C/E复合材料螺旋铣孔切屑形状与切削温度研究

碳纤维增强环氧树脂基体(C/E)复合材料具有优异的性能,广泛用于制造飞行器结构件。在加工C/E复合材料连接孔过程中容易出现分层、撕裂等加工缺陷,而切削温度过高是导致加工缺陷的主要原因之一。螺旋铣孔作为新的制孔技术,加工C/E复合材料时表现出许多优于传统钻孔的特点,受到广泛关注。本文采用专用加工装备开展了C/E复合材料制孔试验,利用红外热像仪实时监测切削温度,分析了螺旋铣孔加工参数对切削温度的影响规律。根据螺旋铣孔运动学规律和切削原理,从未变形切屑形状特点入手分析了螺旋铣孔切削温度的来源和影响因素。研究结果可对深入理解螺旋铣孔加工机理、制定合理的螺旋铣孔加工工艺提供依据。     

力值加载装置控制系统设计

针对力标准机不适用于力值现场校准测试的问题,设计了一种便携式的力值加载装置。该装置采用STM32F103为主控单片机,采用高准确度AD转换器测量力值,优化了力值加载控制算法,避免了力值加载过程中可能出现的各种问题。该装置控制速度快,准确度高,适用于力值现场校准测试。     

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。     

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.     

Longitudinal variation of the equatorial ionosphere: Modeling and experimental results

We describe a new version of the Parameterized Regional Ionospheric Model (PARIM) which has been modified to include the longitudinal dependences. This model has been reconstructed using multidimensional Fourier series. To validate PARIM results, the South America maps of critical frequencies for the E (foE) and F (foF2) regions were compared with the values calculated by Sheffield Plasmasphere-Ionosphere Model (SUPIM) and IRI representations. PARIM presents very good results, the general characteristics of both regions, mainly the presence of the equatorial ionization anomaly, were well reproduced for equinoctial conditions of solar minimum and maximum. The values of foF2 and hmF2 recorded over Jicamarca (12°S; 77°W; dip lat. 1°N; mag. declination 0.3°) and sites of the conjugate point equatorial experiment (COPEX) campaign Boa Vista (2.8°N; 60.7°W; dip lat. 11.4°; mag. declination −13.1°), Cachimbo (9.5°S; 54.8°W; dip lat. −1.8°; mag. declination −15.5°), and Campo Grande (20.4°S; 54.6°W; dip lat. −11.1°; mag. declination −14.0°) have been used in this work. foF2 calculated by PARIM show good agreement with the observations, except during morning over Boa Vista and midnight-morning over Campo Grande. Some discrepancies were also found for the F-region peak height (hmF2) near the geomagnetic equator during times of F₃ layer occurrences. IRI has underestimated both foF2 and hmF2 over equatorial and low latitude sectors during evening-nighttimes, except for Jicamarca where foF2 values were overestimated.