Summary of quantitative interpretation of IMAGE far ultraviolet auroral data

Direct imaging of the magnetosphere by instruments on the IMAGE spacecraft is supplemented by simultaneous observations of the global aurora in three far ultraviolet (FUV) wavelength bands. The purpose of the multi-wavelength imaging is to study the global auroral particle and energy input from the magnetosphere into the atmosphere. This paper describes the method for quantitative interpretation of FUV measurements. The Wide-Band Imaging Camera (WIC) provides broad band ultraviolet images of the aurora with maximum spatial resolution by imaging the nitrogen lines and bands between 140 and 180 nm wavelength. The Spectrographic Imager (SI), a dual wavelength monochromatic instrument, images both Doppler-shifted Lyman-α emissions produced by precipitating protons, in the SI-12 channel and OI 135.6 nm emissions in the SI-13 channel. From the SI-12 Doppler shifted Lyman-α images it is possible to obtain the precipitating proton flux provided assumptions are made regarding the mean energy of the protons. Knowledge of the proton (flux and energy) component allows the calculation of the contribution produced by protons in the WIC and SI-13 instruments. Comparison of the corrected WIC and SI-13 signals provides a measure of the electron mean energy, which can then be used to determine the electron energy flux. To accomplish this, reliable emission modeling and instrument calibrations are required. In-flight calibration using early-type stars was used to validate the pre-flight laboratory calibrations and determine long-term trends in sensitivity. In general, very reasonable agreement is found between in-situ measurements and remote quantitative determinations.     

Heliosphere-Geosphere Interactions Using Low Energy Neutral Atom Imaging

Development of the low energy neutral atom (LENA) imager was originally motivated by a need to remotely sense plasma heating in the topside ionosphere, with the goal of greatly enhanced temporal resolution of an otherwise familiar phenomenon. During ground test and calibration, the LENA imager was found to respond to neutral atoms with energies well above its nominal energy range of 10–750 eV, up to at least 3–4 keV, owing to sputtering interactions with its conversion surface. On orbit, LENA has been found to respond to a ubiquitous neutral atom component of the solar wind, to the neutral atoms formed by magnetosheath interactions with the geocorona during periods of high solar wind pressure, and to the interstellar neutral atoms flowing through the heliosphere during the season of maximal relative wind velocity between spacecraft and interstellar medium. LENA imaging has thus emerged as a promising new tool for studying the interplanetary medium and its interaction with the magnetosphere, in addition to the ionospheric heating and outflow that result from this interaction. LENA emissions from the ionosphere consist of a fast component that can be observed at high altitudes, and slower components that evidently create a quasi-trapped extended superthermal exosphere. The more energetic emissions are responsive to solar wind energy inputs on time scales of a few minutes.     

军机产品贯彻实施AO/FO

工艺规程是指导工人制造产品的重要依据,而装配指令(AO)、制造指令(FO)除规定制造工艺流程外,还集中反映了制造过程的质量与生产管理信息。在将AO/FO与传统工艺规程进行对比的基础上,就我国军机产品在生产过程中如何贯彻实施AO/FO,提高军机生产工艺技术、生产管理和质量控制水平发表了几点看法。     

评定叶片鸟撞击损伤的参数与方法

探讨了在叶片抗岛撞击损伤研究中叶片损伤能力的评定参数与评定方法。结合发动机设计准则与设计规范的要求,提出了2个用于评定叶片损伤能力的叶片变形损伤参数和塑性应变损伤参数;经对模型叶片在不同撞击位置进行的鸟撞击损伤评定,证明方法可行     

叶片包容性计算的软件实现

基于英国和俄罗斯叶片包容性设计方法和理论,应用VB语言开发了叶片包容性计算软件。以某型发动机第1级涡轮叶片为例,用该软件计算了叶片包容性和满足包容性条件下的最小机匣厚度。根据实际要求,也可以用该软件确定满足包容性要求的各设计参数     

用偏微分方程构造车身外形曲面

阐述了在给定边界条件及其他曲面限制因素的情况下,用偏微分方程构造曲面的基本理论;研究了引入曲面形状控制系数来控制生成曲面的形状以及应用于车身外形曲面设计的实现方法,并分析了该方法的特点,最后给出了在车身设计中应用的实例。     

Cf/Al复合材料管件的真空液相成型工艺研究

以高模高强碳纤维M40J(6K)增强铝基复合管为研究对象，研究了真空反压液相浸渗工艺中，纤维束丝分散技术、预制件压缩强度提高技术及碳纤维涂层对管件成型及性能的影响。结果表明：SiCp可以起分散作用，有利于浸渍；加入10％的偏磷酸盐的预制件经680℃真空去胶后的压缩性能满足浸渗要求，纤维保持了较好的平直度且分布均匀。C-Al2O3涂层对复合材料的性能有较大影响，经涂层处理后的预制件所制备出的复合材料的强度比未经涂层处理的提高了13％左右。所制备的复合材料的比强度、比模量较高，密度小于2．5g／cm^3。     

不同组织状态TC4合金靶材损伤行为的研究

采用直径为4mm的CoCr15钢珠作为弹丸对两种不同组织状态的TCA合金进行撞击试验，撞击速度为1．5km／s；观察撞击后不同厚度靶材的宏观损伤及微观损伤行为。结果表明：靶材的组织状态对靶材的宏观损伤行为有很大的影响；时效处理态的组织具有更高的绝热剪切敏感性，在中厚靶发生了绝热冲塞；退火态中厚靶的背面则发生了凸起。各种靶材的微观损伤形式基本相同，在弹坑附近出现了大量的绝热剪切带；微孔洞在绝热剪切带内形核、长大并连结成为裂纹。     

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.     

The Cassini Cosmic Dust Analyzer

The Cassini-Huygens Cosmic Dust Analyzer (CDA) is intended to provide direct observations of dust grains with masses between 10⁻¹⁹ and 10⁻⁹ kg in interplanetary space and in the jovian and saturnian systems, to investigate their physical, chemical and dynamical properties as functions of the distances to the Sun, to Jupiter and to Saturn and its satellites and rings, to study their interaction with the saturnian rings, satellites and magnetosphere. Chemical composition of interplanetary meteoroids will be compared with asteroidal and cometary dust, as well as with Saturn dust, ejecta from rings and satellites. Ring and satellites phenomena which might be effects of meteoroid impacts will be compared with the interplanetary dust environment. Electrical charges of particulate matter in the magnetosphere and its consequences will be studied, e.g. the effects of the ambient plasma and the magnetic field on the trajectories of dust particles as well as fragmentation of particles due to electrostatic disruption.The investigation will be performed with an instrument that measures the mass, composition, electric charge, speed, and flight direction of individual dust particles. It is a highly reliable and versatile instrument with a mass sensitivity 10⁶ times higher than that of the Pioneer 10 and 11 dust detectors which measured dust in the saturnian system. The Cosmic Dust Analyzer has significant inheritance from former space instrumentation developed for the VEGA, Giotto, Galileo, and Ulysses missions. It will reliably measure impacts from as low as 1 impact per month up to 10⁴ impacts per second. The instrument weighs 17 kg and consumes 12 W, the integrated time-of-flight mass spectrometer has a mass resolution of up to 50. The nominal data transmission rate is 524 bits/s and varies between 50 and 4192 bps.This revised version was published online in July 2005 with a corrected cover date.