关于运输网络堵塞流动的研究——分支定界法在求解网络最小流上的应用（Ⅲ）

堵塞是以人为主体在运输网络中经常发生的一种现象。本文中所定义的网络最小流是指在最严重堵塞的情况下通过网络的最大流量，是设计和运行一个运输网络，特别是一个紧急疏散网络的重要参数。本文在堵塞流理论研究的基础上，提出了一种用分支定界思想来求解网络最小流问题的方法，并用实例说明了该算法过程及其应用领域     

Calculation of a safety factor of damaged composite main rotor blade according to limit equilibrium theory

Safety factors of the Ansat helicopter main rotor blade are determined in the root section at various flight modes with taking into account the possible damages.     

航行体垂直发射过程不确定性量化方法的探讨

在发射平台运动、海浪及海流、气水介质突变、空泡溃灭等的影响下,航行体水下垂直发射呈现出干扰因素随机性强、干扰量大、弹道参数变化剧烈等特点。在分析、辨识各种干扰因素的形成机制及组成结构的基础上,建立了描述航行体水下发射过程不确定度的数学模型;介绍了近年来国际上较为热门的不确定性量化研究中的数值方法和进展,主要讨论了基于多项式混沌理论的不确定度量化方法;最后,探讨了未来航行体水下发射过程不确定性量化研究所面临的一些挑战和亟待解决的问题。     

“双证融通”的高职职业能力培养体系的构建

高职教育专业教学和职业能力培养间普遍存在着相互独立运行，融通渠道不畅，缺乏驱动机制等问题。针对上述问题，提出了在学历教育和职业能力培养问建立融通机制的思路，构建了基于“双证融通”的职业能力培养体系，给出了具体的实施和操作方法。     

频率计数器在航天器信号频率测量中的适用性分析

从频率计数器的工作原理出发,分析了航天器测控通信中常用的调相信号、调频信号和相移键控信号的频率测量误差,给出了调相信号和调频信号的测量误差表达式。使用频率计数器对上述3种航天器信号进行了频率测量试验。理论分析和试验结果表明,频率计数器适用于航天器调相信号和调频信号的频率测量,不适用于相移键控信号的频率测量。在实际使用中,为保证测量精度,应根据被测信号的调制方式选择适当的测量方法。     

基于华氏宏观经济数学模型的高等职业教育动态投入产出模型

伴随着经济的发展和产业结构的变化,高等职业教育越来越受重视,高职教育的投入产出关系也引起了人们的关注。通过分析高职教育的投入产出关系,应用华氏宏观经济数学模型建立了高等职业教育动态投入产出模型。它对分析高职教育各项投入的效率具有实际意义。     

Temporal variation of the arterial pressure in healthy young people and its relation to geomagnetic activity in Mexico

We present a study of the temporal behavior of the systolic (SBP) and diastolic (DBP) blood pressure for a sample of 51 normotensive, healthy volunteers, 18 men and 33 women with an average age of 19 years old in Mexico City, Mexico, during April and May, 2008. We divided the data by sex along the circadian rhythm. Three geomagnetic storms occurred during the studied time-span. The strongest one, a moderate storm, is attributed to a coronal hole border that reached the Earth. The ANOVA test applied to the strongest storm showed that even though we are dealing with a moderate geomagnetic storm, there are statistically significant responses of the blood pressure. The superposed epoch analysis during a three-day window around the strongest storm shows that on average the largest changes occurred for the SBP. Moreover, the SBP largest increases occurred two days before and one day after this storm, and women are the most sensitive group as they present larger SBP and DBP average changes than men. Finally, given the small size of the sample, we cannot generalize our results.     

The STEREO/IMPACT Magnetic Field Experiment

The magnetometer on the STEREO mission is one of the sensors in the IMPACT instrument suite. A single, triaxial, wide-range, low-power and noise fluxgate magnetometer of traditional design—and reduced volume configuration—has been implemented in each spacecraft. The sensors are mounted on the IMPACT telescoping booms at a distance of ～3 m from the spacecraft body to reduce magnetic contamination. The electronics have been designed as an integral part of the IMPACT Data Processing Unit, sharing a common power converter and data/command interfaces. The instruments cover the range ±65,536 nT in two intervals controlled by the IDPU (±512 nT; ±65,536 nT). This very wide range allows operation of the instruments during all phases of the mission, including Earth flybys as well as during spacecraft test and integration in the geomagnetic field. The primary STEREO/IMPACT science objectives addressed by the magnetometer are the study of the interplanetary magnetic field (IMF), its response to solar activity, and its relationship to solar wind structure. The instruments were powered on and the booms deployed on November 1, 2006, seven days after the spacecraft were launched, and are operating nominally. A magnetic cleanliness program was implemented to minimize variable spacecraft fields and to ensure that the static spacecraft-generated magnetic field does not interfere with the measurements.     

Geophysical Constraints on the Evolution of Mars

The evolution of Mars is discussed using results from the recent Mars Global Surveyor (MGS) and Mars Pathfinder missions together with results from mantle convection and thermal history models and the chemistry of Martian meteorites. The new MGS topography and gravity data and the data on the rotation of Mars from Mars Pathfinder constrain models of the present interior structure and allow estimates of present crust thickness and thickness variations. The data also allow estimates of lithosphere thickness variation and heat flow assuming that the base of the lithosphere is an isotherm. Although the interpretation is not unambiguous, it can be concluded that Mars has a substantial crust. It may be about 50 km thick on average with thickness variations of another ±50 km. Alternatively, the crust may be substantially thicker with smaller thickness variations. The former estimate of crust thickness can be shown to be in agreement with estimates of volcanic production rates from geologic mapping using data from the camera on MGS and previous missions. According to these estimates most of the crust was produced in the Noachian, roughly the first Gyr of evolution. A substantial part of the lava generated during this time apparently poured onto the surface to produce the Tharsis bulge, the largest tectonic unit in the solar system and the major volcanic center of Mars. Models of crust growth that couple crust growth to mantle convection and thermal evolution are consistent with an early 1 Gyr long phase of vigorous volcanic activity. The simplest explanation for the remnant magnetization of crustal units of mostly the southern hemisphere calls for an active dynamo in the Noachian, again consistent with thermal history calculations that predict the core to become stably stratified after some hundred Myr of convective cooling and dynamo action. The isotope record of the Martian meteorites suggest that the core formed early and rapidly within a few tens of Myr. These data also suggest that the silicate rock component of the planet was partially molten during that time. The isotope data suggest that heterogeneity resulted from core formation and early differentiation and persisted to the recent past. This is often taken as evidence against vigorous mantle convection and early plate tectonics on Mars although the latter assumption can most easily explain the early magnetic field. The physics of mantle convection suggests that there may be a few hundred km thick stagnant, near surface layer in the mantle that would have formed rapidly and may have provided the reservoirs required to explain the isotope data. The relation between the planform of mantle convection and the tectonic features on the surface is difficult to entangle. Models call for long wavelength forms of flow and possibly a few strong plumes in the very early evolution. These plumes may have dissolved with time as the core cooled and may have died off by the end of the Noachian.     

层板冷却特性的实验与数值模拟研究

在大尺寸低速回流式风洞内对一种应用于涡轮叶片的典型的层板结构进行了流阻特性和冷却特性的实验研究,获取了该层板综合冷却效果与层板两侧压比的关系,结果表明层板具有很高的冷却效果。运用商用软件Fluent6 0对其进行了流固耦合传热计算,分析了层板内部复杂的流动和换热情况,得到了在不同的进出口条件下该层板的综合冷却效果。计算结果和实验值进行了比较,两者符合较好,表明通过数值计算获取层板冷却效果的方法是可行的。