某型飞机天线罩防冰装置的性能验证

通过对某型飞机天线罩电热防冰装置的性能验证研究,找到了一种适用于飞机各类防冰装置预设计和对已有防冰装置验证的方法。该方法验证的天线罩防冰装置已经经历了飞行的考验。     

THE STUDY OF AIRPORTTERRAIN EFFECTS ON AUTOLAND FOR ANY AIRPLANE

<正> The terrain profile at several airports has caused some difficulty with autolands on the DC-10 and MD-80. Some operators have reported that the pilot had to disconnect the flight guidance system during flare and land manually. At present, the autoland guidance system is not uniquely designed to handle the variations of terrain. Since there is no accurate substitute for radio altitude(h_(rad)) the only variable left to improve is radio altitude rate (h_(rad)).     

树脂基碳纤维复合材料的热物理性能之一——导热系数

本文讨论了树脂基碳纤维复合材料热导与各种纤维体积含量V_f及温度的关系,研究了树脂基碳纤维复合材料的传热机理,并给出了大量的导热系数数据。     

树脂基碳纤维复合材料的热物理性能之一——热膨胀

本文讨论了碳纤维复合材料的热膨胀机理及热膨胀系数的理论计算,总结归纳了CFRP材料中纤维排布方式、温度等因素对热膨胀系数的影响,最后给出了一些CFRP材料的热膨胀系数。     

动态裂纹扩展韧性 K_(ID) 的估算及方法的评估

通过对30CrMnSi2A钢制成的DCB（带裂尖小孔）试件的试验结果和利用动态有限元法（DFEM）与远场路径无关的J′积分相结合的方法计算了动态裂纹扩展韧性。较全面地对各种估算KID的工程方法进行了分析比较和评估,讨论了使用范围。此外,改进了Kanninen的半经验公式,使它能对于不同泊松比的材料能方便地估算极限速度VL.同时,指出材料常数m应与裂纹的初始长度和止裂长度aa及裂尖半径有关,给出了计算公式,使得估算KID更为简便和合理。     

钝尾物体底部压力计算

 提出了一种简便可靠的计算钝尾物体表面压力分布及底部压力的方法。将钝尾物体绕流流场分为无粘区、边界层区和分离区。无粘区和边界层区分别用位流理论和边界层理论计算。分离区由根据尾流函数等建立的替代模型模拟。利用奇点法解出整个模型的压力分布。计算釆用迭代法进行。对Vanwagenen模型和鲁尔大学模型进行了计算,结果表明该方法是成功的。     

月面巡视器太阳能帆板功率衰减特性研究

太阳能帆板的功率衰减特性分析,对地外天体表面探测器的功率平衡、电源系统健康管理以及长寿命在轨管理有重要意义。通过对月面巡视器在轨运行第2到11月昼的电流遥测进行研究,提出了一种基于有限遥测的太阳能帆板功率衰减特性分析方法。首先利用一种滞环的方法对大量的电流遥测进行数据处理;然后进行日月距离和太阳入射角的归一化,通过数据拟合计算,得出落月第一年太阳能帆板功率衰减约为2.5%,并利用巡视器历次月昼唤醒时刻的太阳入射角变化情况验证了该方法的有效性,对地外天体的太阳能帆板功率衰减特性计算提供一定参考。     

评定运载火箭成本的TRANSCOST模型及其应用

首先介绍评定运载火箭的研制和发射成本的解析模型的结构,着重讨论评定使用成本的新方法,并引入众多参数来修正模型.尔后以“阿里安”4后继型为例,讨论用于未来系统分析和成本比较的模型,分析了采用10种不同方案的可贮低温燃料两级火箭的研制和发射成本.欧洲未来运载火箭系统的关键是要最佳解决有限的研制费用与期望的最低发射成本之间的矛盾.多次使用系统能使发射成本大为降低,但研制费用较大.基于实际参数的成本解析模型能为选择运载火箭方案提供重要的信息.     

Magnetic Field Fluctuations in the Solar Wind, Foreshock and Magnetosheath： Cluster Data Analysis

46 magnetosheath crossing events from the two years (2001.2-2003.1) of Cluster magnetic field measurements are identified and used to investigate the characters of the magnetic field fluctuations in the regions of undisturbed solar wind, foreshock, magnetosheath. The preliminary results indicate the properties of the plasma turbulence in the magnetosheath are strongly controlled by IMF orientation with respect to the bow shock normal. The amplitude of the magnetic field magnitude and direction variations behind quasi-parallel bow shock are larger than those behind quasi-perpendicular bow shock. Almost purely compressional waves are found in quasi-perpendicular magnetosheath.     

Structure of the Program of Short-term Prediction of Powerful Solar Flares

Input data of the system are two-dimensional images and one-dimensional distributions of total and polarized solar emission at 5.2 cm wavelength obtained with SSRT. Together with photoheliograms, magnetograms, Hα-filtergrams and characteristics of active regions received from other sources, they form the initial database. The first stage includes superimposing the images, identifying microwave sources with active regions, assigning NOAA numbers to the sources, and determining for each active region the heliolatitude, extent, and inclination angle of the group's axis to the equator. These data are used to calculate the boundaries of longitude zones for each active region. A next stage involves determining the brightness temperatures of microwave sources less than the polarization distribution, the degree of polarization, and microwave emission flux, as well as calculating the parameters of microwave sources. Each parameter is assigned its own value of the weight factor, and the sum of values is used to draw the conclusion about the flare occurrence probability in each active region and on the Sun in general.