Unlicensed Spectrum Sharing Game Between LEO Satellites and Terrestrial Cognitive Radio Networks

By cognitive radio,the low Earth orbit(LEO) satellites may prefer to operate in the unlicensed spectrum which is open to all the users,and compete for the limited resources with terrestrial cognitive radio networks(CRNs).The competition can be regarded as a game and analyzed with game theory.This particular unlicensed spectrum sharing problem is modeled here,and the special properties of "spatially-distinguished-interference" and the short period of the interactions between satellites and terrestrial CRNs are explored.Then,the problem is formulated as a "partially-blind" finitely repeated prisoner’s dilemma by game theory.Finally,we begin with two promising spectrum sharing schemes,which can be used to enforce the frequency reuse among the remotely located terrestrial CRN players as well as to overcome the observation noise.By analysis and comparison,it is proposed that the novel refreshing-contrite-tit-for-tat(R-CTFT) is the optimal spectrum sharing scheme.Simulation results verify that it can be used to utilize the spectrum most efficiently.     

机载调频无线电高度表敏感特性分析

在国际国内频谱资源有限性、稀缺性日益凸显的大背景下,多种业务共用频段已是必然。通过试验和仿真分析方法研究机载调频无线电高度表对雷达脉冲信号的敏感特性,期望实现二者的同频段共用。研究结果表明,处于同一频段的雷达脉冲信号会对机载调频无线电高度表产生有害干扰,雷达脉冲信号会影响高度表指示,使高度表示值不断增大直至满刻度,从而危及飞行安全。     

Electromagnetic Spectrum Control Programs

The radio frequency spectrum is becoming increasingly saturated and polluted due to intensified use and unnecessary radiations and is being taxed severely to meet man's communications-electronics needs. Additional corrective measures are necessary-improved standards, increased concern for conservation of the resource, greater emphasis on intersystems compatibility, increased research, better educational and training programs, and the inclusion of economic and social values in evaluating the uses to which the spectrum should be put.     

Thermal cyclotron radiation from a hot coronal loop with helical magnetic field

The spectral and polarization properties of thermal cyclotron radio emission from a hot coronal loop with a current along the axis are computed. The magnetic field is supposed to have a component along the loop axis as well as a poloidal part due to the current, both components being of comparable magnitude. In this specific configuration a helical magnetic field is present with a remarkable minimum of its absolute value along the loop axis and a maximum at its periphery. The presence of one or two maxima of magnetic field value along the line of sight results in increasing optical thickness of the gyroresonance layers at appropriate frequencies in the microwave band and, therefore, in enhanced radio emission at those harmonics which are optically thin (for example,s=4). These cannot be observed in models with the commonly employed magnetic field configuration (longitudinal along the loop axis).We show that the frequency spectrum of thermal cyclotron radiation from a hot coronal loop with a helical magnetic field differs from that of the standards-component source (with smooth frequency characteristics and polarization corresponding toe-mode) in that plenty of fine structures (line-like features and cut-offs) are present and theo-mode is prevalent in some frequency intervals. The enhanced radio emission at high harmonics and the complicated form of frequency spectrum in the model considered imply that some microwave sources, which are poorly explained in traditional models of solar active regions, may be associated with helical magnetic fields in hot coronal loops. Computations allow one to indicate spectral and polarizational peculiarities of local sources testifying to the presence of a helical magnetic field.     

Delay?Lock Repeater Tracking System Utilizing Superregenerative Interrogator

A unique delay?lock tracking system is described. The system includes an interrogator and a repeater operating on the same radio frequency, with a pulse repetition rate which is related to the distance. Single radio frequency operation allows utilization of a superregenerative radio frequency stage, which serves as both the receiver and the transmitter of the interrogator unit.     

空间信息网络中面向双卫星的频谱共享方法

认知无线电能为缓解空间信息网络中日益增长的服务需求与紧张的频谱资源之间的矛盾提供有效的解决途径。论文针对静止轨道卫星系统和低轨道卫星系统提出一种基于频率动态分配的频谱共享方法。基于用户信号质量最差场景的干扰分析,定义波束隔离区域以避免同频干扰。此外,针对卫星运动引起的时空动态性,通过卫星星历、频率配置方案以及天线方向图等共享信息来预测可能出现的干扰,在此基础上提出频率动态分配算法来实现频谱共享。仿真结果表明,频谱共享方法在保护主用户的同时可有效提高次级用户的信号质量。     

无线电引信抗海杂波干扰方法

无线电引信抗海杂波的能力决定了舰空导弹无线电引信低空和超低空工作性能,针对海杂波对无线电引信的影响,分析了海面回波的平均功率、海面散射系数、海杂波的多普勒频谱等海杂波特性,提出了无线电引信抗海杂波干扰方法。     

宽带综合射频前端三种实施方案

首先描述了军机上射频传感器的现状，介绍了综合射频收发机三种实施方案及其优缺点和应用，其次针对各种不同实施方案存在的缺点给出了改进措施，最后给出了未来综合射频前端的发展趋势及努力方向。 [关键词] 综合射频前端技术；发射机；接收机；中频架构；零中频；数字收发机     

Very Long Baseline Interferometry: Dependencies on Frequency Stability

Very Long Baseline Interferometry (VLBI) is a differential technique observing radiation of compact extra-galactic radio sources with pairs of radio telescopes. For these observations, the frequency standards at the telescopes need to have very high stability. In this article we discuss why this is, and we investigate exactly how precise the frequency standards need to be. Four areas where good clock performance is needed are considered: coherence, geodetic parameter estimation, correlator synchronization, and UT1 determination. We show that in order to ensure the highest accuracy of VLBI, stability similar to that of a hydrogen maser is needed for time-scales up to a few hours. In the article, we are considering both traditional VLBI where extra-galactic radio sources are observed, as well as observation of man-made artificial radio sources emitted by satellites or spacecrafts.     

面向L波段导航监视功能的波形兼容管理技术研究

随着射频综合技术的发展,各射频功能之间的耦合性越来越高,对其兼容管理的需求越来越大。本文基于某型综合射频系统项目,针对L波段通用波形的兼容管理开展了技术论证和研究。结果表明,该射频兼容管理措施可以有效保证L波段导航监视功能波形正常工作。     

The Lightning And Radio Emission Detector (LRD) instrument

The Lightning and Radio Emission Detector (LRD) instrument will be carried by the Galileo Probe into Jupiter's atmosphere. The LRD will verify the existence of lightning in the atmosphere and will determine the details of many of its basic characteristics. The instrument, operated in its magnetospheric mode at distances of about 5, 4, 3, and 2 planetary radii from Jupiter's center, will also measure the radio frequency (RF) noise spectrum in Jupiter's magnetosphere. The LRD instrument is composed of a ferritecore radio frequency antenna ( 100 Hz to 100 kHz) and two photodiodes mounted behind individual fisheye lenses. The output of the RF antenna is analyzed both separately and in coincidence with the optical signals from the photodiodes. The RF antenna provides data both in the frequency domain (with three narrow-band channels, primarily for deducing the physical properties of distant lightning) and in the time domain with a priority scheme (primarily for determining from individual RF waveforms the physical properties of closeby-lightning).     

射频识别技术在实验室收费系统中的应用

基于ISO14443A国际标准的射频识别技术已经成熟,并得到广泛应用.为此介绍了射频识别技术在实验室收费系统中的应用,给出了射频卡系统的工作原理,详细探讨了Mifare射频卡的结构和特点,并根据实验室收费系统的实际需要,实现了下位机射频卡读写器的软硬件设计和上位机实验室收费系统的设计,最后对系统进行了结果分析.     

月球探测器天文测角/单程无线电时间差分测距/差分测速导航方法

月球探测器高精度导航技术是确保月球探测任务顺利实施的关键技术之一。当前,大多数月球探测器都是利用地面无线电进行导航和控制,但存在可测控弧段短、易受干扰等局限性,且对于月球背面探测,存在无法直接测控的不足。针对上述问题,提出了一种新的基于天文测角/单程无线电差分测距/差分测速的月球探测器组合导航方法。该方法使用了天文星光角距、探测器接收到的来自地面站或中继星的单程无线电时间差分测距和时间差分多普勒测速3种量测信息,可有效抑制星上时钟和频谱仪的时间和频率测量误差。收敛后的平均位置和速度估计误差分别为902.7 m和0.12 m/s,最大的位置和速度估计误差分别为1 548.2 m和0.24 m/s。仿真分析结果表明该方法具有较高自主导航精度。     

认知无线网络及其频谱管理技术

认知无线网络通过不同种类的无线网络体系结构之间的并存和动态频谱接入技术可以为移动用户提供高带宽的服务。高效的频谱管理技术是这一新型网络面临的主要挑战之一。为了更好的理解认知无线网络,文章简单回顾了认知无线电技术,对认知无线网络的结构及特点进行了深入研究,明确了认知无线网络频谱管理的主要任务,并结合认知无线电当前的发展状况对认知无线网络频谱管理技术进行了总结分析。     

The Advent of Land Mobile Satellite Service Systems

The practicality of providing cellular-type communications service to underserved remote areas of the country is now possible through the use of satellites in geostationary orbit. The advent of high-power, land-mobile satellites, coupled with high-performance, low-cost ground receivers, makes it possible to provide mobile radio, mobile telephone, data communication, and other services to large numbers of rural and suburban users. A recent Federal Communications Commission (FCC) decision has allocated L-band (1.5 GHz, 1.6 GHz) spectrum to this service. Even though there is a significant amount of spectrum available at L-band, the expected demand for this service is high and spectral efficient means must be devised to maintain sufficient capacity. Expedient means used to increase capacity, in the absence of additional spectrum, are single channel per carrier, demand assignment multiple access (SCPC-DAMA) with voice, frequency reuse via multiple beams, and orbital reuse by using multiple satellites. Some of the operational, systemic, and technological considerations of the first generation land mobile satellite service (LMSS) that would provide thin-route services to large land masses of North America are considered here.     

The Cassini Radio and Plasma Wave Investigation

The Cassini radio and plasma wave investigation is designed to study radio emissions, plasma waves, thermal plasma, and dust in the vicinity of Saturn. Three nearly orthogonal electric field antennas are used to detect electric fields over a frequency range from 1 Hz to 16 MHz, and three orthogonal search coil magnetic antennas are used to detect magnetic fields over a frequency range from 1 Hz to 12 kHz. A Langmuir probe is used to measure the electron density and temperature. Signals from the electric and magnetic antennas are processed by five receiver systems: a high frequency receiver that covers the frequency range from 3.5 kHz to 16 MHz, a medium frequency receiver that covers the frequency range from 24 Hz to 12 kHz, a low frequency receiver that covers the frequency range from 1 Hz to 26 Hz, a five-channel waveform receiver that covers the frequency range from 1 Hz to 2.5 kHz in two bands, 1 Hz to 26 Hz and 3 Hz to 2.5 kHz, and a wideband receiver that has two frequency bands, 60 Hz to 10.5 kHz and 800 Hz to 75 kHz. In addition, a sounder transmitter can be used to stimulate plasma resonances over a frequency range from 3.6 kHz to 115.2 kHz. Fluxes of micron-sized dust particles can be counted and approximate masses of the dust particles can be determined using the same techniques as Voyager. Compared to Voyagers 1 and 2, which are the only spacecraft that have made radio and plasma wave measurements in the vicinity of Saturn, the Cassini radio and plasma wave instrument has several new capabilities. These include (1) greatly improved sensitivity and dynamic range, (2) the ability to perform direction-finding measurements of remotely generated radio emissions and wave normal measurements of plasma waves, (3) both active and passive measurements of plasma resonances in order to give precise measurements of the local electron density, and (4) Langmuir probe measurements of the local electron density and temperature. With these new capabilities, it will be possible to perform a broad range of studies of radio emissions, wave-particle interactions, thermal plasmas and dust in the vicinity of Saturn.DeceasedThis revised version was published online in July 2005 with a corrected cover date.     

基于DRFM技术的雷达标校器设计与实现

建立了基于数字射频存储器技术构建雷达标校器的方法.该雷达标校器可灵活实现目标运动模拟、多普勒频率加载、目标RCS模拟、多目标模拟等功能,较传统的基于光纤延迟实现的雷达标校器更具有应用价值.针对实际应用需求提出了解决频率捷变的方案,给出了典型模拟策略所需数学模型.应用研究表明,基于数字射频存储器技术的雷达标校器具有较强的...     

《无线个域网技术及应用》探析

无线个域网技术主要有红外技术、家庭射频、蓝牙、ZigBee、超带宽和射频识别等,分析了它们的主要特点、发展现状和应用领域,最后阐述了它们的融合发展趋势。     

Satellite observations of type III solar radio bursts at low frequencies

Type III solar radio bursts have been observed from 10 MHz to 10 kHz by satellite experiments above the terrestrial plasmasphere. Solar radio emission in this frequency range results from excitation of the interplanetary plasma by energetic particles propagating outward along open field lines over distances from 5 R to at least 1 AU from the Sun. This review summarizes the morphology, characteristics and analysis of individual as well as storms of bursts. Substantial evidence is available to show that the radio emission is observed at the second harmonic instead of the fundamental of the plasma frequency. This brings the density scale derived by radio observations into better agreement with direct solar wind density measurements at 1 AU and relaxes the requirement for type III propagation along large density-enhanced regions. This density scale with the measured direction of arrival of the radio burst allows the trajectory of the exciter path to be determined from 10 R to 1 AU. Thus, for example, the dynamics and gross structure of the interplanetary magnetic field can be investigated by this method. Burst rise times are interpreted in terms of exciter length and dispersion while decay times refer to the radiation damping process. The combination of radio observations at the lower frequencies and in-situ measurements on non-relativistic electrons at 1 AU provide data on the energy range and efficiency of the wave-particle interactions responsible for the radio emission.     

Hectometric and kilometric solar radio emission observed from satellites in August 1972

Type II, III, and continuum solar radio events, as well as intense terrestrial magnetospheric radio emissions, were observed at low frequencies (10 MHz to 30 kHz) by the IMP-6 satellite during the period of high solar activity in August 1972. This review covers briefly the unique direction finding capability of the experiment, as well as a detailed chronology of the low frequency radio events, and, where possible, their association with both groundbased radio observations and solar flares. The attempted observation of solar bursts in the presence of intense magnetospheric noise may, as illustrated, lead to erroneous results in the absence of directional information. The problem of assigning an electron density scale and its influence on determining burst trajectories is reviewed. However, for the disturbed conditions existing during the period in question, we feel that such trajectories cannot be determined accurately by this method. In conclusion, the capabilities, limitations, and observing programs of present and future satellite experiments are briefly discussed.