关于对发展航空运输产业若干政策的思考

用大量事实从不同侧面说明航空运输在国民经济中的地位日显重要,为国家的贡献逐年增大.同时分析了航空运输经济效益下降的原因,并提出一系列政策建议以推动航空运输向高层次方向发展.     

Relativistic astrophysics explorer

The great success of the Rossi X-Ray Timing Explorer (RXTE) has shown that X-ray timing is an excellent tool for the study of strong gravitational fields and the measurement of fundamental physical properties of black holes and neutron stars. Here, we describe a next-generation X-ray timing mission, the Relativistic Astrophysics Explorer (RAE), designed to fit within the envelope of a medium-sized mission. The instruments will be a narrow-field X-ray detector array with an area of 6 m² equal to 10 times that of RXTE and a wide-field X-ray monitor. We describe the science made possible with this mission, the design of the instruments, and results on prototype large-area X-ray detectors.     

线性系统的最小解耦设计—一般情形

利用线性系统“根”的概念，研究了输出分块情形下的最小阶动态解耦设计问题，一方面利用根刻画了解耦补偿器的最小阶数，并且给出了设计最小阶补偿器的算法，另一方面获得了新的解耦判据。     

Thermal radiation from magnetized neutron stars

Surface thermal emission has been detected byROSAT from four nearby young neutron stars. Assuming black body emission, the significant pulsations of the observed light curves can be interpreted as due to large surface temperature differences produced by the effect of the crustal magnetic field on the flow of heat from the hot interior toward the cooler surface. However, the energy dependence of the modulation observed in Geminga is incompatible with blackbody emission: this effect will give us a strong constraint on models of the neutron star surface.     

对RLC串联电路中通频带与RLC参数关系的讨论——从一道习题引起的问题

讨论了RLC串联电路中通频带与RLC参数的关系,说明在设计一个RLC串联谐振电路时,在给定谐振频率,电感量和频带宽度时,上下边界频率不能只满足通频带宽度而任意假定,还应满足通频带与RLC这些参数之间关系的表达式.     

含钉孔有限大板应力集中系数解法—解析最小二乘法

在研究孔边应力集中系数的问题中，利用了复变函数方法，设预先满足所有的基本方程的待定复函数，再利用最小二乘法使其满足边界条件，从而解出孔边应力集中系数。     

智能优化算法及其在飞行器优化设计领域的应用综述

在对国内外相关文献进行系统研究的 基础上,阐述了飞行器优化设计领域应用较为广泛的几种智能优化算法的基本原理,分析了 算法的优缺点和改进方法,总结了算法在飞行器轨迹、气动和控制等学科优化设计中的应用 情况。同时,文章对在飞行器优化设计领域应用刚刚起步,但较有发展前景的智能优化算法的 特点和应用情况进行了概述。最后,对智能优化算法在飞行器优化设计领域应用的未来研究 方向进行了分析。
     

出/入口面积相等的收缩-扩张孔气膜冷却特性

采用一种可进行全表面测量的瞬态液晶测量技术测量了一种出口面积与入口面积相等的收缩扩张形孔的气膜冷却特性,研究了动量比(0.5,1,2,4)的影响,并与传统的出口面积小于入口面积的收缩扩张形孔的气膜冷却特性进行了对比。结果表明:收缩扩张形孔射流均完全覆盖了孔下游壁面,射流的交汇以及对涡结构使得孔中心线附近区域的冷却效率较低,而孔间区域的冷却效率较高。在上游区域,孔间区域的换热系数比相对孔中心线附近区域的较高,而在下游区域,对涡结构又使得孔间区域的换热系数比相对较低。出口-入口面积比不同的两种收缩扩张形孔的冷却效率分布规律和换热系数比分布规律都比较相似,但出口-入口面积比为1的收缩扩张形孔的冷却效率以及上游区域的换热系数比的数值都相对较低。而且出口-入口面积比为1的收缩扩张形孔的流量系数明显高于出口-入口面积比小于1的收缩扩张形孔。     

Metal Enrichment Processes

There are many processes that can transport gas from the galaxies to their environment and enrich the environment in this way with metals. These metal enrichment processes have a large influence on the evolution of both the galaxies and their environment. Various processes can contribute to the gas transfer: ram-pressure stripping, galactic winds, AGN outflows, galaxy-galaxy interactions and others. We review their observational evidence, corresponding simulations, their efficiencies, and their time scales as far as they are known to date. It seems that all processes can contribute to the enrichment. There is not a single process that always dominates the enrichment, because the efficiencies of the processes vary strongly with galaxy and environmental properties.     

The Expansion of Coronal Plumes in the Fast Solar Wind

Coronal plumes are believed to be essentially magnetic features: they are rooted in magnetic flux concentrations at the photosphere and are observed to extend nearly radially above coronal holes out to at least 15 solar radii, probably tracing the open field lines. The formation of plumes itself seems to be due to the presence of reconnecting magnetic field lines and this is probably the cause of the observed extremely low values of the Ne/Mg abundance ratio. In the inner corona, where the magnetic force is dominant, steady MHD models of coronal plumes deal essentially with quasi-potential magnetic fields but further out, where the gas pressure starts to be important, total pressure balance across the boundary of these dense structures must be considered. In this paper, the expansion of plumes into the fast polar wind is studied by using a thin flux tube model with two interacting components, plume and interplume. Preliminary results are compared with both remote sensing and solar wind in situ observations and the possible connection between coronal plumes with pressure-balance structures (PBS) and microstreams is discussed. This revised version was published online in June 2006 with corrections to the Cover Date.