“风云一号”气象卫星

本文叙述了中国第一颗气象卫星“风云一号”。这是一颗试验气象卫星,重750公斤,其主体为1.40米×1.40米×1.20米的六面体,连同太阳电池阵共展宽8.60米,高1.76米。运行在太阳同步轨道,高度900公里,倾角99°,每天绕地球运行14圈。地面接收到高质量的图象资料和轨道空间的辐射环境资料。     

观测轮廓显著性耦合时的轨道根数反演方法

针对脉冲轮廓显著性数据耦合情况下无法直接根据显著性数据反演轨道根数的问题,提出了一种根据脉冲轮廓显著性数据的方差特征进行解耦,并逐步实现轨道六根数估计的方法。利用X射线脉冲星实测数据完成了基于观测轮廓显著性数据方差特征的导航验证,实验结果表明根据显著性数据的方差特征可逐次解耦显著性数据,并以方差最小准则得到轨道根数的估计值,且定位误差为7.31 km。本文方法既不依赖标准脉冲轮廓,同时适用于轨道六根数均存在偏差的实际情况,在X射线脉冲星导航的实际应用中更具优势。     

复合轧辊喷射铸造成形坐标跟踪法数值模拟分析

通过计算机模拟,采用跟踪复合轧辊表面轮廓线坐标的方法(坐标跟踪法),计算复合轧辊在不同时刻的形状和尺寸.并分析各种喷射铸造工艺参数对复合轧辊形状的影响规律,模拟结果表明,辊芯平移速度和辊芯半径的变化对复合轧辊的沉积层厚度影响较大,而辊芯旋转速度和喷射距离的单独变化对轧辊沉积厚度影响很小.     

展向截断曲面乘波压缩进气道气动布局

描述了所设计的展向截断曲面乘波压缩进气道.其特点是采用曲面乘波压缩前体,前体进气道压缩面基准流场由等熵压缩波轴对称流场组成,三维乘波面采用密切曲锥方法由前缘线各点流线跟踪拟合构成流面.乘波面根据飞行器和发动机的宽度要求进行了截断.数值计算和风洞试验结果表明:与相同几何收缩比的四波系压缩进气道相比,在马赫数为4.5时,曲面乘波压缩进气道流量系数提高12%,总压恢复系数提高39%;在马赫数为6时,曲面乘波压缩进气道流量系数提高4%,总压恢复系数提高50%.超然冲压发动机性能明显提高.      

电离层短波射线追踪

本文以电离层等离子体参量的平均背景模式计算为基础, 给出一种电离层短波射线轨迹计算方法。供短波通信系统、工作于短波段的其它系统(如HF雷达的目标定位系统)及有关研究工作使用参考。      

利用转移矩阵进行姿态控制

传统欧拉角控制方法在处理大姿态角机动时往往出现奇异和交联问题。针对这一问题对欧拉角的跳变现象进行了讨论,并从飞行器实际姿态与需求姿态之间的空间关系入手,给出了一种消除欧拉角跳变现象的有效方法－转移矩阵法,仿真计算表明,该方法在大型航天器的姿态控制中可以有效地消除欧拉角奇异、交联和跳跃现象,在欧拉角跳变的情况下仍然能够实现对飞行器的控制。     

耗散大气中风场对内重力波传播的影响

使用考虑大气耗散的射线跟踪算法,计算了风场作用下重力波的传播情况.结果表明,风场对快速重力波分量影响较小,但对反射和传播区域的慢速波的影响较大,表现在顺风时使反射区范围缩小,逆风时使反射区范围扩大.在传播区,顺风场使慢速波分量的传播距离变小,传播高度降低,而逆风则使慢速重力波分量的传播距离明显增大,传播高度上升.分析表明,重力波传播的丰富多样性是由风场对波的衰减和反射等滤波作用引起的.      

Equatorial secondary cosmic ray observatory to study space weather and terrestrial events

Recently, equatorial secondary cosmic ray observatory has been established at Equatorial Geophysical Research Laboratory (EGRL), Tirunelveli, (Geographic Coordinates: 8.71°N, 77.76°E), to study secondary cosmic rays (SCR) produced due to the interaction of primary cosmic rays with the Earth’s atmosphere. EGRL is a regional center of Indian Institute of Geomagnetism (IIG), located near the equator in the Southern part of India. Two NaI(Tl) scintillation detectors are installed inside the temperature controlled environment. One detector is cylindrical in shape of size 7.62?cm?×?7.62?cm and another one is rectangular cuboid of 10.16?cm?×?10.16?cm?×?40.64?cm size. Besides NaI(Tl) detectors, various other research facilities such as the Geomagnetic observatory, Medium Frequency Radar System, Digital Ionosonde, All-sky airglow imager, Atmospheric electricity laboratory to measure the near-Earth atmospheric electric fields are also available at EGRL. With the accessibility of multi- instrument facilities, the objective is set to understand the relationship between SCR and various atmospheric and ionospheric processes, during space weather and terrestrial events.For gamma-ray spectroscopy, it is important to test the performance of the NaI(Tl) scintillation detectors and to calibrate the gamma-ray spectrum in terms of energy. The present article describes the details of the experimental setup installed near the equator to study cosmic rays, along with the performance testing and calibration of the detectors under various conditions. A systematic shift in the gain is observed with varying temperature of the detector system. It is found that the detector’s response to the variations in the temperature is not just linear or non-linear type, but it depends on the history of the variation, indicating temperature hysteresis effects on NaI detector and PMT system. This signifies the importance of isothermal environment while studying SCR flux using NaI(Tl) detectors, especially for the experiments conducted during daytime such as solar eclipses etc.     

The effect of collisions in ionogram inversion

The results of this paper demonstrate that the effect of collisions on the group refraction index is small, when the ordinary ray is considered. If, however, in order to improve the performance of a system for automatic interpretation of ionograms, the information contained in ordinary and extraordinary traces is combined, the effect of collisions between the electrons and neutral molecules should be taken into account for the extraordinary ray. The magnitude of these differences is generally very small and must be compared with the resolution in the virtual vertical height of the ionosonde, resolution which is typically of the order of few kilometers.     

Radial distribution of galactic cosmic rays at solar maximum

In this paper we analyze the spatial distribution of galactic cosmic rays during periods of maximum solar activity of the cycles 21, 22 and 23. We have used a two dimensional model to solve the cosmic ray transport equation. This model includes all relevant physical processes: diffusion, convection, drift and shock effects on cosmic ray propagation inside the heliosphere. We focused on the study of the radial distribution of galactic cosmic rays, and compare our results with the spacecraft observations for two energies (175 MeV H and 265 MeV/n He). Although the radial intensities of galactic cosmic rays can be explained qualitatively with all three local interstellar spectra (LISs) used in this work, we applied a reduced chi-squared analysis to investigate the best LIS that could fit the data.