Relationships between energetic storm particle events and interplanetary shocks driven by full and partial halo coronal mass ejections

We have analysed energetic storm particle (ESP) events in 116 interplanetary (IP) shocks driven by front-side full and partial halo coronal mass ejections (CMEs) with speeds $>$400 km s^?1during the years 1996–2015. We investigated the occurrence and relationships of ESP events with several parameters describing the IP shocks, and the associated CMEs, type II radio bursts, and solar energetic particle (SEP) events. Most of the shocks (57 %) were associated with an ESP event at proton energies $>$1 MeV.The shock transit speeds from the Sun to 1 AU of the shocks associated with an ESP event were significantly greater than those of the shocks without an ESP event, and best distinguished these two groups of shocks from each other. The occurrence and maximum intensity of the ESP events also had the strongest dependence on the shock transit speed compared to the other parameters investigated. The correlation coefficient between ESP peak intensities and shock transit speeds was highest (0.73 $\pm$ 0.04) at 6.2 MeV. Weaker dependences were found on the shock speed at 1 AU, Alfvénic and magnetosonic Mach numbers, shock compression ratio, and CME speed. On average all these parameters were significantly different for shocks capable to accelerate ESPs compared to shocks not associated with ESPs, while the differences in the shock normal angle and in the width and longitude of the CMEs were insignificant.The CME-driven shocks producing energetic decametric–hectometric (DH) type II radio bursts and high-intensity SEP events proved to produce also more frequently ESP events with larger particle flux enhancements than other shocks. Together with the shock transit speed, the characteristics of solar DH type II radio bursts and SEP events play an important role in the occurrence and maximum intensity of ESP events at 1 AU.     

测量船通信网络自检测方法

针对测量船通信网络由2层帧方式交换升级为3层包交换方式后无法使用上星自环检测方式实现自检测的问题,在分析通信网络自检测模式下的链路特性的基础上,提出基于组播报文实现自检测的构想。设计利用组播洪泛特性实现报文环回的网络拓扑结构以及实现检测与对比报文的硬件设备,阐述检测软件发送、接收、处理报文的流程,实现了网络通断、时延及丢包率的自检测,并通过模拟检测实验证明了设计方案是切实可行的。     

能量和协方差检验的联合频谱感知算法研究

快速准确的频谱感知是认知无线电系统有效通信的前提。现有的能量检测算法易受噪声波动影响,为提高频谱感知的性能,采用了联合频谱感知算法。方法利用双门限的能量检测法进行粗检,并使用协方差检测算法对中间混淆区域进行二次判决。在噪声不确定的情况下,对联合频谱感知算法性能进行了仿真分析。仿真结果表明,在噪声波动较大时,算法有效地提高频谱检测的性能,而且计算复杂度得到降低,并优于能量检测法和协方差检测法。     

NOVEL HIGH-SPEED FPGA-BASED FFT PROCESSOR

A novel architecture for computing the fast Fourier transform ( FFT ) on programmable devices is presented.To improve the system operation speed , a hybrid parallel FFT algorithm is used.Results indicate that the use of an 8×8parallel structure for realizing the 64-point FFT leads to a 8times higher processing speed compared with its counterparts employing other series of techniques.     

基于无线通信的城市路灯监控系统

通过多种通信技术和计算机对城市路灯实现集中监控，监督级、监控级与现场控制级形成三级分布式计算机控制系统。监督级与监控级之间通过Intranet／Internet交互；监控级与现场控制级之间采用无线电台、GPRS及SMS等多种通信技术。     

Difficulties in the study of cosmic radio noise absorption at 30 MHz using riometer at low latitude station,Kolhapur (Lat-16.8°N,Long-74.25°E)

A dual dipole antenna has been installed at low latitude station Kolhapur (Geographic 16.8°N, 74.25°E), Maharashtra, India for the study of cosmic radio noise absorption using Solid State Riometer (which operates at 30 MHz) during pre phase of 24th solar maxima. The aim for this type of study over Kolhapur was to know the response of lower (D region) ionosphere over low latitude by cosmic radio noise absorption using riometer technique during quite period as well as sudden ionospheric disturbances (SID). The observations are being taken for 3 years. Two different sites (∼40 km away from each other) were used for the installation of riometer equipment assuming minimum local noise. It is found that solar noise to cosmic radio noise hence resulting in signal saturation. The night time signal is relatively free of interference but sometimes local noise is responsible for spike-like signatures. Hence it is concluded that Kolhapur (a low latitude station) is not suitable for the study of cosmic radio noise absorption on 30 MHz with riometer and dual dipole antenna. Proper choice for operating frequency of riometer and antenna gain is suggested for low latitude use of this technique for ionospheric deviative and nondeviative absorption studies.     

The beginning of cosmic ray astrophysics

A short history of the beginning of cosmic ray (CR) astrophysics is considered: from the hypothesis on CR origin as a result of Supernova explosions in the Metagalaxy, to a model of solar origin of CR, galactic origin based on the stochastic mechanism of charged particle acceleration in interstellar space, to extragalactic and hierarchical models of CR origin, as well as galactic CR origin taking into account radio-astronomical data. We consider also the first balloon results on the chemical contents of primary CR (especially of the contents Li, Be, B), important for any model of CR origin. Investigations of the injection problem, CR drift and diffusion acceleration by shock waves, and CR generation in Supernova remnants were also important steps in the beginning of CR astrophysics.     

基于随机时隙的RFID读写器防冲突方法

针对密集读写器环境下的无线射频识别(RFID,Radio Frequency Identification)多读写器冲突情况,提出了一种基于随机时隙并通过中央计算机协调的读写器防冲突方法.首先,中央计算机发送每轮起始命令和时隙指令,读写器根据当前利用率随机选择时隙.选择当前时隙的读写器若没有接收到忙信号则发送信标并侦听,若无邻近读写器发送信标则开始读写标签,否则该轮回停止工作.若时隙末存在没有接收到忙信号的读写器则在额外时隙发送二次信标.与现有的分布式防冲突方法相比,该方法具有较好的吞吐量和公平性.     

First millimetric detections of AE Aquarii

We report the first millimetric detections of the magnetic cataclysmic variable AE Aquarii, accompanied by contemporaneous microwave observations. These data show that the time-averaged spectrum is well fit by a power-law which extends to mm wavelengths. We suggest that the spectrum is consistent with that expected from a superposition of flare-like events.     

通信系统电磁兼容性设计

一个设计不好的无线电发射机, 工作时产生的谐波十分严重, 而接收设备又对电磁干扰非常敏感。本文介绍了发射机谐波的抑制方法和接收机抗干扰技术体制, 实现自适应通信, 确保通信质量。