AZ91镁合金搅拌摩擦加工后的组织与性能

采用400rpm-100mm/min,800rpm-100mm/min,800rpm-200mm/min三种工艺参数对铸态AZ91镁合金进行搅拌摩擦加工(FSP)处理,并对合金加工前后的显微组织和拉伸性能及微观断裂机制进行分析。结果表明,经800rpm-100mm/min工艺FSP处理后,合金的显微组织明显细化,延伸率和抗拉强度显著提高,综合拉伸性能最好,且拉伸断口主要表现为韧性断裂的特征。这主要是由于在FSP过程中合金发生动态再结晶,使合金晶粒显著细化及粗大β相的溶解和破碎所致。     

无人作战飞机自主控制分级递阶控制结构

把智能控制领域的分级递阶控制结构应用于无人作战飞机(UAV)自主控制的结构设计,根据"精度随智能降低而提高(IPDI)"的原则,把该控制系统分为3个层次:执行级、协调级和组织级。执行级完成高精度的局部控制任务;协调级产生航迹及导航信号,并对子系统的工作进行协调;组织级提供决策支持。提出了通过内外回路的方法来实现整个控制系统的硬件。根据每一级的功能需求,提炼出在多任务模式下各级的关键技术,进行了模块化分解,并分析了它们之间的逻辑关系。重点阐述了协调级和组织级的约束条件及实现过程。     

航空发动机燃烧室主燃区的数值模拟分析

概述了先进燃烧室的主燃区数值模拟,论述了采用气动喷嘴时确定边界条件的方法和模拟燃油喷嘴油滴轨迹的结果。对某型发动机燃烧室的主燃区进行了数值模拟,给出了熄火时主燃区流场,分析了主燃区温场对出口温场的影响     

涡轮叶片叶冠的预扭设计分析

对在工作状态下的某型航空发动机叶冠不同预扭角的低压涡轮叶片应力进行了计算分析,给出了装配状态下叶冠阻尼面应力状态的计算分析方法。     

精密球新型研磨方式的仿真研究

在精密球偏心V形槽研磨方式的基础上,提出一种新的研磨方式。运动分析结果表明,与偏心V形槽和传统V形槽研磨方式不同,该研磨方式下球坯的自转轴能够在180°范围内摆动,使研磨轨迹在球坯表面的分布更为均匀。通过仿真计算发现,在该研磨方式下偏心距对球坯表面研磨均匀性影响较小,并且,各槽内球坯所受研磨均匀性相同。     

基于非结构动网格的非定常气动力计算

对用于非结构动网格生成的弹簧近似方法进行了研究。通过采用顶点弹簧方法,分析研究了弹簧倔强系数的取值,同时通过引入挤压倔强系数和边界修正,对标准弹簧近似方法进行了改进。改进后的方法可以大大提高网格变形能力和网格质量。应用本文发展的非结构动网格生成方法耦合求解基于Arbitrary Lagrangian-Eulerian(ALE)描述的欧拉方程,计算了谐和振动NACA0012翼型及矩形机翼的跨声速非定常气动力,计算结果与参考文献提供的结果及实验结果吻合良好。     

电控旋翼直升机配平及操纵特点分析

对采用电控旋翼直升机的配平及操纵特性进行了研究。首先根据电控旋翼的刚体桨叶变距运动方程，推导了襟翼操纵量与桨叶桨距的显式关系式。以此为基础，建立了电控旋翼直升机的飞行动力学模型。以WZ-1直升机为样例直升机，对比分析了电控旋翼直升机与常规直升机的配平特性和操纵响应特性。结果表明，电控旋翼直升机具有与常规直升机类似的配平和操纵特性，桨叶预安装角和桨根扭簧刚度这两个参数对其影响显著。     

Diffusive Shock Acceleration and Magnetic Field Amplification

Diffusive shock acceleration is the theory of particle acceleration through multiple shock crossings. In order for this process to proceed at a rate that can be reconciled with observations of high-energy electrons in the vicinity of the shock, and for cosmic rays protons to be accelerated to energies up to observed galactic values, significant magnetic field amplification is required. In this review we will discuss various theories on how magnetic field amplification can proceed in the presence of a cosmic ray population. On both short and long length scales, cosmic ray streaming can induce instabilities that act to amplify the magnetic field. Developments in this area that have occurred over the past decade are the main focus of this paper.     

如何为《飞机工程》撰写符合规范又有创新的论文

介绍了科技论文规范表达对收集、储存、处理、加工、检索、利用、交流和传播的作用，结合《飞机工程》投稿的实际，指出了作者在文字、标点、符号、图表、公式、量和单位表达中容易忽视和写错的一些技术细节，给出了科技论文规范表达的撰写格式，以及为《飞机工程》投稿时应注意的事项。     

Imaging Plasma Density Structures in the Soft X-Rays Generated by Solar Wind Charge Exchange with Neutrals

Both heliophysics and planetary physics seek to understand the complex nature of the solar wind’s interaction with solar system obstacles like Earth’s magnetosphere, the ionospheres of Venus and Mars, and comets. Studies with this objective are frequently conducted with the help of single or multipoint in situ electromagnetic field and particle observations, guided by the predictions of both local and global numerical simulations, and placed in context by observations from far and extreme ultraviolet (FUV, EUV), hard X-ray, and energetic neutral atom imagers (ENA). Each proposed interaction mechanism (e.g., steady or transient magnetic reconnection, local or global magnetic reconnection, ion pick-up, or the Kelvin-Helmholtz instability) generates diagnostic plasma density structures. The significance of each mechanism to the overall interaction (as measured in terms of atmospheric/ionospheric loss at comets, Venus, and Mars or global magnetospheric/ionospheric convection at Earth) remains to be determined but can be evaluated on the basis of how often the density signatures that it generates are observed as a function of solar wind conditions. This paper reviews efforts to image the diagnostic plasma density structures in the soft (low energy, 0.1–2.0 keV) X-rays produced when high charge state solar wind ions exchange electrons with the exospheric neutrals surrounding solar system obstacles.The introduction notes that theory, local, and global simulations predict the characteristics of plasma boundaries such the bow shock and magnetopause (including location, density gradient, and motion) and regions such as the magnetosheath (including density and width) as a function of location, solar wind conditions, and the particular mechanism operating. In situ measurements confirm the existence of time- and spatial-dependent plasma density structures like the bow shock, magnetosheath, and magnetopause/ionopause at Venus, Mars, comets, and the Earth. However, in situ measurements rarely suffice to determine the global extent of these density structures or their global variation as a function of solar wind conditions, except in the form of empirical studies based on observations from many different times and solar wind conditions. Remote sensing observations provide global information about auroral ovals (FUV and hard X-ray), the terrestrial plasmasphere (EUV), and the terrestrial ring current (ENA). ENA instruments with low energy thresholds (\(\sim1~\mbox{keV}\)) have recently been used to obtain important information concerning the magnetosheaths of Venus, Mars, and the Earth. Recent technological developments make these magnetosheaths valuable potential targets for high-cadence wide-field-of-view soft X-ray imagers.Section 2 describes proposed dayside interaction mechanisms, including reconnection, the Kelvin-Helmholtz instability, and other processes in greater detail with an emphasis on the plasma density structures that they generate. It focuses upon the questions that remain as yet unanswered, such as the significance of each proposed interaction mode, which can be determined from its occurrence pattern as a function of location and solar wind conditions. Section 3 outlines the physics underlying the charge exchange generation of soft X-rays. Section 4 lists the background sources (helium focusing cone, planetary, and cosmic) of soft X-rays from which the charge exchange emissions generated by solar wind exchange must be distinguished. With the help of simulations employing state-of-the-art magnetohydrodynamic models for the solar wind-magnetosphere interaction, models for Earth’s exosphere, and knowledge concerning these background emissions, Sect. 5 demonstrates that boundaries and regions such as the bow shock, magnetosheath, magnetopause, and cusps can readily be identified in images of charge exchange emissions. Section 6 reviews observations by (generally narrow) field of view (FOV) astrophysical telescopes that confirm the presence of these emissions at the intensities predicted by the simulations. Section 7 describes the design of a notional wide FOV “lobster-eye” telescope capable of imaging the global interactions and shows how it might be used to extract information concerning the global interaction of the solar wind with solar system obstacles. The conclusion outlines prospects for missions employing such wide FOV imagers.