模态法辨识针刺C/ C 复合材料弹性模量

针对传统方法测量C/ C 复合材料弹性模量精度差问题,提出了一种利用模态试验辨识材料弹性 模量的新方法。数值仿真结果表明板件材料振动频率与弹性模量之间存在模糊对应关系,利用此关系采用二 分法及二阶响应面近似模型对材料弹性模量进行辨识,并分别利用各向同性薄壁板件及正交各向异性薄壁板 件对此方法进行验证,计算结果误差最大为16. 67%,最小仅为0. 5%,表明该方法准确有效。最后将其应用于 针刺C/ C 复合材料,获得了其弹性模量。仿真及试验结果均表明该方法无损、高效且准确度高。     

含氢 WC/ C 复合涂层在不同润滑油环境的摩擦性能

利用非平衡磁控溅射技术,通过同时离化乙炔气体和共溅射石墨靶与碳化钨靶,在304不锈钢和单晶硅基底上沉积具有Cr过渡层和WC过渡层的含氢WC/C复合涂层。采用扫描电镜、Raman光谱仪、X射线衍射仪、纳米压痕仪等对涂层的微观结构、力学性能进行分析。利用Rtec摩擦磨损试验机对WC/C复合涂层与304不锈钢基底在PAO基础润滑油环境、发动机润滑油环境以及腐蚀性发动机润滑油环境进行摩擦性能测试。结果表明:涂层内含有较多类石墨sp2键,WC1-x相镶嵌在非晶碳基质中构成多相复合结构;涂层的硬度和弹性模量明显高于304不锈钢基底,且其H/E值远高于基底;与304不锈钢基底相比,在三种润滑油环境下涂层均具有较低的摩擦因数和磨损率。     

ZrB2 及其复合陶瓷的高温抗氧化性能

综述了ZrB_2及其复合陶瓷的高温氧化行为,认为ZrB_2陶瓷是一种优异的高温结构材料,其氧化失效是由于氧化产物B_2O_3保护层挥发失效而导致的;二元陶瓷ZrB_2-SiC由于SiC的加入,高温抗氧化性能大大提高,并对其在不同温度下的氧化物结构进行了阐述。在此基础上提出了进一步提高ZrB_2-SiC陶瓷抗氧化性能和服役温度的方法,并以添加TaC和LaB_6形成三元复相陶瓷为例进行了说明。     

WC/C复合涂层海水环境的耐蚀性与摩擦性能

采用非平衡磁控溅射技术在304L不锈钢和单晶硅基底上沉积WC/C多层复合涂层,利用扫描电镜、Raman光谱仪、X射线衍射仪等研究WC/C复合涂层的微观结构,采用纳米压痕仪、划痕测试系统测试涂层的力学性能,利用电化学测试系统和摩擦磨损试验机分别研究涂层在人工配置的海水环境的耐蚀性能和摩擦性能。结果表明:WC/C复合涂层内含有较多类石墨sp2键结构,存在WC1-x相并镶嵌在非晶碳基质中。较之于304L不锈钢基底,WC/C复合涂层在海水环境中表现出更好的耐蚀性与更优异的摩擦适应性。     

基于MSC/PATRAN的飞机结构强度静力试验数据实时跟踪与处理系统开发

 在Windows环境下,以MSC/PATRAN为平台,利用平台提供的二次开发语言PCL(Patran Command Language),并结合C++语言,通过客户化、增设特定的命令和窗体等技术开发了飞机结构强度静力试验数据实时跟踪与处理系统TestDTAS（Test Data Tracking, Analyzing and Processing System）。在结构试验进行中,TestDTAS可以实时地监测结构试验件中应力和位移的变化情况,并与理论分析结果进行对比,而在试验结束后,TestDTAS可以进行试验数据回放和分析,从而将试验与理论分析有机的结合在一起,对结构静力试验和结构设计有很高的实用价值。     

Comparison of ionospheric F2 peak parameters foF2 and hmF2 with IRI2001 at Hainan

Monthly median values of foF2, hmF2 and M(3000)F2 parameters, with quarter-hourly time interval resolution for the diurnal variation, obtained with DPS4 digisonde at Hainan (19.5°N, 109.1°E; Geomagnetic coordinates: 178.95°E, 8.1°N) are used to investigate the low-latitude ionospheric variations and comparisons with the International Reference Ionosphere (IRI) model predictions. The data used for the present study covers the period from February 2002 to April 2007, which is characterized by a wide range of solar activity, ranging from high solar activity (2002) to low solar activity (2007). The results show that (1) Generally, IRI predictions follow well the diurnal and seasonal variation patterns of the experimental values of foF2, especially in the summer of 2002. However, there are systematic deviation between experimental values and IRI predictions with either CCIR or URSI coefficients. Generally IRI model greatly underestimate the values of foF2 from about noon to sunrise of next day, especially in the afternoon, and slightly overestimate them from sunrise to about noon. It seems that there are bigger deviations between IRI Model predictions and the experimental observations for the moderate solar activity. (2) Generally the IRI-predicted hmF2 values using CCIR M(3000)F2 option shows a poor agreement with the experimental results, but there is a relatively good agreement in summer at low solar activity. The deviation between the IRI-predicted hmF2 using CCIR M(3000)F2 and observed hmF2 is bigger from noon to sunset and around sunrise especially at high solar activity. The occurrence time of hmF2 peak (about 1200 LT) of the IRI model predictions is earlier than that of observations (around 1500 LT). The agreement between the IRI hmF2 obtained with the measured M(3000)F2 and the observed hmF2 is very good except that IRI overestimates slightly hmF2 in the daytime in summer at high solar activity and underestimates it in the nighttime with lower values near sunrise at low solar activity.     

A statistical study of C IV regions in 20 Oe-stars

In this paper, using the Gauss-Rotation model (GR model), we analyse the UV C IV resonance lines in the spectra of 20 Oe-stars of different spectral subtypes, in order to detect the structure of C IV region. We study the presence and behavior of absorption clouds and analyse their characteristics. From this analysis we can calculate the values of a group of physical parameters, such as the apparent rotational and radial velocities, the random velocities of the thermal motions of the ions, the Full Width at Half Maximum (FWHM), the optical depth, as well as the absorbed energy and the column density of the independent regions of matter, which produce the main and the satellite clouds of the studied spectral lines. Finally, we present the relations between these physical parameters and the spectral subtypes of the studied stars and we give our results about the structure of the C IV region in their atmosphere.     

Mapping lunar surface chemistry: New prospects with the Chandrayaan-2 Large Area Soft X-ray Spectrometer (CLASS)

Surface chemistry of airless bodies in the solar system can be derived from remote X-ray spectral measurements from an orbiting spacecraft. X-rays from planetary surfaces are excited primarily by solar X-rays. Several experiments in the past have used this technique of X-ray fluorescence for deriving abundances of the major rock forming elements. The Chandrayaan-2 orbiter carries an X-ray fluorescence experiment named CLASS that is designed based on results from its predecessor C1XS flown on Chandrayaan-1. We discuss the new aspects of lunar science that can be potentially achieved with CLASS.     

A broad climatology of very high latitude substorms

Magnetic data from a newly commissioned Indian Antarctic station Bharati (corrected geomagnetic (CGM) coordinates 74.7°S, 97.2°E) and closely-spaced IMAGE chain observatories (∼100° magnetic meridian in Northern hemisphere) has been analyzed to study the climatology of substorms which were localized poleward of the standard auroral oval. We considered four austral summers (year 2007–2010) when data from Bharati was available. Several very high latitude substorms were observed in this duration when the solar activity remained unexpectedly low for a long time. Various features of very high latitude substorms, e.g., local time dependence, interplanetary state, hemispherical asymmetry and their nightside low latitude signatures are examined. Events studied here, suggested the following properties of substorms occurring at very high latitudes: (1) maximum occurrence was observed near magnetic midnight (21:00–02:00 MLT). (2) In contradiction to earlier reports, many substorms were observed even during negative IMF Bz condition. In addition, majority of substorms occurred during low or moderate solar wind streams. (3) Magnetic signatures were often pronounced in the winter hemisphere. (4) Even if widely used standard AE indices fail to monitor very high latitude substorms, their low latitude signatures are often evident.     

50吨级氢氧火箭发动机的设计与研制

系统性地回顾了长征五号运载火箭芯一级50t级氢氧火箭发动机YF-77的设计与研制历程。通过分析氢氧发动机的特点以及国内外氢氧发动机的发展现状,阐述了国内新一代运载火箭研发的技术路线和50t级氢氧火箭发动机的研制背景;对50t级氢氧火箭发动机的总体技术方案及其特点进行了分析与总结,并在此基础上对发动机主要组件的技术方案及其特点开展分析;对发动机热试车情况、可靠性验证情况和故障排除情况进行了分析;对50t级氢氧火箭发动机的研制情况、技术特点进行了总结,并对国内氢氧发动机和液氧/甲烷发动机的发展进行了展望。