复杂可修系统可信度建模中任务维修度计算的统计推断方法

在设定每一部件的致命性故障率为常数并在确定出各部件任务修复时间置信上限的基础上,通过对可能发生的多次致命性故障事件的概率状态描述,得到了部件故障率与系统可信度的定量关系,进而依据这一可信度的建模原理归纳出不考虑任务修复时间的具体分布类型时复杂可修串联系统可信度的计算方法,同时也给出了任务维修度的统计推断表达式;最后,以典型的 ４ 部件串联可修系统为例,探讨了致命性故障次数、允许任务修复时间、部件任务修复时间的不同置信上限等的变化对系统可信度的影响,并论证了系统可靠性、维修性和保障性与可信度的关系。     

提高数控系统可靠性的解析余度研究

为提高航空发动机数字控制系统的可靠性，本文用解析余度技术，对系统传感器故障检测，隔离、调整的方法进行仿真研究，仿真系统中的发动机数学模型是用一系列小偏差线化模型去逼进某一实际发动机的试车数据而得到的，这里建立的传感器故障模型模拟各种故障的发生，设计分离的卡尔曼滤波器产生的残差秩序构造－决策函数，对故障进行检测及隔离调查。本文在ＭＡＴＬＡＢ语言环境，对可能发生的故障进行了仿真研究，所得结果说明，这种     

用于生物医学信号检测的超薄测力传感器

随着社会文明程度的不断提高和人口老龄化的发展，人体股骨骨折的预防在现代社会中的重要性和巨大社会意义日益引起人们的关注。通过仿真实验研究冲击状态下人体皮下脂肪对冲击能量的吸收和冲击力的衰减机理，可以为骨折防护器的设计提供可靠依据。本文介绍了利用压电薄膜制作的超薄测力传感器在上述实验中的应用、测量原理和和测量系统的构成以及与之相配套的计算机应用软件。     

三维接触问题有限元解法的单元选取初析

本文对８节点六面体线性等参元和２０节点六面体二次等参元的特性进行了分析和计算。根据三维接触问题有限元解法的特点指出．在三维接触问题有限元解法中，为避免单元特性与接触条件相抵触，只能选用８节点六面体等参元，而不能选用２０节点六面体等参元，并通过计算实例进行了验证。     

低速涡轮叶栅风洞中叶片表面边界层转捩图像捕捉

在高性能航空与民用燃汽轮机设计过程中,涡轮叶栅内部叶片表面边界层由层流向湍流的转捩始终得到设计者的关注,原因就在于叶片表面边界层流态与叶型损失密切相关。笔者在特定的低速来流条件下,采用多种剪敏液晶显示材料,深入研究了叶栅风洞中叶片表面边界层流态剪敏液晶显示技术,对美国联合技术公司(UTC)提供的涡轮叶栅进行了大量吹风实验,从实验拍摄的图像分析,证实了该项技术能够在一定范围内较为准确地探测叶片表面边界层转捩的发生。为从机理上更深刻地认识叶片表面粘性边界层转捩机制,笔者对来流马赫数和冲角对转捩过程的影响进行了分析。     

On the 3D structure of the nebula around η-Carinae

The asymmetric shape of the nebula around η-Carinae (Homunculus) can be explained by a spherical expansion in a non-homogeneous medium. Two models are analyzed: an exponential and an inverse power law dependence for the density as a function of distance from the equatorial plane. The presence of a medium with variable density along the polar direction progressively converts the original spherical shell into a bipolar nebula. In the case of the nebula around η-Carinae, we know the time elapsed since the great outburst in 1840. An exact match between observed radii and velocities can be obtained by fine tuning the parameters involved, such as initial radius, initial velocity and the typical scale that characterizes the gradient in density. The observed radius and velocity of the Homunculus as a function of the polar angle in spherical coordinates can be compared with the corresponding simulated data by introducing the efficiency in a single or multiple directions. Once the 3D spatial structure of the Homunculus is obtained, we can compose the image by integrating along the line of sight. In order to simulate the observed image, we have considered a bipolar nebula with constant thickness and an optically thin emitting layer. Some simulated cuts of the relative intensity are reported and may represent a useful reference for the astronomical cuts.     

基于导航星域和K矢量的快速星图识别算法

星图识别算法是星敏感器的关键技术,快速性和可靠性一直是对其评价的重要指标。提出了基于K矢量查找表和导航星域联合进行超快速星图识别的方法。首先根据星敏感器视场和所能敏感的星等建立全天球导航星表;再依据K矢量的原则对全天的导航星按照星对角距进行分类,建立星对角距所对应导航星的K矢量和K矢量查找表。利用星敏感器视场中的4颗星构成6组星对角距,将其中的5组星对角距所对应K矢量查找表域的星对组进行导航星表域（简称导航星域）的变换,根据另外一组星对角距所对应的K矢量查找表域的值对前面5组导航星域的值同时进行索引比较,直接找到了满足条件的4颗导航星,即完成全天的星图识别。最后,通过计算机仿真,实验室模拟和真实星空实验三个层次验证了此方法的可靠性和快速性。     

Heliospheric asymmetries due to the action of the interstellar magnetic field

We discuss the asymmetry of the heliospheric discontinuities obtained from the analysis of 3D modeling of the solar wind (SW) interaction with local interstellar medium (LISM). The flow of charged particles is governed by the ideal MHD equations and the flow of neutral particles is described by the Boltzmann equation. The emphasis is made on the asymmetries of the termination shock (TS) and the heliopause under the combined action of the interstellar and interplanetary magnetic fields (ISMF and IMF) in the presence of neutral hydrogen atoms whose transport through the heliosphere is modeled kinetically, using a Monte Carlo approach. We show that the deflection of neutral hydrogen flow from its original direction in the unperturbed LISM is highly anisotropic and evaluate a possible angle between the hydrogen deflection plane measured in the SOHO SWAN experiment and the plane containing the ISMF and LISM velocity vectors for different ISMF strengths. It is shown that the ISMF of a strength greater than 4 μG can account for the 10 AU difference in the TS heliocentric difference observed during its crossing by the Voyager 1 and Voyager 2 spacecraft, which however results in a larger discrepancy between the calculated and observed velocity distributions. The effect of a strong ISMF on the distribution of plasma quantities in the inner heliosheath and on 2–3 kHz radio emission is discussed.     

Physics of ion acceleration in the solar flare on 2005 September 7 determines γ-ray and neutron production

Relativistic neutrons were observed by the neutron monitors at Mt. Chacaltaya and Mexico City and by the solar neutron telescopes at Chacaltaya and Mt. Sierra Negra in association with an X17.0 flare on 2005 September 7. The neutron signal continued for more than 20 min with high statistical significance. Intense emissions of γ-rays were also registered by INTEGRAL, and during the decay phase by RHESSI. We analyzed these data using the solar-flare magnetic-loop transport and interaction model of Hua et al. [Hua, X.-M., Kozlovsky, B., Lingenfelter, R.E. et al. Angular and energy-dependent neutron emission from solar flare magnetic loops, Astrophys. J. Suppl. Ser. 140, 563–579, 2002], and found that the model could successfully fit the data with intermediate values of loop magnetic convergence and pitch-angle scattering parameters. These results indicate that solar neutrons were produced at the same time as the γ-ray line emission and that ions were continuously accelerated at the emission site.