基于哈希链表和时间链表的HTTP代理缓存机制的实现

随着互联网的快速发展，越来越多的用户需要访问Internet资源，局域网人的众多用户如何能够通过一条Internet连接进行快速的网络浏览？这涉及到WEB代理服务器的核心部分--HTTP缓存系统。HTTP代理服务器的缓存系统将用户浏览的网页保存在代理服务器中，一旦有用户浏览相同的网页并且该网页还没有更新，则代理服务器直接将网页传递给用户，无需重新下载。因此，缓存明显加快了浏览速度。本文首先介绍了代理服务器的缓存原理，然后对缓存机制的具体功能进行了划分，最后给出基于哈希链表和时间链表的缓存系统的实现方法。     

组合式三相逆变器负载特性的分析与研究

分析了组合式三相逆变器，该逆变器三相分别独立控制，易实现功率器件的软开关、无输出变压器的三相四线制输出和模块化的结构；具体分析了影响该三相逆变器输出电压不平衡度的因素，讨论了其带对称与不对称负载的特性，着重分析了不对称负载对每个单相逆变器的影响，得到了组合式三相逆变器中单模块设计与普通单相逆变器的不同点，并给出了实验数据和相应波形。实验结果表明，组合式三相逆变器具有良好的带不平衡负载的能力和优良的电气性能。     

M46J高模量碳纤维预浸QY8911纤维束性能研究

以航空发动机应用为背景，研究了M46J／QY8911缠绕复合材料的预浸纱制备方法及性能，根据M46J特性，对现有的GB3326中纤维束力学性能测试试样的加强方式进行了改进，制作了M46J浸渍QY8911树脂的纤维束试样并测试其力学性能，同时与M46J浸渍环氧树脂的纤维束的力学性能进行比较，研究表明，不同树脂特性，不同固化工艺以及制造中所施加的张力都会影响到纤维束的纤维利用率。     

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。     

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。     

An empirical model of the plasma environment around Mercury

Since the flyby observations by Mariner 10 in 1974 and 1975, Mercury has been one of the most interesting objects for space physics and planetary exploration. The MESSENGER and BepiColombo missions now plan to revisit this planet. In order to design plasma instruments for the BepiColombo mission, we have estimated electron and ion fluxes around Mercury with an empirical model, which has been developed for the Earth’s magnetotail. The solar wind data needed as input parameters are derived from Helios observations. The result shows that our predicted electron fluxes at aphelion agree well with the Mariner-10 data. It is also noted that ion instruments must cover a very wide dynamic range of proton fluxes. However, the applicability of the Earth’s magnetospheric model to Mercury is, in itself, an important issue for comparative magnetospheric studies.     

Research on a complex CME event including Hα, LASCO, radio and MDI observations

We present our research on a fast and decelerating partial halo coronal mass ejection (CME) event detected in multi-wavelengths in the chromosphere and the corona on 14 October, 1999. The event involved a whole complex active area which spanned more than 40° of heliolongitude. It included a strong solar flare (XI/1N) and a complex eruptive filament within an active region of the entire complex. Especially, several radio sources were detected in the decimetric range prior to the CME by the Nançay Radioheliograph (NRH). A linear force-free field extrapolation of the Michelson Doppler Imager (MDI) magnetogram was performed to calculate the magnetic topology of the complex prior to the triggering of the event. The presence of a coronal null point combined with the occurrence of two distant and nearly simultaneous radio sources put strong arguments in favor of the generalized breakout model for the triggering of the eruption. The analysis of the subsequent development of the event suggests that large interconnecting loops were ejected together with the CME.     

Non-Thermal Processes in Cosmological Simulations

Non-thermal components are key ingredients for understanding clusters of galaxies. In the hierarchical model of structure formation, shocks and large-scale turbulence are unavoidable in the cluster formation processes. Understanding the amplification and evolution of the magnetic field in galaxy clusters is necessary for modelling both the heat transport and the dissipative processes in the hot intra-cluster plasma. The acceleration, transport and interactions of non-thermal energetic particles are essential for modelling the observed emissions. Therefore, the inclusion of the non-thermal components will be mandatory for simulating accurately the global dynamical processes in clusters. In this review, we summarise the results obtained with the simulations of the formation of galaxy clusters which address the issues of shocks, magnetic field, cosmic ray particles and turbulence.     

1994年2月21日行星际激波引起的磁暴

利用Imp-8,Geotail和Goes-6等卫星资料,研究了1994年2月21日0900UT到达地球磁层的行星际激波引起的磁暴期间,从太阳风向磁层传输能量的有关问题.结果指出:（1）南向行星际磁场（IMF）的长持续时间不是太阳风向磁层输能的必要条件.南北振荡的,较强IMF也能产生显著的能量传输;（2）行星际扰动磁场通过弓激波和磁层顶后扰动磁能增加,增幅将近5倍;（3）在磁层内扰动磁场的Bz分量在1×10-4Hz附近显著被吸收.这一低频扰动磁场可能是磁暴期间导致氧离子和质子等环电流粒子向内扩散并被加速的原因之一.