基于B-P本构模型的涡轮盘应力分析

针对Bodner-Partom统一粘塑性本构方程,采用Euler前差显式积分方法,编制了用户子程序,把该本构方程结合进了大型通用有限元软件ANSYS,进行了一维和二维的算例验证,并针对某涡轮盘进行了三维应力分析。该程序可考虑材料变形的率相关、循环加载等情况,适用于航空发动机高温部件非线性结构分析。      

自由涡轮叶片/轮盘耦合振动特性分析

自由涡轮是航空发动机的关键部件,其工作环境非常恶劣,承受着离心载荷、热载荷、气动载荷及振动载荷等的复合作用。利用UG软件对某型自由涡轮2级涡轮轮盘/叶片进行3维实体建模,导入ANSYS构建其耦合振动分析的有限元模型,以静强度分析中的模型为基础,考虑温度场和离心载荷的影响,计算出涡轮叶片/轮盘不同转速下的动频。从Campbell图可见,涡轮叶片/轮盘在工作转速下没有发生共振的危险,该型涡轮设计合理。     

基于ANSYS的多辐板风扇盘结构 优化设计技术

基于ANSYS优化平台,建立了风扇盘子午面优化设计模型,筛选了主要的优化设计变量.针对典型风扇盘设计问题,分别进行了单辐板及多辐板结构优化设计.结果表明,在满足轮盘变形、强度要求的条件下,多辐板风扇盘比单辐板风扇盘可明显减轻质量,并且其应力分布更为均匀,说明对于轮缘较宽的风扇盘,多辐板轮盘结构具有明显优越性.同时,多辐板轮盘结构还有利于增强轮缘弯曲刚度.      

基于蒙特卡罗方法的小卫星偏心分离动力学分析

对小卫星单星偏心分离动力学进行了研究。建立了基于多体动力学理论的偏心在轨分离模型,用ADAMS平台对小卫星分离过程动力学进行仿真,结果显示两者误差小于0.15%,验证了仿真模型的正确性。用Monte-Carlo法对分离动力学性能进行了优化,分析了不同因素对分离角速度和分离速度的敏感度,给出了三种优化方案。     

航天记录器的发展和转型

概述中国航天记录器近五十年的发展历程,阐述航天记录器技术转型的十年过程,简要介绍目前航天记录器应用的新进展。     

相变光盘多层膜系结构的最佳光匹配研究

论述了相变光盘最佳膜系结构的设计。采用导纳矩阵法计算膜系的能量反射率，用量优化计算方法编程计算，提出了第二大极值解作为在工艺上可行的实用光盘的膜系结构，并按这种膜系结构制作样品，其擦写循环数达１００万次上。     

Numerical study on flow fields and aerodynamics of tilt rotor aircraft in conversion mode based on embedded grid and actuator model

A method combining rotor actuator disk model and embedded grid technique is presented in this paper, aimed at predicting the flow fields and aerodynamic characteristics of tilt rotor aircraft in conversion mode more efficiently and effectively. In this method, rotor's influence is considered in terms of the momentum it impacts to the fluid around it; transformation matrixes among different coordinate systems are deduced to extend actuator method's utility to conversion mode flow fields' calculation. Meanwhile, an embedded grid system is designed, in which grids generated around fuselage and actuator disk are regarded as background grid and minor grid respectively, and a new method is presented for ‘donor searching' and ‘hole cutting' during grid assembling. Based on the above methods, flow fields of tilt rotor aircraft in conversion mode are simulated, with threedimensional Navier–Stokes equations discretized by a second-order upwind finite-volume scheme and an implicit lower–upper symmetric Gauss–Seidel(LU-SGS) time-stepping scheme. Numerical results demonstrate that the proposed CFD method is very effective in simulating the conversion mode flow fields of tilt rotor aircraft.     

The ‘soot line’: Destruction of presolar polycyclic aromatic hydrocarbons in the terrestrial planet-forming region of disks

Interstellar material is highly processed when subjected to the physical conditions that prevail in the inner regions of protoplanetary disks, the potential birthplace of habitable planets. Polycyclic aromatic hydrocarbons (PAHs) are abundant in the interstellar medium, and they have also been observed in the disks around young stars, with evidence for some modification in the latter. Using a chemical model developed for sooting flames, we have investigated the chemical evolution of PAHs in warm (1000–2000 K) and oxygen-rich (C/O < 1) conditions appropriate for the region where habitable planets may eventually form. Our study focuses on (1) delineating the conditions under which PAHs will react and (2) identifying the key reaction pathways and reaction products characterizing this chemical evolution. We find that reactions with H, OH and O are the main pathways for destroying PAHs over disk timescale at temperatures greater than about 1000 K. In the process, high abundances of C₂H₂ persist over long timescales due to the kinetic inhibition of reactions that eventually drive the carbon into CO, CO₂ and CH₄. The thermal destruction of PAHs may thus be the cause of the abundant C₂H₂ that has been observed in disks. We propose that protoplanetary disks have a ‘soot line’, within which PAHs are irreversibly destroyed via thermally-driven reactions. The soot line will play an important role, analogous to that of the ‘snow line’, in the bulk carbon content of meteorites and habitable planets.     

Growth of hydrodynamic perturbations in accretion disks: Possible route to non-magnetic turbulence

We study the possible origin of hydrodynamic turbulence in cold accretion disks such as those in star-forming systems and quiescent cataclysmic variables. As these systems are expected to have neutral gas, the turbulent viscosity is likely to be hydrodynamic in origin, not magnetohydrodynamic. Therefore, MRI will be sluggish or even absent in such disks. Although there are no exponentially growing eigenmodes in a hydrodynamic disk because of the non-normal nature of the eigenmodes, a large transient growth in the energy is still possible, which may enable the system to switch to a turbulent state. For a Keplerian disk, we estimate that the energy will grow by a factor of 1000 for a Reynolds number close to a million.     

失调叶片盘耦合振动的力学模型

借助于子结构模态综合法,为研究真实的失调叶片盘耦合振动问题提出了一种非常接近于实际叶片盘的力学模型和简便的理论分析方法;并通过对一个实际失调叶片盘的强迫振动试验,对力学模型、计算公式和程序进行了考核验证。结果表明,试验与计算相当吻合。