基于MBSE思想的航空发动机控制系统设计方法

在航空发动机控制系统设计开发过程中,存在需求理解偏差、需求实现描述不清晰、设计过程缺失等问题,严重影响产 品后续使用。为了构建完整、规范、准确的系统设计要求,完整描述系统设计过程,引入基于模型的系统工程思想。通过需求分析 将用户需求条目化,并对每条需求进行确认;通过功能分解,将复杂系统模块化;利用功能描述将需求量化、图形化,明确各项功能 的具体行为;在要求制定过程中引入数据流管理,将整个系统设计过程有机结合在一起。结果表明：采用基于模型的系统工程思 想构建满足产品研发的控制系统正向设计方法,实现了顶层需求的100%覆盖和追溯,可将模糊的需求通过建模方式具体化、显形 化。通过N1测量对设计方法进行了验证,表明该方法可用于工程设计。     

不同压比状态下超声速射流冲击斜板的声场/流场特性

为研究超声速射流冲击斜板的噪声特性及声源特性,针对不同压比下,超声速射流流场及声场分别进行了高频PIV（particle image velocimetry)测量与远场噪声测量。PIV测量结果可观测到激波格栅形成过程以及冲击斜板对它的影响。声场测量结果可捕捉到自由射流与冲击射流中不同的纯音频率随压比增加的转变过程。通过一一对比各纯音模态与流场模态,可区分各纯音模态的声源特性。结果表明:当压比在2.0~3.2之间时,共出现五种纯音模态:A模态纯音频率为剪切层大尺度涡脱落频率,此时流场呈现同轴模态;d模态和e模态中纯音频率主要为冲击纯音频率,且e模态出现时流场转化为螺旋模态,这是一种不稳定模态;当压比大于等于2.53时,纯音模态稳定成单一模态B,B模态纯音频率为啸叫频率,其流场结构转化回同轴模态,啸叫频率对斜板的存在与否不敏感;啸叫频率随着压比的增加逐渐减小,其二次谐频在基频幅值较小的方向上会出现一个强声波辐射。      

面向复杂构型飞机的非定常气动力建模与辨识

不论是现代高机动隐身战斗机的设计需求还是常规布局飞机的飞行动力学分析,深入研究大迎角飞行时的非线性非定常气动力模型都极其重要。基于纵向运动小振幅及大振幅强迫振荡试验数据,分析了常规稳定导数模型的准确性,并从导数模型出发发展了简化涡流和分离流时间迟滞效应的非定常气动力线性模型和非线性模型,最后应用风洞典型机动历程模拟试验验证了模型的有效性。结果表明：对于复杂构型高机动飞机模型,发展并改进的非线性微分方程模型可以准确预测飞机不同机动下的非定常气动力特性,具有较强的工程可行性。     

基于Bayesian-MCMC估计的隐身飞机RCS模型优化

对隐身飞机的雷达散射截面(RCS)统计建模时,传统方法通过直接计算RCS样本的统计特征估计模型参数,可能会产生较大的拟合误差。本文提出采用贝叶斯-蒙特卡罗(Bayesian-MCMC )方法提高起伏模型的参数估计精度,从而减小模型的拟合误差。首先将卡方分布模型和对数正态分布模型进行贝叶斯推导,得到其特征参数的后验估计表达式。然后采用MCMC算法构造后验分布的马尔可夫链,从而计算特征参数的估计值。最后通过比较2种方法的拟合曲线及其误差可知,本文方法适用于2种起伏模型,模型参数的估计误差比收敛误差门限值低1~2个数量级,2种分布模型的拟合精度均提高50%以上。      

面向深空时变信道的数据传输策略

将呈现随机“好”、“坏”状态跳变的深空Ka频段链路噪声温度建模为两状态Gilbert-Elliot信道,考虑深空下行发送端只能获得延迟的信道状态信息（CSI）的限制,结合部分观测马尔科夫决策理论设计了基于延迟CSI预测信道状态的自适应最大化吞吐量传输策略。理论推导了在深空通信环境下最优传输策略的关键阈值,并给出了简化的闭合解计算式。通过地球-火星通信参数仿真,校验了该方案能有效提高吞吐量,提高文件传输效率。     

二氧化氮催化硝化甘油分解机理的数值计算

采用密度泛函理论（DFT）在B3LYP/6-31+G（d,p）水平上模拟计算了NO₂对硝化甘油（NG）催化分解的反应机理。通过与O—NO₂均裂、HNO₂分子内消去反应对比发现,NO₂分子对NG分解反应有显著的催化效应;NG的催化分解途径有α-H夺氢催化和β-H夺氢催化,计算得出2种途径的反应能垒分别为105.337 k J/mol和124.381 k J/mol,说明α-H夺氢催化更容易发生。     

一种无人机旋翼设计方法

为了提高多旋翼无人机的航时,本文提出了一种无人机旋翼设计方法.该方法根据给定的爬升速度、旋翼转速、拉力、旋翼直径、桨叶数、翼型,能够计算出最大力效旋翼的几何特性,包括弦长分布、桨叶角分布.利用该方法设计了某型无人机的旋翼,得到了桨叶角和弦长沿径向的分布.制作了旋翼模型,并且开展了旋翼台架试验.在不同转速下,测量出拉力、...     

Research on failure criterion of composite based on unified macro- and micro-mechanical model

A new unified macro- and micro-mechanics failure analysis method for composite structures was developed in order to take the effects of composite micro structure into consideration. In this method, the macro stress distribution of composite structure was calculated by commercial finite element analysis software. According to the macro stress distribution, the damage point was searched and the micro-stress distribution was calculated by reformulated finite-volume direct averaging micromechanics (FVDAM), which was a multi-scale finite element method for composite. The micro structure failure modes were estimated with the failure strength of constituents. A unidirectional composite plate with a circular hole in the center under two kinds of loads was analyzed with the traditional macro-mechanical failure analysis method and the unified macro- and micro-mechanics failure analysis method. The results obtained by the two methods are consistent, which show this new method’s accuracy and efficiency.     

Si3 N4 粉体的分散及表面改性

研究了以聚丙烯酸铵为分散剂的Si3N4悬浮体的分散特性,以及酸洗和热氧化两种表面改性方法对Si3N4悬浮体的分散性和流变特性的影响.结果表明:分散剂聚丙烯酸铵的最佳酸碱环境为pH=9,最佳使用含量为0.2wt％,酸洗可有效去除粉料中的金属杂质,使Si3N4粉体在悬浮体中粒径分布更集中且粒径主峰值向小粒径移动,同时可使悬浮体的黏度降低.热氧化处理可大幅度降低Si3N4悬浮体的黏度,提高其流变特性.     

Solar Wind Turbulence and the Role of Ion Instabilities

Solar wind is probably the best laboratory to study turbulence in astrophysical plasmas. In addition to the presence of magnetic field, the differences with neutral fluid isotropic turbulence are: (i) weakness of collisional dissipation and (ii) presence of several characteristic space and time scales. In this paper we discuss observational properties of solar wind turbulence in a large range from the MHD to the electron scales. At MHD scales, within the inertial range, turbulence cascade of magnetic fluctuations develops mostly in the plane perpendicular to the mean field, with the Kolmogorov scaling $k_{\perp}^{-5/3}$ for the perpendicular cascade and $k_{\|}^{-2}$ for the parallel one. Solar wind turbulence is compressible in nature: density fluctuations at MHD scales have the Kolmogorov spectrum. Velocity fluctuations do not follow magnetic field ones: their spectrum is a power-law with a ?3/2 spectral index. Probability distribution functions of different plasma parameters are not Gaussian, indicating presence of intermittency. At the moment there is no global model taking into account all these observed properties of the inertial range. At ion scales, turbulent spectra have a break, compressibility increases and the density fluctuation spectrum has a local flattening. Around ion scales, magnetic spectra are variable and ion instabilities occur as a function of the local plasma parameters. Between ion and electron scales, a small scale turbulent cascade seems to be established. It is characterized by a well defined power-law spectrum in magnetic and density fluctuations with a spectral index close to ?2.8. Approaching electron scales, the fluctuations are no more self-similar: an exponential cut-off is usually observed (for time intervals without quasi-parallel whistlers) indicating an onset of dissipation. The small scale inertial range between ion and electron scales and the electron dissipation range can be together described by $\sim k_{\perp}^{-\alpha}\exp(-k_{\perp}\ell_{d})$ , with α?8/3 and the dissipation scale ? _d close to the electron Larmor radius ? _d ?ρ _e . The nature of this small scale cascade and a possible dissipation mechanism are still under debate.