表面裂纹理论的回顾与评述(下)

本文简要地介绍了近几十年国内外表面断裂力学理论的发展状况及所取得的一些成果，重点介绍了应力强度因子求法和裂纹扩展速率的描述。同时对应用于圆柱体上的表面裂纹应力强度因子求法及裂纹扩展速率的描述等方面成果进行了评述。     

基于CFD/CSD耦合的叶轮机叶片失速颤振计算

为了研究叶轮机叶片的失速颤振特性,发展了一种计算流体力学与计算结构力学(CFD/CSD)时域耦合方法。该方法通过每一物理时刻CFD和CSD的循环迭代实现了耦合计算。在CFD分析中,采用鲁棒性较好的空间离散格式AUSM+-UP,并基于延迟脱体涡模型(DDES)模拟了带分离流动。在结构分析中,通过模态法构建了旋转叶片动力学方程并运用杂交多步方法进行求解。以孤立转子Rotor37为例,计算了不同工况下流场总体与细节参数,与实验结果的对比验证了CFD算法的精度。对某转子叶片进行了颤振特性研究,计算所得的广义位移时间响应曲线表明该叶片在近失速工况下会发生失速颤振,其表现形式为一阶弯曲模态发散且各阶模态之间不耦合。分析表明,流场不稳定和非定常效应是引起失速颤振的关键因素,同时折合频率的降低也会导致原本气动弹性稳定的叶片发生失速颤振。     

跨声速压气机多圆柱孔式处理机匣设计与扩稳机理研究

基于对跨声速轴流压气机内部失稳触发机制的认识,设计了一种新型多圆柱孔式处理机匣结构。对带该处理机匣的跨声速轴流压气机转子Rotor-37的内部流动进行了全三维非定常数值模拟,结果表明该新型多圆柱孔式处理机匣结构可使压气机的综合裕度提高6.5%,而最高效率点效率仅降低0.19%。对多圆柱孔式处理机匣的扩稳机理进行了详细分析,结果表明处理机匣能有效消除低速流体团引起的通道阻塞现象,并将低速阻塞流体团抽吸进入处理机匣容腔,然后从前端喷口预旋喷出以抑制叶顶区域的流动分离,从而有效提高跨声速轴流压气机的失速裕度。     

三维数模随动下的机翼结构重量优化

目前,基于快速建模下的重量重心估算系统得到了快速发展。为了进一步提高结构重量估算精度,研究了如何在重量重心快速分析(WCGA)系统环境中构建优化模块。以机翼结构重量优化为例,提出优化流程,对优化模块功能进行分解,给出模型简化要求。以A320飞机机翼为例,对梁和长桁进行优化,结果显示,经过优化,有效减轻了结构重量,且相比于传统的减重优化设计方法,极大提高了计算效率。     

某型压差活门的动态特性分析

压差活门是航空发动机数控系统燃油计量装置中重要的液压部件,其稳定性和动态性能直接影响控制系统的整体性能。根据压差活门非线性微分方程,采用小偏差线性化方法,推导出了压差活门的动态数学模型,得到了压差活门的方框图以及传递函数。选取某压差活门参数建立了Simulink仿真模型,分别在频域和时域分析了其动态性能。结果表明:在频域上,比较了有无节流器时的回路增益函数伯德图,认为敏感油路上的节流器可以改善稳定性且提高控制精度,通过设计节流器的尺寸可以调节穿越频域,从而改善系统的动态性能;在时域上,分析了不同节流器尺寸下阶跃响应的动态性能,其试验结果与实际工程经验一致。     

民机高速风洞试验的阻力雷诺数效应修正

在飞机设计阶段,获得准确的气动特性数据对设计者是十分重要的,采用缩比模型的风洞试验是主要途径之一。但是风洞条件限制了试验的Re数,从而影响了对跨音速巡航阻力的评估,因此需要对风洞试验结果的阻力进行Re数效应修正。分析了风洞试验结果阻力的误差构成,提出了Re数效应修正的风洞试验数据基础;进一步就跨音速巡航阻力的构成进行分析,论述了对最小阻力和升致阻力分项修正的方法,并对修正结果进行了验证,得到了一种可靠的工程方法。     

卫星ATM网络中自适应FEC情况下的有效带宽估计

针对采用自适应前向差错控制（AFEC）的卫星异步传递模式（ATM）网络，研究了两种有效带宽估计方法。由于AFEC码率的动态特性使业务实际的传输速率具有不固定性，因此估计有效带宽时要考虑AFEC的影响。首先针对一般卫星时变信道和多码率AFEC情况下的卫星ATM，应用流体近似方法分析了有效带宽的计算，然而该方法要求的条件及计算复杂度均比较高，应用中有局限性。以此方法为基础，提出了采用修正因子的估计方法。数值结果表明采用修正因子的有效带宽估计方法比较简单可靠，适用面较广。     

耳朵识别身份系统

打击恐怖主义首先要预防恐怖分子,生物识别技术有助于将恐怖分子从人群中识别出来.耳朵是长期保持稳定的一个生物特征,并且耳朵的独特性十分明显.介绍了耳朵识别系统的系统功能和设计思路,采用VC 6.0和SQL SERVER 2000数据库,实现耳朵图像数据采集、图像预处理、图像存储等基本功能.     

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’’.     

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.