Particle acceleration and kinematics in solar flares – A Synthesis of Recent Observations and Theoretical Concepts (Invited Review)

We review the physical processes of particle acceleration, injection, propagation, trapping, and energy loss in solar flare conditions. An understanding of these basic physical processes is inexorable to interpret the detailed timing and spectral evolution of the radiative signatures caused by nonthermal particles in hard X-rays, gamma-rays, and radio wavelengths. In contrast to other more theoretically oriented reviews on particle acceleration processes, we aim here to capitalize on the numerous observations from recent spacecraft missions, such as from the Compton Gamma Ray Observatory (CGRO), the Yohkoh Hard X-Ray Telescope (HXT) and Soft X-Ray Telescope (SXT), and the Transition Region and Coronal Explorer (TRACE). High-precision energy-dependent time delay measurements from CGRO and spatial imaging with Yohkoh and TRACE provide invaluable observational constraints on the topology of the acceleration region, the reconstruction of magnetic reconnection processes, the resulting electromagnetic fields, and the kinematics of energized (nonthermal) particles. This revised version was published online in June 2006 with corrections to the Cover Date.     

The massive star distribution in the Galaxy and the Magellanic Clouds

The numbers and distribution of Population I O-type stars and Wolf-Rayet stars are reviewed. The numbers of known WR stars in the Galaxy, the LMC and the SMC are 185, 114, and 9, respectively. Distances and galactic distributions determined by various authors are compared. The single star and binary distributions are discussed in the light of evolutionary studies.     

Radiation driven winds of hot stars: Theory of O-star atmospheres as a spectroscopic tool

The status of the continuing effort to construct radiation driven wind models for O-Stars atmospheres is reviewed. Emphasis is given to several problems relating to the fomation of UV line spectra the use of accurate atomic data, the inclusion of EUV radiation by shock heated matter, the simulation of photospheric line blocking.A new tool for O-star diagnostics is presented. This is based on the use of wind models to calculate synthetic high resolution spectra covering the observable UV region. A comparison with observed spectra then gives physical constraints on the properties of stellar winds and stellar parameters, additionally abundances can be determined.The astrophysical potential of this method is demonstrated by an application to two Of-stars, the galactic O4f-star -Puppis and the LMC O3f-star Melnick 42. With regard to effective temperatures and gravities, the results from the application of classical methods to the analysis of photospheric lines are only partially verified. Explanations for the shortcomings of classical NLTE methods are discussed.     

Spectral analyses of Wolf-Rayet stars: Theory,results, conclusions

Stratified Non-LTE models for expanding atmospheres became available in the recent years. They are based on the idealizing assumptions of spherical symmetry, stationarity and radiative equilibrium. From a critical discussion we conclude that this standard model is basically adequate for describing real Wolf-Rayet atmospheres and hence can be applied for quantitative spectral analyses of their spectra.By means of these models, the fundamental parameters have been determined meanwhile for the majority of the known Galactic WR stars. Most of them populate a vertical strip in the Herzsprung-Russell diagram at effective temperatures of 35 kK, the luminosities ranging from 10^4.5 to 10^5.9 L . Only early-type WN stars with strong lines and WC stars are hotter. The chemical composition of WR atmospheres corresponds to nuclear-processed material (WN: hydrogen burning in the CNO cycle; WC: helium burning). Hydrogen is depleted but still detectable in the cooler part of the WN subclass.Different scenarios for the evolutionary formation of the Wolf-Rayet stars are discussed in the light of the empirical data provided from the spectral analyses. Post-red-supergiant evolution can principally explain the basic observational properties, except the rather low luminosities of a considerable fraction of WN stars. Among the alternative scenarios, close-binary evolution can theoretically produce the least-luminous WN stars. However, final conclusions about the evolutionary formation of the WR stars are not yet possible.     

故障诊断专家系统

以运七飞机起落架为实例研究开发了通用故障诊断专家系统，对系统的需求分析和功能，知识的获取与表达、推理逻辑及系统模型建立等技术关键进行了论述，且用故障树分析、故障模式、影响分析及面向对象技术等方法作为解决关键的措施。     

多电飞机电源系统的负载稳定性分析

阐述了恒功率负载的概念及其特性,介绍了电源系统中恒功率负载的工作原理,并对多电飞机电源系统的系统特性进行了分析。在此分析基础上,提出了解决负阻抗特性引起的飞机电源系统不稳定的方法,最后给出了保证系统稳定的条件。     

汽车电子牌照系统设计

利用无线收发技术和计算机控制管理技术，来实现和完成汽车电子牌照的检测与车辆的管理，其特点是自动检查车牌，自动完成各种控制，该系统安装、测试、维修简单，成本低、效益高。     

一等环规测量仪的研制

一等环规测量仪是将激光干涉仪测长技术、静态光电显微镜瞄准技术和精密微位移定位技术作为主体测量技术，以上三项技术的有机结合使该仪器的测量不确定度达到了国际法制计量组织(OIML)规定的一等环规的测量要求。     

入侵检测中拒绝服务攻击模式分析

基于特征的IDS为了检测到攻击,必须处理能与攻击表现相匹配的攻击描述,该过程可以简化为与网络报文部分匹配的模式描述,也可以复杂化为将多传感器输出映射到抽象攻击表现的状态机描述或神经网络描述。描述了入侵检测系统(IDS)中涉及的几个典型拒绝服务攻击(DoS)模式,对这些DoS攻击模式进行了详细的分析。DoS特征是书写检测特定攻击过滤器的必要知识,详细描述了这些DoS攻击的特征,并提出了抵御DoS攻击的一个应对措施———IDS。     

AHP在企业货币资金占有率计算中的应用

持有一定数额的货币资金是企业维持正常生产经营的保证，文章利用层次分析法对企业货币资金的占有率计算问题进行了研究，为企业持有合理数量的货币资金提供一种有效的计算方法。