加油机尾流场建模与仿真分析

提出了等效气动效应法,建立了加油机尾流场的等效扰动模型。等效气动效应法采用逐点积分方法和加权平均方法,将尾流的影响等效为受油机运动方程直接可用的平均风速度和风梯度。对不同状态下受油机所受尾流的扰动作用进行了仿真。结果表明,扰动模型与实际情况比较符合。     

The Genesis Solar Wind Concentrator Target: Mass Fractionation Characterised by Neon Isotopes

The concentrator on Genesis provided samples of increased fluences of solar wind ions for precise determination of the oxygen isotopic composition. The concentration process caused mass fractionation as a function of the radial target position. This fractionation was measured using Ne released by UV laser ablation and compared with modelled Ne data, obtained from ion-trajectory simulations. Measured data show that the concentrator performed as expected and indicate a radially symmetric concentration process. Measured concentration factors are up to ∼30 at the target centre. The total range of isotopic fractionation along the target radius is 3.8%/amu, with monotonically decreasing ²⁰Ne/²²Ne towards the centre, which differs from model predictions. We discuss potential reasons and propose future attempts to overcome these disagreements.     

Galactic Wind: Mass Fractionation and Cosmic Ray Acceleration

The dynamical and chemical effects of the Galactic Wind are discussed. This wind is primarily driven by the pressure gradient of the Cosmic Rays. Assuming the latter to be accelerated in the Supernova Remnants of the disk which at the same time produce the Hot Interstellar Medium, it is argued that the gas removed by the wind is enriched in the nucleosynthesis products of Supernova explosions. Therefore the moderate mass loss through this wind should still be able to remove a substantial amount of metals, opening the way for stars to produce more metals than observed in the disk, by e.g. assuming a Salpeter-type stellar initial mass function beyond a few Solar masses. The wind also allows a global, physically appealing interpretation of Cosmic Ray propagation and escape from the Galaxy. In addition the spiral structure of the disk induces periodic pressure waves in the expanding wind that become a sawtooth shock wave train at large distances which can re-accelerate “knee” particles coming from the disk sources. This new Galactic Cosmic Ray component can reach energies of a few×10¹⁸ eV and may contribute to the juncture between the particles of Galactic and extragalactic origin in the observed overall Cosmic Ray spectrum.     

The Origin of Mercury’s Internal Magnetic Field

Mariner 10 measurements proved the existence of a large-scale internal magnetic field on Mercury. The observed field amplitude, however, is too weak to be compatible with typical convective planetary dynamos. The Lorentz force based on an extrapolation of Mariner 10 data to the dynamo region is 10⁻⁴ times smaller than the Coriolis force. This is at odds with the idea that planetary dynamos are thought to work in the so-called magnetostrophic regime, where Coriolis force and Lorentz force should be of comparable magnitude. Recent convective dynamo simulations reviewed here seem to resolve this caveat. We show that the available convective power indeed suffices to drive a magnetostrophic dynamo even when the heat flow though Mercury’s core–mantle boundary is subadiabatic, as suggested by thermal evolution models. Two possible causes are analyzed that could explain why the observations do not reflect a stronger internal field. First, toroidal magnetic fields can be strong but are confined to the conductive core, and second, the observations do not resolve potentially strong small-scale contributions. We review different dynamo simulations that promote either or both effects by (1) strongly driving convection, (2) assuming a particularly small inner core, or (3) assuming a very large inner core. These models still fall somewhat short of explaining the low amplitude of Mariner 10 observations, but the incorporation of an additional effect helps to reach this goal: The subadiabatic heat flow through Mercury’s core–mantle boundary may cause the outer part of the core to be stably stratified, which would largely exclude convective motions in this region. The magnetic field, which is small scale, strong, and very time dependent in the lower convective part of the core, must diffuse through the stagnant layer. Here, the electromagnetic skin effect filters out the more rapidly varying high-order contributions and mainly leaves behind the weaker and slower varying dipole and quadrupole components (Christensen in Nature 444:1056–1058, 2006). Messenger and BepiColombo data will allow us to discriminate between the various models in terms of the magnetic fields spatial structure, its degree of axisymmetry, and its secular variation.     

柔性-刚性混合翼微型飞行器气动特性研究

提出了一种将柔性翼和刚性翼相结合的柔性-刚性混合翼微型飞行器新概念布局型式，通过与刚性翼微型飞行器的风洞对比试验研究了该新概念布局的气动特性。在此基础上，进行了柔性-刚性混合翼微型飞行器试验原理样机的飞行试验验证。风洞试验和飞行试验研究结果表明：柔性-刚性混合翼微型飞行器的新概念布局是可行的；与刚性翼微型飞行器相比而言，柔性-刚性混合翼微型飞行器具有更好的气动特性，对解决微型飞行器抗风稳定飞行问题是有效的。     

隐身外形飞行器用埋入式进气道的设计与风洞实验研究

本文为隐身外形飞行器用埋入式进气道发展了一套设计方法。该方法的理论基础是埋入式进气道进气机理和气动S弯概念,其关键技术包含通道中心线设计、横截面面积变化规律设计以及横截面形状设计等,各技术可以方便地用数学方法加以描述,整个方法易于编程实现。并结合一种隐身外形无人机提出了埋入式进气道方案,通过实验得到了此类隐身外形飞行器用埋入式进气道的气动特性。结果表明,所提出的埋入式进气道方案可行,所设计的模型进气道性能良好,所发展的设计方法合理。同时验证了埋入式进气道进气机理的正确性,也表明隐身外形飞行器与埋入式进气道的组合方案具有十分光明的应用前景。     

可重复使用航天器再入段复合控制方法研究

可重复使用航天器再入过程初期,反作用力控制系统是其姿态控制的主要手段,结合气动舵面可以减小飞行器对该系统的总冲需求,提高飞行器动态响应特性。给出了反作用力控制系统与气动舵面复合姿态控制系统的组成及三种复合控制指令分配策略,并进行了仿真计算,分析了三种策略的姿态控制效果及总冲需求。仿真结果表明,三种方法均能完成飞行器姿态控制,并各有其优缺点,研究结果为航天器飞行控制系统控制律设计提供了有效参考。     

扩展分支分析方法在飞行动力学中的应用

将分支分析和突变理论方法扩展后,应用于飞机全包线范围内平衡特性的连续计算和稳定性分析,提出了以扩展分支分析方法为基础的反馈参数连续调参的控制律设计方法。研究结果表明,扩展分支分析方法不仅能获得飞行性能指标,而且可确定非线性飞行动力学系统的稳定特性,是综合进行性能计算、品质分析及控制律设计的一种有效方法。     

基于模拟退火算法与响应面模型的三维气动优化设计方法

提出了一套适用于高耗时三维气动设计问题的优化设计体系.其主要思想是采用改进拉丁超立方体试验设计选取样本点,应用自行开发的三维粘性流场求解程序进行流场计算建立数据库,采用二次响应面方法建立近似模型,再应用高效模拟退火算法进行全局寻优.以NASA rotor57为对象,在详细进行流场计算基础上采用所提出的优化体系对其进行了三维积叠优化设计.在对流量、效率加以严格约束的条件下,总压比可提高1.8%,对流场结构进行了分析.优化结果表明本优化方法省时,适于三维气动设计的特点.     

大振幅实验对常规动导数实验包容性研究

某飞机模型在南京航空航天大学NH-2低速风洞中进行大振幅振动动态试验.模型绕通过重心的机体坐标轴分别作单独俯仰、偏航、滚转的大振幅振动,采用内式应变天平测量模型的非定常空气动力.通过非定常空气动力建模和动导数仿真方法,获得模型的纵横向稳定性导数和交叉导数.仿真结果与常规动导数试验结果比较,两者在量级和规律上一致.分析表明,模型大振幅振动实验结果包含了常规动导数实验的信息,模型的动导数可以从大振幅振动实验结果中获取.