直升机机体－主减－旋翼耦合系统动稳定性分析

对单桨常尾桨铰接式直升机机体－主减－族翼耦合系统动稳定性进行了分析研究。在建立的数学模型中,除了考虑机体沿侧向和纵向的平动,机身的横滚、俯仰和偏航,旋翼的挥舞和摆振外,还特别考虑了机身的横向运动及主减的摆动和传动特性。以某型直升机为基础的研究表明：挥舞对耦合系统的动稳定性有一定影响;不考虑挥舞和主减支承特性时,对耦合系统动稳定性的分析偏于保守;在合适的主减支承条件下,主减对耦合系统的动稳定性影响不大;旋翼的挥舞与主减的摆动是耦合的,这使主减的固有频率提高。     

橇式起落架动刚度及阻尼特性试验研究

起落架动刚度及阻尼特性是研究直升机“地面共振”问题两个重要参数。刚进入国产化阶段的模式起落架迄今尚无可靠的理论计算方法来确定这两个参数．本试验研究利用某型直升机真实的模式起落架为试件，采用机械阻抗测量法来研究该起落架的动刚度及阻尼特性。试验使用电液伺服激振设备，对模式起落架进行不同频率的激振，实时测量相应的载荷及位移响应，从而得出了模式起落架的动刚度及阻尼。试验模拟了直升机完全停机及半升力卸载情况，在机场及冰面降落情况，以及３个不同方向的受载情况。试验结果已直接用于某型直升机的“地面共振”分析。     

一种微波等离子体原子氧模拟装置

介绍了一种新颖的原子氧模拟试验装置。该装置采用了微波电子回旋共振（ｅｌｅｃｔｒｏｎｃｙｃｌｏｔｒｏｎｒｅｓｏｎａｎｃｅ简称“ＥＣＲ”）的先进技术。最佳调试状态下，可获得１０（１５）／（ｃｍ２·ｓ）的束流。在该试验装置上，对航天器上常用的Ｋａｐｔｏｎ和石墨环氧材料进行了原子氧效应试验，首次在国内成功的获得了原子氧束流模拟试验的样品结果。对样品的表面形貌分析证明：试验结果完全与国外同类设备的试验结论一致，这标志着中国在原子氧地面模拟技术领域的研究已取得重要进展。     

SPR生物传感器在生命科学及在航天医学中的应用

表面等离子体共振生物传感器在分析生物分子相互作用方面，具有灵敏度高、实时在线、简单快捷和抗干扰能力强等优点，被广泛应用于临床检验、药物筛选等研究领域；因其能满足空间特殊环境下的使用要求，在航天医学领域具有广阔的应用前景．本文综述了表面等离子体共振生物传感器的原理、特点、在生命科学研究中的应用及在航天医学中的应用前景．     

连续自由流电泳微重力下分离模式蛋白质的研究

以连续自由流电泳的区带电泳模式分离血红蛋白和细胞色素C，比较了不同缓冲液甘油浓度下的分离效果，确定了最终装载在神舟4号飞船上A3—2型电泳仪的电泳分离条件，通过地面和空间实验，初步探讨了微重力对连续自由流电泳分离的影响，并对电泳的分离产物做了多种检测．     

微量气味成分的自由基簇射技术脱除

研究了密闭体系中微量气味污染物的脱除作用与机理。采用电晕放电自由基簇射技术，实现了人工环境下氧化性自由基的产生；以电子自旋共振技术（ESR）对气态羟基自由基实施了捕集和检测，验证了在羟基自由基的存在下NH3被氧化为N2。通过U—I获得反应能耗和污染物去除效率为：NH3脱除效率为90．6％时，能耗1．0W。研究表明：自由基簇射技术产生的氧化性自由基可有效去除密闭生存环境中产生的NH3等微量有害气味成分，将在空间站等密闭生存系统内空气净化中有很好的应用前景。     

固体冲压发动机喷管用C/C-SiC复合材料

采用"化学气相渗透+先驱体浸渍裂解"(CVI+PIP)混合工艺制备固体冲压发动机用C/C-SiC复合材料喷管内层,综合考查复合材料的微观结构、弯曲性能和抗烧蚀性能以及固冲发动机C/C-SiC喷管内层水压和点火实验。结果表明:复合材料的弯曲强度达到197 MPa,且断裂破坏行为呈现典型的韧性模式;复合材料具有优异的抗氧化烧蚀性能,氧化烧蚀200 s后线烧蚀率仅为0.0063 mm·s-1;研制的C/C-SiC复合材料构件的水压爆破压强为6.5 MPa,表明构件具有良好的整体承载能力;C/C-SiC复合材料喷管内层高温综合性能通过了固体冲压发动机点火实验考核。     

TMS320C6678多核DSP的加载配置和实现方法

程序代码正确的固化加载运行是多核DSP应用的前提和基础.简要介绍了DSP的加载器和加载过程,阐述了多核处理器件的加载配置管理方法.以TI公司的多核DSP TMS320C6678为例,介绍了多核DSP的加载模式和流程,详细阐述了EMIF16的Nor FLASH加载实现方法,可以实现多核DSP软件的正确、可靠加载运行.     

Global ionospheric scintillations revealed by GPS radio occultation data with FY3C satellite before midnight during the March 2015 storm

Global observations of S4 amplitude scintillation index by the GPS Occultation Sounder (GNOS) on FengYun-3 C (FY3C) satellite reveal global dynamic patterns of a strong pre-midnight scintillations in F-region of the ionosphere during the St. Patrick’s Day geomagnetic super storm of 17–19 March 2015. The observed strong scintillations mainly occurred in the low latitudes, caused by equatorial plasma bubbles. During the main storm phase (March 17), the scintillations were first triggered in the New Zealand sector near 160°E longitudes, extending beyond 40°S dip latitude. They were also enhanced in the Indian sector, but significantly suppressed in East Asia near 120°E longitude and in Africa around 30°E longitude. During the initial recovery phase (March 18–19), the global scintillations were seldom observed in GNOS data. During the later recovery phase (after March 19), the scintillations recovered to the pre-storm level in Indian, African, and American sectors, but not in East Asian and any of Pacific sectors. These results closely correlate with observations of the density depletion structures by the Communication/Navigation Outage Forecasting System (C/NOFS) satellite, and ground-based instruments. Such consistency indicates reliability of our scintillation sensing approach even in a case-by-case comparison study. The prompt penetration electric field and disturbance dynamo electric field are suggested as the main factors that control the enhancement and inhibition of the scintillations during the storm, respectively.     

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.