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.     

涡轮叶片尾缘凹坑/凸起结构气膜冷却特性研究

为探究吸力面凹坑和凸起结构对涡轮叶片尾缘气膜冷却特性的影响,在吹风比M=1.1时(雷诺数Re=2.5×10~5),采用数值模拟方法,通过在叶片尾缘吸力面上加入凹坑或凸起,对涡轮叶片尾缘的冷却性能和流动机理进行了详细分析。结果表明:与原始结构相比,叶片尾缘凹坑和凸起结构提高了劈缝出口下游远距离端X/H6 (H为劈缝宽度,为4.8mm)区域气膜冷却效率,对下游的X/H6区域气膜冷却效率影响较小;三种叶片尾缘结构,沿着流向方向会产生由二维展向涡到发卡涡,再到流向涡的变化过程,凹坑和凸起结构通过抑制流体的扰动,改变流体流动情况,提高了劈缝出口下游远距离端气膜冷却效率。     

某型发动机低压压气机导叶角度偏关故障分析与排除

针对某型发动机低压压气机导流叶片角度低于标准值即偏关的故障,详细分析了故障现象,阐述了低压压气机导流叶片调节通道工作原理及控制计划,剖析故障机理。根据所制定的排故流程,提出并分析了可能引发该故障的综合电子调节器、电路、传感器故障模式,最终确定综合电子调节器故障导致低压压气机导流叶片角度低于标准值。更换综合电子调节器,进行外场试车验证。结果表明:发动机工作参数正常,推力稳定,低压压气机导流叶片角度符合要求。     

一种铝锂合金搅拌摩擦焊接头力学性能及微观组织研究

研究了C24S-T8铝锂合金搅拌摩擦焊接头力学性能及微观组织。通过焊接工艺参数的优化,获得了无孔洞缺陷、焊缝质量优异的接头,强度系数约82%。拉伸时塑性变形及断裂集中于焊缝处。基材晶粒呈薄饼状,沿轧制方向拉长;焊核区为细小等轴的再结晶晶粒,平均晶粒尺寸约2.3μm,大部分晶界是大于15°的大角度晶界;热机影响区的晶粒在焊接过程中发生了偏转和变形。C24S-T8铝锂合金基材强化相包括T1相(Al2CuLi)、θ’相(Al2Cu)和S’相(Al2CuMg);热机影响区及焊核区内强化相完全溶解,造成硬度下降。     

折叠翼飞机的气动特性分析

常规飞机具有单一的最优性能,折叠翼飞机通过改变机翼的折叠角度来改变飞机的气动性能,从而能够更好地完成多种任务。对折叠翼飞机进行建模并运用计算流体力学软件进行数值计算,根据计算结果分析折叠翼飞机的气动性能。结果表明：机翼折叠角度的改变,对飞机的失速迎角、俯冲性能、副翼操纵响应和纵横向操稳特性等产生很大影响;飞机失速迎角在机翼折叠后变大,飞机机翼折叠后飞机俯冲更迅速。     

一种乘波前体进气道的一体化设计及性能分析

采用特征线方法设计了具有直线初始激波、内收缩段消除激波反射、出口参数均匀可控的基准内锥流场.基于密切内锥(osculating inward turning cone,OIC)乘波体设计方法,发展了一体化密切内锥乘波前体进气道(osculating inward turning cone waverider inlet,OICWI)设计技术.基于一体化基准内锥流场和前体进气道设计技术,设计了密切内锥乘波前体进气道.采用数值软件对设计的乘波前体进气道进行了仿真分析,结论如下:①OICWI的设计是遵循气动原理的.②一体化密切内锥乘波前体进气道的前缘形状、内收缩比及出口参数可以根据需求定量准确设计.③理论设计结果和模拟结果吻合一致,证明设计方法是正确可靠的.④数值模拟研究结果表明一体化密切内锥乘波前体进气道具有较好的出口流场均匀度及较高的流量捕获率和较高的总压恢复特性.      

基于MVC架构的航电系统软件研究与应用

针对大规模复杂航电系统软件的设计和开发,引入MVC(模型-视图-控制)的软件体系架构和设计模式,对软件行为主体进行持续抽象和封装,并在项目开发过程中迭代应用。研究结果证明,采用MVC架构很好的提高了软件设计和开发的可靠性、可扩展性和可复用性,增强了应用系统软件架构的灵活性和适应性。     

密切内锥乘波前体进气道一体化设计和性能分析

采用特征线方法设计了具有直线初始激波、内收缩段消除激波反射、出口参数均匀可控的基准内锥流场。基于密切内锥(Osculating Inward turning Cone,OIC)乘波体设计方法,发展了密切内锥乘波前体进气道(Os-culating Inward turning Cone Waverider Inlet,OICWI)一体化设计技术。基于基准内锥流场和前体进气道一体化设计技术,设计了密切内锥乘波前体进气道。采用数值方法对设计的密切内锥乘波前体进气道进行了计算分析,结果表明无粘流场结构和基准内锥流场吻合,无粘模拟结果和理论设计结果吻合。粘性数值模拟结果显示一体化进气道具有较高的流量捕获率及总压恢复特性,进气道出口流场分布均匀。     

碳纤维表面微观结构的定量化表征方法

通过使用Matlab编程处理日本东丽T300、国产GCF-1和GCF-2等3种碳纤维样品断面的扫描电镜照片,采用二值标签算法获得了碳纤维的直径及圆度等碳纤维物理特征定量数据。建立了采用直线方程切线法寻找并计算碳纤维表面沟槽的数量及尺度的方法,发现3种碳纤维样品的边缘沟槽的深度及宽度的分布均符合Weibull分布的特征。3种碳纤维的表面物理特征随温度变化的规律相同,说明其在结构上存在着一致性。经过不同温度热处理后3种碳纤维样品的圆度值变化不大,平均直径随着热处理温度的升高逐渐减小,并且表面沟槽的数量及分布的变化规律相同,说明其结构存在一致性。3种碳纤维的圆度等表面物理特征存在一定差异,T300的圆度小于国产GCF-1及GCF-2碳纤维。     

带扰流柱内冷通道对表面气膜冷却特性的影响

为了讨论内冷通道结构对表面气膜冷却特性的影响,通过数值模拟的方法,计算研究不同结构下,冷气流过带有扰流柱内冷通道对表面气膜冷却特性的影响,并研究冷气通道与燃气掺混后的冷却效果;采用六种不同结构的扰流柱与气膜孔排列方式,计算中吹风比的范围为0．1〈M〈2．0。结果表明：冷气通道内的扰流柱对进入气膜孔的冷气起到稳定作用,比冷气通道内不加扰流柱的气膜冷却效果好,而且扰流柱与气膜孔不同的排列方式对气膜冷却效果有显著影响,因此选择合适的排列方式有利于气膜冷却。