直径比对冲击气膜组合冷却流动与换热的影响

 通过数值模拟,研究了涡轮叶片弦中区所采用的新型双层腔冷却结构的冷却特性,系统分析了冲击气膜组合冷却的流动与换热特性,讨论了冷气进口雷诺数Re、吹风比M以及气膜孔与冲击孔的直径比D/d对组合冷却效果的影响。计算参数范围是：冷气进口雷诺数Re＝2 000～5 000,吹风比M＝0.6～2.0。计算结果表明, 冷气进口Re,M以及D/d对双层腔结构冷却效果的影响非常明显,在计算范围内:（1）Re和M越高,冷却效果越好;（2）当冲击孔直径一定时,增加气膜孔的直径,冷却效果会随之增加;（3）当冲击孔直径一定时,增加气膜孔的直径,流阻系数会随之减小。     

The Role of Magnetic Reconnection in CME Acceleration

Observations carried out from the coronagraphs on board space missions (LASCO/SOHO, Solar Maximum and Skylab) and ground-based facilities (HAO/Mauna Loa Observatory) show that coronal mass ejections (CMEs) can be classified into two classes based on their kinematics evolution. These two classes of CMEs are so-called fast and slow CMEs. The fast CME starts with a high initial speed that remains more or less constant; it is also called the constant-speed CME. On the other hand, the slow CME starts with a low initial speed, but shows a gradual acceleration; it is also called the accelerated and slow CME. Low and Zhang [Astrophys. J. 564, L53–L56, 2002] suggested that these two classes of CMEs could be a result of a difference in the initial topology of the magnetic fields associated with the underlying quiescent prominences. A normal prominence magnetic field topology will lead to a fast CME, while an inverse quiescent prominence results in a slow CME, because of the nature of the magnetic reconnection processes. In a recent study given by Wu et al. [Solar Phys. 225, 157–175, 2004], it was shown that an inverse quiescent prominence magnetic topology also could produce a fast CME. In this study, we perform a numerical MHD simulation for CMEs occurring in both normal and inverse quiescent prominence magnetic topology. This study demonstrates three major physical processes responsible for destabilization of these two types of prominence magnetic field topologies that can launch CMEs. These three initiation processes are identical to those used by Wu et al. [Solar Phys. 225, 157–175, 2004]. The simulations show that both fast and slow CMEs can be initiated from these two different types of magnetic topologies. However, the normal quiescent prominence magnetic topology does show the possibility for launching a reconnection island (or secondary O-line) that might be thought of as a “CME’’.     

Analysis of crack opening stresses for center- and edge-crack tension specimens

Accurate determination of crack opening stress is of central importance to fatigue crack growth analysis and life prediction based on the crack-closure model. This paper studies the crack opening behavior for center- and edge-crack tension specimens. It is found that the crack opening stress is affected by the crack tip element. By taking the crack tip element into account, a modified crack opening stress equation is given for the center-crack tension specimen. Crack surface displace- ment equations for an edge crack in a semi-infinite plate under remote uniform tension and partially distributed pressure are derived by using the weight function method. Based on these displacements, a crack opening stress equation for an edge crack in a semi-infinite plate under uniform tension has been developed. The study shows that the crack opening stress is geometry-dependent, and the weight function method provides an effective and reliable tool to deal with such geometry depen- dence.     

一种高精度夹具的设计原理

通过对定位精度高达２μｍ,又非常便捷装卸的瑞士ＥＲＯＷＡ夹具结构原理的介绍,以引起国内同行的关注,旨在推广应用于我国航空精密零件及工模具生产中,以期解决长期困惑我国的高位置精度问题。     

切削工具材料的发展综述

具体介绍切削工具材料如高速钢、硬质合金、陶瓷、金属陶瓷、刀具涂层技术、超硬材料的演变和进展。     

高性能与高功能纤维的发展

概述了用于复合材料增强体的高性能纤维和具有各种物理与化学功能用途的高功能纤维的进展现状并推测其发展趋势。     

激光功率与底面状态对选区激光熔化球化的影响

为研究激光功率与底面状态对选区激光熔化熔池流动的影响,基于离散单元法建立了选区激光熔化铺粉模型,采用粒径分布与实验相符的马氏体时效钢粉末分别铺展到平坦底面和增材底面上,将计算获得的粉末分布导入到基于有限体积法建立的选区激光熔化熔池计算流体力学模型中,研究激光功率和基板底面粗糙度对熔池流动和熔道表面形貌的影响。采用激光单道扫描实验验证铺粉模型和选区激光熔化模型。结果表明：随着激光功率的降低,单位长度的球化数量增加;由于增材底面使熔池润湿性变差,同时又对熔池流动行为产生扰动,使得增材粗糙底面上熔道的球化数量增加。选区激光熔化铺粉模拟及激光单道扫描模拟结果与实验结果吻合较好。本研究可为选区激光熔化工艺中工艺参数的选择提供理论指导。     

基于FTA方法对某型飞机直流电源系统故障分析

对某型飞机直流电源系统的“一个整流器故障”进行了分析 ,介绍了故障树分析的应用方法 ,并且对实际故障建立了故障树     

A Class of TVD Type Combined Numerical Scheme for MHD Equations With a Survey About Numerical Methods in Solar Wind Simulations

It has been believed that three-dimensional, numerical, magnetohydrodynamic (MHD) modelling must play a crucial role in a seamless forecasting system. This system refers to space weather originating on the sun; propagation of disturbances through the solar wind and interplanetary magnetic field (IMF), and thence, transmission into the magnetosphere, ionosphere, and thermosphere. This role comes as no surprise to numerical modelers that participate in the numerical modelling of atmospheric environments as well as the meteorological conditions at Earth. Space scientists have paid great attention to operational numerical space weather prediction models. To this purpose practical progress has been made in the past years. Here first is reviewed the progress of the numerical methods in solar wind modelling. Then, based on our discussion, a new numerical scheme of total variation diminishing (TVD) type for magnetohydrodynamic equations in spherical coordinates is proposed by taking into account convergence, stability and resolution. This new MHD model is established by solving the fluid equations of MHD system with a modified Lax-Friedrichs scheme and the magnetic induction equations with MacCormack II scheme for the purpose of developing a combined scheme of quick convergence as well as of TVD property. To verify the validation of the scheme, the propagation of one-dimensional MHD fast and slow shock problem is discussed with the numerical results conforming to the existing results obtained by the piece-wise parabolic method (PPM). Finally, some conclusions are made. This revised version was published online in August 2006 with corrections to the Cover Date.