络的权系数.应用该模型对某飞机模型做俯仰-滚转耦合运动的非定常气动力进行了辨识.结果表明,基于模糊聚类的模糊神经网络计算速度快,辨识结果与实验结果符合较好.用模糊聚类技术可以解决模糊神经网络的结构辨识问题,基于模糊聚类的模糊神经网络可以很好地用于复杂机动飞行的非定常气动力建模.     

一个基于WINDOWS环境的网络连接服务

该文介绍了在校园网环境及WINDOWS平台，采用TCP/IP协议设计并开发PING网络连接服务和客户机/服务器功能的VC^ 程序。     

基于神经网络的某导弹姿态控制系统故障诊断

介绍了多层前向神经网络及其算法 ,讨论了神经网络在故障诊断方面的应用 ,并对某导弹姿态控制系统的典型故障进行了神经网络建模 ,经测试取得了良好的效果。     

高校教务管理模式探析

该教务管理模式是在总结全国现有大多数普通高校教务管理模式的基础上进行开发研究的,其高效的事务处理机制和信息管理模式,为学校的教务工作提供了直观的评价数据,为提高教务工作效率和推进高校教学改革提供了重要的参考依据。利用先进的技术手段和指导思想提高教育、培养、管理水平,对人才的综合素质培养,对打造高品牌大学均有深远意义。教务管理模式系统是数字化校园极为重要的组成部分之一,实现统一、规范、自动化、高效的信息管理系统事在必行。     

洪都集团企业级信息系统数据备份策略研究

分析了洪都集团当前企业级信息系统数据备份系统中存在的问题,结合目前的主流数据备份策略,提出了基于SAN(存储局域网)的高速、可靠、安全的洪都集团新的企业级信息系统数据备份策略。     

基于CORBA的分布式网络管理的研究

详细地介绍了将CORBA这种面向对象地分布式中间件用于网络管理的方法,着重探讨在实现基于CORBA的分布式网络管理中的关键的技术-CORBA/SNMP网关,通过CORBA/SNMP网关实现CORBA域与SNMP域的透明通信。     

基于图像识别的发动机内窥智能检测系统研究

介绍了一种基于图像识别技术的航空发动机内窥检测的新方法，采用最大类间方差法计算二值化分割的最佳阈值，并将提取的图像特征输入神经网络进行分层识别，最后由专家系统对损伤程度进行了诊断。通过现场测试，证明了该方法的有效性和实用性．     

应用ART1神经网络仿真车间分组

阐述了ART1神经网络在制造单元设计过程中形成零件族的基本方法,并在基于MATLAB的软件平台上,利用其神经网络工具箱对生产过程中的实际情况进行了仿真和应用。     

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.