考虑可压缩与热传导的壁面函数边界条件及其应用

考虑到可压缩和热传导效应的壁面函数边界条件,被耦合到了采用k-ω两方程湍流模型、用有限体积法求解N-S方程的程序中。壁面函数基于耦合的速度和温度型,并且在边界层内的粘性子区和对数区内一致有效。引入壁面函数边界条件后,通过算例验证在y <100的范围内,得到的物面压力、摩阻、热流与实验结果比较,结果可靠。而无壁面函数边界条件时,要得到相同精度的结果,要求y ≈1。壁面函数的引入,为工程上准确预测飞行器在湍流流动中表面受力与气动热提供了保障。     

A swept fin-induced flow field with different height mounting gaps

In order to apply the air fin successfully and ensure the maneuverability of hypersonic vehicle, a key problem to be studied urgently is the heat flux brought by the fin mounting gap. The appearance of mounting gap and fin shaft can induce many complex flow structures which need more attentions to be investigated. Under Ma 6, Nano-tracer-based Planar Laser Scattering (NPLS) and Temperature Sensitive Paints (TSP) were applied to visualize and measure transient flow structures and heat flux distribution of a swept fin-induced flow field with different height mounting gaps. Complementarily, Reynolds-averaged N-S equations were solved with k-ω SST turbulent model. The heat flux distribution results of numerical simulation and TSP observed the change of high heat flux region with different mounting gap, both in position and magnitude. The streamlines based on Computational Fluid Dynamics (CFD) and flow visualization results obtained by NPLS revealed the cause of high heat flux region. The high heat flux region in this flow field is mainly related to the reattachment of vortex and flow stagnation. The increase of gap height can lead to stronger gap overflow and shaft-induced horseshoe vortex, which are source of the high heat flux around the fin. The case with the highest mounting gap (4 mm) en-counters the most severe aerodynamic heating, both on the surface of fin and plate. Thus, under the premise of ensuring the flexibility of the fin, the gap should be set as small as possible.     

日照边缘区域电离层对耀斑的响应特点研究

利用MSIS模型和背景太阳辐射谱模型,在一定大耀斑辐射谱假设的前提下,计算了耀斑期间日照边缘区域的电子产生率,分析了这一区域电离层电子密度的变化特点.结果表明,大耀斑期间在日照边缘区域,甚至大于太阳天顶角90°的区域都有明显的电子产生率的增加.从不同太阳天顶角处的电子产生率剖面的形态来看,随着天顶角的增加最大电离率减少,但高度增加.计算还显示了在太阳天顶角小于90°的区域内电子产生率的垂直分布有明显的双峰结构,这种结构对应着电离层的E区和F区,但在天顶角大于90°区域,F区的电子产生率要大得多.考虑到离子和电子的复合过程,这一区域的总电子含量的增加主要产生在高F区.      

氢氧内燃机增氧定容燃烧特性研究

航天器携带推进剂有限,氢氧内燃机适宜采用纯氢纯氧+富氢燃烧方式,但目前内燃机纯氢纯氧燃烧缺乏地面试验验证。为此开展氢氧内燃机增氧定容燃烧试验,采用内燃机定容燃烧逐步增氧的技术路线,获得增氧乃至纯氧条件下氢氧内燃机的层流燃烧特性,实现氢氧内燃机高性能高可靠工作。试验结果表明：随着氧气浓度的增大,层流燃烧速度随当量比成倍增加,变化的幅度会逐渐减小;高氧气浓度条件下,层流燃烧速度维持在很高的水平,且随当量比的变化很小。     

无人机电静液起落架收放及刹车系统仿真研究

无人机起落架收放及刹车系统在无人机的起飞、降落和刹车的过程中发挥着至关重要的作用,随着无人机飞行条件和要求的日益严苛,传统的液压系统已经无法满足需要。电静液系统既保留了传统液压系统的优点,又兼备电作动的优势。根据电静液作动器的工作原理,设计一款无人机起落架收放和刹车功能一体化的电静液系统,将改进型的PID 控制方式运用到起落架收放的控制中,并且设计两种模糊PID 控制方式运用于防滑刹车功能中,在此基础上进行基于AMESim 和MATLAB/Simulink 的联合仿真用于验证系统性能,并对仿真结果进行对比分析。结果表明：模糊PID 的控制方式控制效果良好,可以有效地改善无人机起落架收放和刹车过程的稳定性,使得起落架收放更安全,刹车效率更高。     

面向机载综合监视系统的ADS-B技术综述

广播式自动相关监视（ADS-B）作为机载综合监视系统（ISS）的新增重要组成部分,在保证飞机飞行安全的前提下,在监视成本和效率方面展现出优势,引领了未来监视技术的发展。本文首先介绍了ADS-B系统功能与优劣势,梳理了国内外技术和产品现状;然后从保障飞行安全和高效的角度出发,分析和综述了机载ISS中ADS-B的关键技术,并详细阐述了技术内涵及难点;最后结合下一代空域运行理念,探讨和展望了技术发展趋势,提出了4个ADS-B技术的未来发展方向,为推动ADS-B技术在实际运行与理论研究方面的发展提供参考。     

飞行管理系统下降路径构建及应用研究

在飞行管理系统下降设计中，通过下降路径的构建可为接近目的机场提供一个垂直轨迹，使飞机遵守终端区各种限制要求，从而精确控制下降路径，满足安全性要求。本文分析了下降路径的定义及其在典型机型中的构建方法，给出了下降路径的描述方法及实现途径，并对具体机型中的应用做了简要介绍。     

高速BPSK相干光通信系统对激光器线宽要求

文章概述了激光器相位噪声对零差相干检测光通信系统性能的影响，对特定的基于平衡探测的科斯塔斯（Costas）环路接收系统相位误差进行了详细的理论分析，最后获得了不同传输码速率下的零差相干检测光通信系统对激光器线宽的具体要求。     

CCSDS在我国航天领域的应用展望

CCSDS(空间数据系统咨询委员会)建议有利于增强测控系统互联互通互支持能力,满足未来航天任务对空间信息高速传输及灵活高效信息调度机制的要求,应当作为我国构建天地一体化信息网络的首选标准。提出了加强顶层设计、循序渐进地推进CCSDS建议在我国实现工程化应用的总体思路,并提出在应用过程中应当注重创新任务操作模式、关注信息安全、深化关键技术研究与验证。     

Variation in the ionospheric propagating factor M(3000)F2 at Ouagadougou,Burkina Faso

We use hourly monthly median values of propagation factor M(3000)F2 data observed at Ouagadougou Ionospheric Observatory (geographic12.4°N, 1.5°W; 5.9^o dip), Burkina Faso (West Africa) during the years Januar1987–December1988 (average F10.7 < 130 × 10⁻²² W/m²/Hz, representative of low solar flux conditions) and for January 1989–December1990 (average F10.7 ? 130 × 10⁻²² W/m²/Hz, representative of high solar epoch) for magnetically quiet conditions to describe local time, seasonal and solar cycle variations of equatorial ionospheric propagation factor M(3000)F2 in the African region. We show that that seasonal trend between solar maximum and solar minimum curves display simple patterns for all seasons and exhibits reasonable disparity with root mean square error (RMSE) of about 0.31, 0.29 and 0.26 for December solstice, June solstice and equinox, respectively. Variability Σ defined by the percentage ratio of the absolute standard deviation to the mean indicates significant dissimilarity for the two solar flux levels. Solar maximum day (10–14 LT) and night (22–02 LT) values show considerable variations than the solar minimum day and night values. We compare our observations with those of the IRI 2007 to validate the prediction capacity of the empirical model. We find that the IRI model tends to underestimate and overestimate the observed values of M(3000)F2, in particular, during June solstice season. There are large discrepancies, mainly during high solar flux equinox and December solstice between dawn and local midnight. On the other hand, IRI provides a slightly better predictions for M(3000)F2 between 0900 and 1500 LT during equinox low and high solar activity and equinox high sunspot number. Our data are of great importance in the area of short-wave telecommunication and ionospheric modeling.