智能控制大功率氨压机制冷系统

本文将模糊控制、神经元控制等智能控制技术成功地应用于大型活塞式氨压机制冷系统，实现了恒转矩负载的变频调速节能。实际运行结果证明，该智能控制的大功率氨压机制冷系统工作稳定、控制精度高、节能效果显著，具有很好的经济效益及推广应用价值。     

卫星抗辐射加固技术

分析了FY－1C卫星运行轨道空间辐射环境，介绍了整星、单机、器件抗辐射要求。卫星研制过程中，对各单抗和系统在技术设计、元器件设计、软件编制等的抗辐射加固设计要求。特别对有CPU和存储器的单粒子翻转效应（SEU）和闩锁效应（SEL）试验。仪器和系统的软件均用故障注入的方法完成了抗SEU的仿真试验。     

76°/40°双三角翼前缘涡破裂及其控制实验研究

流动显示结果表明,喷流能有效地推迟双三角翼前缘涡的破裂,且随着攻角的增大,前缘涡破裂位置逐渐推后,喷流极大地改善了大攻角情况下前缘涡的非对称破裂特性,能有效地克服可能出现的机翼的"摇滚"现象.另外,后缘喷流可以减弱乃至消除前缘涡混掺现象的发生,进而有利于飞行器的操纵.     

关联性与文化的解读和建构

根据Sperber和Wilson的关联理论及其认知语境观,说明外语读者如何在认知语境中寻找最佳关联,可以对作者所设置的文化缺省进行连贯解读,从而实现跨文化图式的建构。     

海河两岸传统文化商贸区的无形资产开发利用研究

针对传统文化商贸区的无形资产资源特点与海河开发主题定位,进行了深入研究.将无形资产资源分成老字号、老品牌和旅游商贸文化两部分,并对现在经营过程中存在的问题提出了提升老字号竞争力、发展旅游品牌、政府营造宏观经济环境三大方面的对策及具体建议.     

新时期高校学生党建工作的思考

文章以学生党建工作的实践角度，从认识学生党员发展工作的重要性，学生党员发展基本途径和教育培养过程做了探讨。     

起落架落震试验测试系统的现状及其发展

能动地我国起落架落震试验测试系统发展的现状进行分析，指出了落震试验测试系统所存在的问题，说明了未来的发展重点及方向。     

Modeling of dynamic evolution of coronal loops

Parameters of expanding magnetic loops and arches and of mass flows generated by them in the corona have been computed in a 1D two-fluid approximation. Two possible trigger mechanisms of the coronal transients have been considered: (i) sudden increase of the background magnetic field strength, and (ii) heating and compression plasma inside these magnetic structures. We discuss the formation of shock waves and their dependence on dynamics and geometry of the magnetic structures.     

Solar Gamma-Ray Spectroscopy

Interactions of ions accelerated in solar flares produce gamma-ray lines and continuum and neutrons. These emissions contain a rich set of observables that provides information about both the accelerated ions and the environment where the ions are transported and interact. Ion interactions with the various nuclei present in the ambient medium produce gamma-ray lines at unique energies. How abundance information is extracted from the measurements is discussed and results from analyses of a number of solar flares are presented. The analyses indicate that the composition of the ambient gas where the ions interact (typically at chromospheric densities) is different from that of the photosphere and more like the composition of the corona, exhibiting low-FIP elemental enhancements that may vary from flare to flare. Evidence for increased Ne/O and the photospheric ³He abundance is also discussed.     

Observations of loops and prominences

We review recent observations by the Yohkoh-SXT in collaboration with other spacecraft and ground-based observatories of coronal loops and prominences. These new results point to problems that SoHO will be able to address. With a unique combination of rapid-cadence digital imaging (32 s full-disk and 2 s partial-frame images), high spatial resolution (2.5 arcsec pixels), high sensitivity (EM 10⁴² cm^–3), a low-scatter mirror, and large dynamic range, SXT can observe a vast range of targets on the Sun. Over the first 21 months of Yohkoh operations, SXT has taken over one million images of the corona and so is building up an invaluable long-term database on the large-scale corona and loop geometry. The most striking thing about the SXT images is the range of loop sizes and shapes. The active regions are a bright tangle of magnetic field lines, surrounded by a network of large-scale quiet-Sun loops stretching over distances in excess of 10⁵ km. The cross-section of most loops seems to be constant. Loops displaying significant increase in the ratio of the footpoint to loop-top diameter () are the exception, not the rule, implying the presence of widespread currents in the corona.All magnetic structures show changes. Time scales range from seconds to months. The question of how these structures are formed, become filled with hot plasma, and are maintained is still open. While we see the propagation of brightenings along the length of active-region loops and in X-ray jets with velocities of several hundred km/s, much higher velocities are seen in the quiet Sun. In XBP flares, for example, velocities of over 1000 km/s are common. Active-region loops seem to be in constant motion, moving slowly outward, carrying plasma with them. During flares, loops often produce localized brightenings at the base and later at the apex of the loop. Quiescent filaments and prominences have been observed regularly. Their coronal manifestation seems to be an extended arcade of loops overlying the filament. Reliable alignment of the ground-based data with the X-ray images make it possible to make a detailed intercomparison of the hot and cold plasma structures over extended periods. Hence we are able to follow the long-term evolution of these structures and see how they become destabilized and erupt.