国外微波等离子推进器研究的新进展

回顾了国外微波等离子推进器（ＭＰＴ）的发展历史，简单介绍其基本工作原理与主要部件的设计、选材，论述理论与实验研究的新进展，给出推力、比冲与实验参数的范围。通过与电弧及电阻加热推进器的比较，得出结论：微波等离子推进器具有寿命长、效率和比冲高的优点，可用于地球同步通讯卫星的南北位置保持等。     

纤维缠绕复合材料层间质量声-超声无损评价

叙述了用声－超声进行复合材料危害性缺陷无损评价的研究，认为，声－超声信号在试样厚度上产生纵不皮共振，使得频谱能量集中在某些频率点附近，而声波又以切波的形式由发射换能器传向接收换能器，可用声－超声谱峰的位置来无损评价纤维缠绕增强型复合材料的层间结合质量。实验结果表明这一参量对纤维增强型合材料中的分层或紧贴型分层比较灵敏。     

战术导弹垂直发射系统的现状及发展趋势

介绍了垂直发射装置通用化、箱式化和模块化的总体特征。详细论述了国外现役8种类型的垂直发射系统，根据基本结构特点将垂直发射装置分为模块式结构、独立布置的分离式结构和旋转式结构，另依据发射动力将垂直发射装置分为热发射和冷发射。以热发射的同心筒式结构和冷发射采用的大倾角、模块化设计为例．分析了垂直发射装置的发展趋势。     

The Brazilian scientific microsatellite SACI-1

The National Space Research Institute (INPE) is developing the first Brazilian Scientific Microsatellite (SACI-1) based on the vanguard technology and on the experience acquired through projects developed by Brazilian Space Program. The SACI-1 is a 750km polar orbit satellite. The spacecraft will combine spin stabilization with geomagnetic control and has a total mass of 60 kg. The overall dimensions are 640×470×470 mm. The SACI-1 satellite shall be launched together with CBERS (China-Brazil Earth Resource Satellite). Its platform is being designed for multiple mission applications. The Brazilian Academy of Sciences has selected four scientific payloads that characterize the mission. The scientific experiments are: ORCAS (Solar and Anomalous Cosmic Rays Observation in the Magnetosphere), PLASMEX (Study of Plasma Bubbles), FOTSAT (Airglow Photometer), and MAGNEX (Geomagnetic Experiment).     

Models of P/Borrelly: Activity and dust mantle formation

Comet 19P/Borrelly was observed by Deep Space One spacecraft on September 22, 2001 (Soderblom et al., 2002).The DS1 images show a very dark and elongate nucleus with a complex topography; the IR spectra show a strong red-ward slope consistent with a very hot and dry surface (345K to 300K). During DS1 encounter the comet coma was dominated by a prominent jet but most of the comet was inactive, confirming the Earth-based observations that <10% of the surface is actively sublimating. We have developed a thermal evolution model of comet PBorrelly, using a numerical code that is able to solve the heat conduction and gas diffusion equations at the same time across an idealized spherical nucleus ( De Sanctis et al., 1999, 2000; Capria et al., 2000; Coradini et al., 1997a,b). The comet nucleus is composed by water, volatiles ices and dust in different proportions. The refractory component is made by grains that are embedded in the icy matrix. The code is able to account for the dust release, contributing to the dust flux, and the formation of dust mantles on the comet surface. The model was applied to a cometary nucleus with the estimated physical and dynamical characteristics of P/Borrelly in order to infer the status and activity level of a body on such an orbit during the DS1 observation. The comet gas flux, differentiation and thermal behavior were simulated and reproduced. The model results are in good agreement with the DS1 flyby results and the ground based observations, in terms of activity, dust coverage and temperatures of the surface.     

The population of massive stars in R136 from HST/FOC UV observations

New ultraviolet (1300 A, 3400 A),HST FOC observations have been used to derive the UV color-magnitude diagram (CMD) of R136, with the main scientific goal of studying the upper end of the stellar mass function at ultraviolet wavelengths where the color degeneracy encountered in visual CMDs is less severe. The CMD has been compared to a set of theoretical isochrones, which have been computed using the latest generation of evolutionary models and model atmospheres for early type stars. Wolf-Rayet stars are included. Comparison of theTheoretical andobserved CMD suggests that there are no stars brighter than M₁₃₀–11. We use the observed main sequence turn-off and the known spectroscopic properties of the stellar population to derive constraints on the most probable age of R136. The presence of WNL stars and the lack of red supergiants suggests a most likely age of 3±1 Myr. A theoretical isochrone of 3±1 Myr is consistent with the observed stellar content of R136 if the most massive stars have initial masses around 50 M.Bases on Observations with the NASA/ESA Hubble Space Telescope, obtained at the STScI, which is operated by AURA, Inc., under NASA contract NAS5-26555.Astrophysics Division, Space Science Department, ESA     

大迎角下鸭翼涡与边条涡的干扰特性

 在风洞测力、水洞染色线和激光片光实验的基础上 ,对翼身组合体鸭翼边条翼布局大迎角涡系干扰机理进行了分析和探讨 ,揭示了该布局增升的机理。鸭翼涡位于机翼内侧 ,其与边条涡的相互诱导致使边条涡向外翼偏折 ,既改善了外翼的流态 ,又使机翼前缘涡量卷入边条涡 ,增强了边条涡的强度 ,从而延迟其破裂。两方面的共同作用 ,提高了主翼的涡升力 ,起到增升作用。     

Experimental Aspects of Mid-Frequency Pulsations (f≈10–100 mHz) in the Southern Polar Cap

We review the results obtained in the frequency range of Pc3 (22-100 mHz) and Pc4 (7-22 mHz) pulsations at Italian Antarctic stations in the southern polar cap (“Mario Zucchelli”, at Terra Nova Bay, TNB, 80^˚.S; “Concordia”, the Italian/French base at Dome C, DMC, 89^˚.S). The absence of a midnight enhancement in the pulsation power suggests a negligible substorm influence at extreme latitudes, while the sharp noon enhancement, which appears only at TNB, is determined by the closer proximity of the station to cusp related phenomena. The relationship between the frequency of the band-limited signals and the interplanetary magnetic field strength, the cone angle influence, and the higher correlation of the Pc3 power with the solar wind speed in the morning hours suggest a global scenario in which upstream waves would be mainly responsible for the mid-frequency activity in the polar cap. However, the polarization pattern is odd with respect to the predictions for tailward propagating modes.     

基于CORBA实现专业领域软件在网络环境下的集成

如何有效地将已有系统集成或移植到新系统中 ,是集成系统开发中提出的一个重要问题。本文基于CORBA技术探讨如何实现遗留系统集成的方法 ,并通过实例重点阐述如何将已有的系统封装成CORBA对象的步骤。     

气动参数对后台阶三维缝隙换热影响的研究

针对涡轮叶片尾缘冷却结构特点,建立了后台阶三维缝隙结构气膜冷却特性试验台,测量了缝隙中心和肋中心下游换热系数的局部分布,研究了不同雷诺数Re(5000~15000)与吹风比Br(0.5~2.0)对换热系数的影响规律,试验结果表明:(1)出口的换热系数总体呈下降趋势,但在肋后中心线略有起伏;(2)随着Re的增大,换热系数增大,随着Br的增大,换热系数减小;(3)在靠近出口位置,由于热边界层与三维掺混特性流场的影响,使得换热变得复杂。