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。     

时延-角度特性研究

本文在球不对称局域准抛物电离层模型下,设计了一套射线追踪算法的计算机程序。研究了时延随角度变化特性。指出了最小时延的传统求解方法的适应范围,讨论了时延-角度特性曲线与返回散射电离图的关系及其能量分布特点。     

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.     

星敏感器光学系统的热/结构/光分析

星敏感器是高精度的航天器姿态测量器件,其性能受太空温度环境的影响。运用有限元法和光线追迹法,建立星敏感器光学系统的热/结构/光分析模型,研究光学系统温度分布与星敏感器测量误差的关系,得到了算例光学系统在温度均匀分布条件下的温度变化以及轴向温度梯度变化、侧向温度梯度变化与星敏感器测量误差的关系曲线;给出了算例光学系统热误差小于角秒量级的温度条件:均匀温度分布条件下温度变化量≤10℃、轴向温度梯度≤0.1310℃/mm、侧向温度梯度≤0.0325℃/mm,为高精度星敏感器光学系统热控制提供科学的依据。     

Real-time ray-based channel generation and emulation for UAV communications

A real-time ray-based hardware emulator for Unmanned Aerial Vehicle (UAV) communication channels which suits for the Three-Dimensional (3D) dynamic scenarios and considers the movements of both terminals is developed in this paper. The time-variant channel parameters, i.e., ray delay, ray gain, and ray Doppler frequency are precalculated in the host by using the Ray Tracing (RT) method. Meanwhile, RT simulation dramatically increases the number of valid rays. To address the problem of resource limitation and huge computational burden in the implementation, an efficient ray coefficients generation method based on iteration is proposed and implemented. With the advantages of low cost and high flexibility, a Software Defined Radio (SDR) hardware platform is used to emulate the ray-based UAV channels by utilizing the compact architecture including the Time-Division (TD) scheme and Tapped-Delay Line (TDL) for channel convolution. Finally, hardware measurement results demonstrate that the properties of emulated channel, i.e., Power Delay Profile (PDP) and Doppler Power Spectrum Density (DPSD) consist with the simulated ones, which verifies the correctness of hardware implementation. The proposed channel emulator provides an efficient way for optimization, verification, and evaluation of UAV communication systems.     

基于GPU的电磁计算与SAR回波仿真加速方法研究

电磁计算与SAR（Synthetic aperture Radar,合成孔径雷达）回波仿真算法在雷达系统设计、雷达算法验证与目标自动识别算法研究等方面起着重要的作用,针对传统的电磁计算与SAR回波仿真算法耗时过长的问题,本文提出了一种基于GPU（Graphic Processing Unit,图形处理器）的电磁计算与SAR回波仿真全流程加速方法。首先,将传统算法中的三个核心计算部分——射线跟踪、电磁计算与SAR回波仿真进行多线程划分,然后利用GPU通用计算平台,并行处理所有线程单元,加快仿真速度。最后,实验结果表明：该方法相对于单核CPU计算的加速比达到450左右,相对于10核心CPU计算的加速比达到50左右。该方法在保证生成数据与传统算法一致的前提下,实现了良好的加速效果。     

Cosmic Ray Electrons

Modulation of cosmic electrons is similar to that of nuclei, but there are clear differences. At energies below 100 MeV the electron spectrum has a negative slope, which may in some way be related to electrons released from the magnetosphere of the planet Jupiter. If there is such a relationship, its nature is not established, and alternative explanations for the upturn exist. At higher energies, electrons are predominantly negatively charged, and it is probable that the difference in net charge sign from that of nuclei is responsible for many of the observed differences in the behavior of electrons and nuclei under modulation. A consistent picture of the cosmic positron abundance and its time variation may be emerging from the world dataset.     

Time of flight measurements over a radio link from Uppsala to Bruntingthorpe and their application to testing predictions methods that approximate the ray tracing technique

Time of flight measurements (TOF) over the radio link between Uppsala (Tx: 59.9°N, 17.6°E) and Bruntingthorpe (Rx: 52.5°N, 1.1°W) have been performed every 2 min at six frequencies (4.637, 6.954, 8.008, 10.391, 11.118, and 14.364 MHz) during the period November 2006–January 2008. Such measurements have been compared with the TOF provided by three prediction methods that approximate the ray tracing technique: IRI-95, SIRM&BR_D, and ICEPAC. The root mean square deviation (rms) between TOF monthly median measurements and TOF monthly median predictions and the differences (DP) between the length of the median and predicted ray path have been calculated. The results, which are presented in terms of rms and DP for different seasons and different time periods, have indicated that the approximate methods are inadequate and that for more accurate predictions ray tracing techniques should be applied.     

The gamma-ray observatory mission objectives and its significance for gamma-ray astronomy

The Gamma Ray Observatory (GRO) is an approved NASA mission, programmed for launch in 1988. Its complement of four detectors has established goals: 1) to study the nature of compact γ-ray sources such as neutron stars and black holes, or objects whose nature is yet to be understood; 2) to search for evidence of nucleosynthesis especially in the regions of supernovae; 3) to study structural features and dynamical properties of our galaxy; 4) to explore other galaxies, especially the extraordinary types such as radio, Seyferts, and quasars; and 5) to study cosmological effects by examining the diffuse radiation in detail. This paper discusses the design, objectives, and expected scientific results of each of the GRO instruments in view of the GRO mission goals.     

Hard X-ray observations of Cygnus X-1 with the MISO telescope

The black hole candidate Cygnus X-1 was observed in the hard X ray - soft γ ray energy range by the MISO telescope on two different occasions: in September 1979 and May 1980. We have measured two hard X-ray states of the source: in 1979 the observed spectrum confirms the superlow state measured in the same period by the HEAO-3 satellite, while in 1980 the MISO X-ray data are consistent with the so called low state of Cygnus X-1. In both occasions, no γ -ray excess has been observed above 200 KeV.