转子爆破对飞机机体结构危害的风险量化方法研究

结合某型民用飞机转子爆破对机体结构危害的风险量化分析经验,通过对系统的处理方法进行类比,以概率统计为基础,将转子爆破对飞机机体的危害进行分级量化,形成了1套典型分析方法,可为其他型号飞机的相关设计工作提供借鉴。     

民机系统发动机转子爆破特定风险分析方法

基于美国联邦航空局咨询通告给出的发动机非包容转子爆破特定风险安全性评估指南,提出了一种简单易用的发动机非包容转子爆破安全性分析方法。建立了简化的转子碎片碰撞角度计算模型,以确定受转子碎片影响的系统部件;改进了失效部件组合检查单,提高分析工作效率,并确定转子碎片对系统的安全性影响。相比于传统分析方法,简化了转子爆破风险安全性分析过程,减少了分析工作量,适用于飞机系统研制初期对转子爆破风险的危害性进行保守性评估,以指导系统架构优化设计。     

鲁棒EKF在脉冲星导航系统中的应用

针对脉冲星导航系统的滤波问题,传统的扩展卡尔曼滤波(EKF)算法存在不能克服系统模型存在不确定性参数以及乘性噪声等缺陷,提出一种鲁棒EKF算法。首先,分析了状态预测误差方程和估计误差方程,利用统计学原理,得到了状态预测方差矩阵和状态估计方差矩阵计算等式。由于系统模型存在不确定性参数,状态预测协方差矩阵和状态估计协方差矩阵无法计算;因此,利用4个重要矩阵不等式,分析并找到预测方差矩阵和状态估计方差矩阵的上界。最后,利用状态估计误差协方差矩阵上界设计状态增益矩阵,使得状态估计协方差矩阵的迹最小。将该算法对脉冲星导航系统进行仿真,仿真结果验证了所提算法的有效性。     

C/ C-PAA 与C/ C-FA 弯曲性能对比

通过PIP工艺制备了C/C-PAA、C/C-FA复合材料,对PAA、FA裂解碳的XRD、浸渍效果以及C/C-PAA和C/C-FA的弯曲强度进行了分析.结果表明:PAA裂解碳的炭质量、浸渍效果较好,C/C-PAA弯曲强度比C/C-FA弯曲强度高34.9％,弯曲模量对比不明显.     

M40J/CE/EP复合材料出气性能研究

通过地面环境模拟实验,分析了高模碳纤维/环氧树脂改性氰酸酯复合材料(M40J/CE/EP)的表面元素,研究了高真空加热环境下复合材料的真空出气性能和出气气体成分.结果表明,M40J/CE/EP复合材料的表面主要由C、O、N元素构成;经高真空加热后,复合材料的出气气体成分以小分子挥发物和碳氢化合物电离碎片为主,有可能在空间低温条件下冷凝在航天器的敏感器件表面而造成污染;通过真空出气性能实验测得,M40J/CE/EP复合材料的总质量损失(TML)的平均值为0.27%,收集到的可凝挥发物(CVCM)为0,完全达到出气筛选合格的指标要求.     

高浓度颗粒流冲刷条件下硅橡胶和EPDM绝热材料动态烧蚀实验

利用X射线实时诊断技术(RTR)针对硅橡胶和EPDM绝热材料,开展了高浓度颗粒流冲刷条件下动态烧蚀实验研究,成功获得了绝热材料烧蚀表面退移过程的序列图像。研究表明:(1)在本实验条件下,硅橡胶绝热材料颗粒冲刷区域的瞬时烧蚀率在0～2s内迅速增加,2s之后瞬时烧蚀率略有下降并趋于稳定;EPDM绝热材料颗粒冲刷区域的瞬时烧蚀率在0～1s内迅速增加,1s之后瞬时烧蚀率趋于稳定;(2)相同冲刷条件下硅橡胶绝热材料抗颗粒流冲刷性能比EPDM绝热材料差,硅橡胶绝热材料不适合在高过载发动机中应用;(3)高浓度颗粒流冲刷条件下绝热材料的烧蚀率比常规条件下要严重的多,其机理主要是高温颗粒流对炭化层有强烈的机械剥蚀效应和热化学烧蚀作用。实验结果对硅橡胶和EPDM绝热材料烧蚀机理研究及烧蚀建模具有重要参考价值。     

不同工件超光滑表面残余应力的测试研究

通过对玻璃、陶瓷、金属3个试件进行超精密加工,使试件表面粗糙度达到纳米级,采用非破坏性的X射线衍射sin2ψ法测量原理对不同试件的残余应力进行了测试研究。结果表明:在本试验条件下,3个试件都只存在残余压应力,并且陶瓷的残余压应力最大,金属残余压应力最小。     

Statistical study of radio drifting pulsation structures with associated CMEs and other observations

Solar radio burst, especially the fine structures (FSs) and the drifting pulsation structures (DPSs), may be used as an important diagnostics tool to draw the evolution map of the flare loop in the initial phase of solar flares. In this work, 52 radio events were found accompanying with DPSs. They were all observed with the Solar Radio Spectrometers (0.625–7.6 GHz) of China during 1998–2004. Combining the radio observations with LASCO-C2, Goes-8 SXR, H_α, EUV and Trace observations, we analyzed all these events and obtained some statistic conclusions: First, 88% DPSs take place at the initial phase of the radio burst, and their rich spectrum characteristics are helpful to understand the events further. Second, 83% DPSs are associated with CMEs or ejection events, and all the events are accompanied by Goes SXR flare. Third, for CMEs and DPSs, which take the first step, there is no significant predominance of either of them. The relationship between the DPSs and CMEs is still not clear in this study because of the lack of spatial resolution in the centimeter–decimeter band. However, the EIT or Trace ejection happened during the onset/end time of DPSs. They are signatures of the initial phase of CMEs. Two events will be illustrated to explain this.     

MESSENGER and the Chemistry of Mercury’s Surface

The instrument suite on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft is well suited to address several of Mercury’s outstanding geochemical problems. A combination of data from the Gamma-Ray and Neutron Spectrometer (GRNS) and X-Ray Spectrometer (XRS) instruments will yield the surface abundances of both volatile (K) and refractory (Al, Ca, and Th) elements, which will test the three competing hypotheses for the origin of Mercury’s high bulk metal fraction: aerodynamic drag in the early solar nebula, preferential vaporization of silicates, or giant impact. These same elements, with the addition of Mg, Si, and Fe, will put significant constraints on geochemical processes that have formed the crust and produced any later volcanism. The Neutron Spectrometer sensor on the GRNS instrument will yield estimates of the amount of H in surface materials and may ascertain if the permanently shadowed polar craters have a significant excess of H due to water ice. A comparison of the FeO content of olivine and pyroxene determined by the Mercury Atmospheric and Surface Composition Spectrometer (MASCS) instrument with the total Fe determined through both GRNS and XRS will permit an estimate of the amount of Fe present in other forms, including metal and sulfides.     

Stellar Coronal Astronomy

Coronal astronomy is by now a fairly mature discipline, with a quarter century having gone by since the detection of the first stellar X-ray coronal source (Capella), and having benefitted from a series of major orbiting observing facilities. Serveral observational characteristics of coronal X-ray and EUV emission have been solidly established through extensive observations, and are by now common, almost text-book, knowledge. At the same time the implications of coronal astronomy for broader astrophysical questions (e.g.Galactic structure, stellar formation, stellar structure, etc.) have become appreciated. The interpretation of stellar coronal properties is however still often open to debate, and will need qualitatively new observational data to book further progress. In the present review we try to recapitulate our view on the status of the field at the beginning of a new era, in which the high sensitivity and the high spectral resolution provided by Chandra and SMM-Newton will address new questions which were not accessible before. This revised version was published online in August 2006 with corrections to the Cover Date.