束丝SiC纤维增强铝复合材料界面TEM研究

利用透射电镜 (TEM )对由几种不同方法制备的束丝SiC纤维增强铝复合材料 (包括超声液相浸渗法制备的复合丝、由复合丝热压得到的板材以及由真空液相压渗法制备的板材等 )的界面微观特征进行了研究 ,结果显示 ,制造态及 5 5 0℃× 1h热暴露条件下复合材料没有发生界面反应 ,在 6 5 0℃× 1h热暴露条件下有厚度 10 0～2 0 0nm的界面反应区。该研究表明 ,SiC/Al复合材料在制备工艺条件下具有有良好的界面化学相容性     

缩尺模拟板相关性研究

介绍了模拟板由小模型到大模型的研制过程，着重讨论了模拟板小模型与大模型在流场总压恢复系数、周向不均匀度、低压区范围等方面的相关性问题。研究结果表明由小模型到大模型的研制方案是正确可行的。     

超音尾喷流红外抑制方案的研究

超音速发动机尾喷流的红外抑制是超音速飞行器隐身性能的重要组成部分。本文提出两种超音速尾喷流的红外抑制方案二次旋流方案与组合波瓣方案 ,并对两种方案共 7组试验件在不同的结构和二次流速度情况下进行了大量重复试验。在旋流方案试验中 ,对二次流加旋诱发大尺度流向涡进行了系统的研究 ,得到旋流角度、二次流速度等对掺混效果的影响规律 ,试验结果表明 :对于本结构方案 ,当二次流速度为 49m/s,旋流角在 3 0°左右 ,掺混效果最好 ,且随二次流流速的增加而加强。在组合波瓣方案的试验中 ,对组合波瓣用于超音尾喷流红外抑制进行了研究 ,试验结果表明可对超音尾喷流的红外起到有效的抑制作用。     

The Cassini Visual And Infrared Mapping Spectrometer (Vims) Investigation

The Cassini visual and infrared mapping spectrometer (VIMS) investigation is a multidisciplinary study of the Saturnian system. Visual and near-infrared imaging spectroscopy and high-speed spectrophotometry are the observational techniques. The scope of the investigation includes the rings, the surfaces of the icy satellites and Titan, and the atmospheres of Saturn and Titan. In this paper, we will elucidate the major scientific and measurement goals of the investigation, the major characteristics of the Cassini VIMS instrument, the instrument calibration, and operation, and the results of the recent Cassini flybys of Venus and the Earth–Moon system.This revised version was published online in July 2005 with a corrected cover date.     

Polar format algorithm for bistatic SAR

Matched filtering (MF) of phase history data is a mathematically ideal but computationally expensive approach to bistatic synthetic aperture radar (SAR) image formation. Fast backprojection algorithms (BPAs) for image formation have recently been shown to give improved O(N/sup 2/ log/sub 2/N) performance. An O(N/sup 2/ log/sub 2/N) bistatic polar format algorithm (PFA) based on a bistatic far-field assumption is derived. This algorithm is a generalization of the popular PFA for monostatic SAR image formation and is highly amenable to implementation with existing monostatic image formation processors. Limits on the size of an imaged scene, analogous to those in monostatic systems, are derived for the bistatic PFA.     

The Time-of-Flight Energy,Angle, Mass Spectrograph (Teams) Experiment for Fast

The Time-of-flight Energy Angle Mass Spectrograph (TEAMS) is being flown on the FAST Small Explorer mission to measure the 3-dimensional distribution function of the major ion species present in the lower magnetosphere. The instrument is similar to time-of-flight plasma analyzer systems that have been designed and planned for flight as CODIF (COmposition and DIstribution Function analyzer) on the four European Space Agency Cluster-II spacecraft and, as ESIC (Equator-S Ion Composition instrument) on Equator-S. This instrument allows the 3-dimensional distribution functions of individual ion species to be determined within spin period (2.5 s). Two-dimensional distributions are measured in 80 ms. These capabilities are crucial for the study of selective energization processes in the auroral regions of the magnetosphere. The design, operational characteristics, and test and calibration results for this instrument are presented. The sensor consists of a toroidal top-hat electrostatic analyzer with instantaneous acceptance of ions over 360° in polar angle. After post-acceleration of the incoming ions by up to 25 kV, a time-of-flight mass spectrograph discriminates the individual species. It has been demonstrated through calibration that the instrument can easily separate H⁺, He²⁺, He⁺, O⁺ and, for energies after post-acceleration of > 20 keV, even O₂ ⁺ molecules. On-board mass discrimination and the internal accumulation of several distinct data quantities combined with the spacecraft's flexible telemetry formatting allow for instrument data rates from 7.8 kb s^–1 to 315 kb s^–1 to be telemetered to ground through the FAST centralized Instrument Data Processor.     

Rigidity Dependence and Time Response of Cosmic Rays to the Modulation Steps in the Rising Part of Solar Cycle 23. Cospin/ket Results

Previous work on the latitudinal gradient and on the amplitude of the recurrent cosmic ray decreases, has shown that their magnitude does not decrease monotonically with the particle rigidity, but it presents a broad maximun around 1–2 GV. We have extended this analysis to study the behaviour of cosmic-ray particles during the modulation steps in the rising part of the solar activity of the present Solar cycle. We found that the ‘depth’ of the modulation step decreases monotonically with increasing rigidity and that the least energetic particles are the last to reach their minimum intensity value. We also considered in this analysis electrons of equal rigidity to study the influence of the charge sign on the particle behaviour during the modulation steps. This revised version was published online in August 2006 with corrections to the Cover Date.     

Ring Currents and Internal Plasma Sources

The discovery of terrestrial O⁺ and other heavy ions in magnetospheric hot plasmas, combined with the association of energetic ionospheric outflows with geomagnetic activity, led to the conclusion that increasing geomagnetic activity is responsible for filling the magnetosphere with ionospheric plasma. Recently it has been discovered that a major source of ionospheric heavy ion plasma outflow is responsive to the earliest impact of coronal mass ejecta upon the dayside ionosphere. Thus a large increase in ionospheric outflows begins promptly during the initial phase of geomagnetic storms, and is already present during the main phase development of such storms. We hypothesize that enhancement of the internal source of plasma actually supports the transition from substorm enhancements of aurora to storm-time ring current development in the inner magnetosphere. Other planets known to have ring current-like plasmas also have substantial internal sources of plasma, notably Jupiter and Saturn. One planet having a small magnetosphere, but very little internal source of plasma, is Mercury. Observations suggest that Mercury has substorms, but are ambiguous with regard to the possibility of magnetic storms of the planet. The Messenger mission to Mercury should provide an interesting test of our hypothesis. Mercury should support at most a modest ring current if its internal plasma source is as small as is currently believed. If substantiated, this hypothesis would support a general conclusion that the magnetospheric inflationary response is a characteristic of magnetospheres with substantial internal plasma sources. We quantitatively define this hypothesis and pose it as a problem in comparative magnetospheres.     

应用于小发柔性转子的高速动平衡技术

从某新型涡轴发动机动力涡轮转子的结构特点出发 ,简要说明了对该转子进行实际高速动平衡操作存在的困难及采取的对策。在试验过程中 ,创造性地应用影响系数法和自行设计加工的精密平衡卡箍 ,高质量地完成了细长柔性转子的高速动平衡试验。研究表明 :高速动平衡技术可大大减小细长柔性转子的动挠度和支承动反力 ,从而达到减小发动机振动的目的     

细观力学有限元法预测复合材料宏观有效弹性模量

基于能量等效原理提出了复合材料有效弹性模量的定义，并指出了该定义的基础及前提条件。为从理论上计算复合材料宏观有效弹性模量，建立了通过细观力学有限元法计算复合材料有效弹性模量的方法。复合材料宏观弹性模量，是通过对复合材料细观结构代表性体积元的力学响应的计算来得到，在该计算方法中，给出了施加简便的边界载荷以及恰当的边界变形约束条件的方法。数值计算结果与部分试验结果具有较好的一致性，表明所提出的方法能够较好地计算复合材料的宏观有效弹性模量。