Global Response of Martian Plasma Environment to an Interplanetary Structure: From Ena and Plasma Observations at Mars

As a part of the global plasma environment study of Mars and its response to the solar wind, we have analyzed a peculiar case of the subsolar energetic neutral atom (ENA) jet observed on June 7, 2004 by the Neutral Particle Detector (NPD) on board the Mars Express satellite. The “subsolar ENA jet” is generated by the interaction between the solar wind and the Martian exosphere, and is one of the most intense sources of ENA flux observed in the vicinity of Mars. On June 7, 2004 (orbit 485 of Mars Express), the NPD observed a very intense subsolar ENA jet, which then abruptly decreased within ∼10 sec followed by quasi-periodic (∼1 min) flux variations. Simultaneously, the plasma sensors detected a solar wind structure, which was most likely an interplanetary shock surface. The abrupt decrease of the ENA flux and the quasi-periodic flux variations can be understood in the framework of the global response of the Martian plasma obstacle to the interplanetary shock. The generation region of the subsolar ENA jet was pushed towards the planet by the interplanetary shock; and therefore, Mars Express went out of the ENA jet region. Associated global vibrations of the Martian plasma obstacle may have been the cause of the quasi-periodic flux variations of the ENA flux at the spacecraft location.     

跨音速压气机中的涡结构与失速机理分析

将一种新的涡识别方法应用于压气机流场的分析.该方法采用应变率张量和旋转张量的第四不变量,具有在识别流场中涡的存在的同时,分析该处涡处于拉伸(生成)或松弛(溃灭)状态的能力.通过将该方法与传统的动压头和流线、速度矢量等分析方法的结合,本文对所研究的跨音速压气机的失速过程进行了分析和讨论.     

基于Hamilton-Jacobi方程的编队飞行控制

 针对椭圆参考轨道的编队飞行控制系统,基于哈密尔顿 雅克比（Hamilton-Jacobi）方程,给出一种新的生成函数半解析近似解的计算方法,同时推导了编队飞行控制系统相对运动的线性状态转移矩阵,并且验证了模型的精度。在此基础上,结合一个具体的编队飞行任务,采用线性规划算法得到了队形保持的闭环控制器,该算法得到的是脉冲形式的控制序列,因此更具有实际意义。同时还提出了一种简单的避免生成函数奇异点的方法,从而减少了生成函数间相互转换所带来的计算量。最后的非线性仿真结果验证了控制方法的有效性。     

Coronal Observations of CMEs

CMEs have been observed for over 30 years with a wide variety of instruments. It is now possible to derive detailed and quantitative information on CME morphology, velocity, acceleration and mass. Flares associated with CMEs are observed in X-rays, and several different radio signatures are also seen. Optical and UV spectra of CMEs both on the disk and at the limb provide velocities along the line of sight and diagnostics for temperature, density and composition. From the vast quantity of data we attempt to synthesize the current state of knowledge of the properties of CMEs, along with some specific observed characteristics that illuminate the physical processes occurring during CME eruption. These include the common three-part structures of CMEs, which is generally attributed to compressed material at the leading edge, a low-density magnetic bubble and dense prominence gas. Signatures of shock waves are seen, but the location of these shocks relative to the other structures and the occurrence rate at the heights where Solar Energetic Particles are produced remains controversial. The relationships among CMEs, Moreton waves, EIT waves, and EUV dimming are also cloudy. The close connection between CMEs and flares suggests that magnetic reconnection plays an important role in CME eruption and evolution. We discuss the evidence for reconnection in current sheets from white-light, X-ray, radio and UV observations. Finally, we summarize the requirements for future instrumentation that might answer the outstanding questions and the opportunities that new space-based and ground-based observatories will provide in the future.     

NEPE推进剂力学性能与化学安定性关联老化行为及机理

为了剖析NEPE推进剂力学性能老化特性,研究了其力学性能与化学安定性关联老化行为及其机理。力学性能与化学安定性对比以及正交试验结果表明:两者的老化行为存在关联性,且呈“两段式”。通过理化参数与化学安定性对比以及高效液相色谱测试,阐明了关联老化行为的内在机理是:安定剂不断与硝酸酯分解出的氮氧化物反应生成亚硝基产物,抑制硝酸酯的自催化分解,安定剂通过对硝酸酯分解产物的稳定作用而间接地对粘合剂母体起到了稳定作用,从而形成了NEPE推进剂特有的力学性能与化学安定性老化“两段式”关联行为。     

全站仪检测数据管理系统

介绍了全站仪检测数据管理系统。本系统以FoxPro for Windows为基础,采用模块结构,具有对检测数据录入修改,自动转换,成果计算,查询显示等功能,实现了系统数据管理和处理的一体化。     

耐高温有机无机杂化聚酰亚胺树脂及其复合材料

文摘综述了近年来国内外在有机无机杂化聚酰亚胺树脂及其复合材料方面的研究进展,重点介绍了含笼状倍半硅氧烷和硅氧烷结构的有机无机杂化聚酰亚胺树脂的制备方法,对树脂的分子结构与其耐热性和热氧化稳定性之间的关系进行了分析总结,并对有机无机杂化聚酰亚胺树脂及其复合材料的应用和未来发展进行了探讨。     

倾转旋翼机冗余操纵的舵面分配策略和飞行转换路径分析

倾转旋翼机的不同舵面存在冗余操纵,而冗余舵面的分配策略和飞行转换路径对其控制重构具有重要的意义。对建立的小型无人倾转旋翼机全量非线性飞行动力学模型在不同飞行模式下的进行配平计算、模型线化后,求出单位操纵面位移所引起的俯仰、滚转和偏航力矩的改变量,即考察倾转旋翼机各操纵面的操纵功效,并对其结果进行详细分析,以确定倾转旋翼机的冗余舵面控制重构能力;确定各飞行模式下倾转旋翼机的操纵方式,给出舵面分配策略的权重系数矩阵;在此基础上,提出三种不同的全模式飞行转换路径方案,并分别计算三种方案下倾转旋翼机的飞行速度与前倾角、姿态角及操纵量的关系。结果表明:三种方案都能实现对飞行器的合理操纵,表明倾转旋翼机的冗余舵面控制重构是可以实现的。     

基于型面节点的复合材料构件模具型面修正研究

针对复合材料在热压罐中固化变形造成的零件尺寸误差、带应力装配、降低疲劳寿命等长期困扰航空、航天工业的问题,研究复合材料固化变形的影响因素、作用机理等,并利用基准点的位置坐标,实现两曲面间的匹配,提出变形修正的算法和切实可行的修正手段,从而在模具设计时对模具型面做相应的补偿,减少试模、修模次数,实现复合材料固化变形的有效控制,达到复合材料精准制造的目的。     

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.