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。     

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.     

Satellite proximate interception vector guidance based on differential games

This paper studies the proximate satellite interception guidance strategies where both the interceptor and target can perform orbital maneuvers with magnitude limited thrusts. This problem is regarded as a pursuit-evasion game since satellites in both sides will try their best to capture or escape. In this game, the distance of these two players is small enough so that the highly nonlinear earth-centered gravitational dynamics can be reduced to the linear Clohessy-Wiltshire (CW) equations. The system is then simplified by introducing the zero effort miss variables. Saddle solution is formulated for the pursuit-evasion game and time-to-go is estimated similarly as that for the exo-atmospheric interception. Then a vector guidance is derived to ensure that the interception can be achieved in the optimal time. The proposed guidance law is validated by numerical simulations.     

ATS-6 Radio Frequency Interference Measurement Experiment

The frequency band from 5.925 to 6.425 GHz is served by fixed satellites and by terrestrial microwave links. There is a possibility of microwave links pointed at the horizon causing interference to the uplinks of domestic and international communications satellites sharing the same frequency band. A mathematical model has been derived for predicting the fields at geostationary orbit based on the known characteristics and known distribution of the terrestrial microwave relay system. The Applications Technology Satellite-6 (ATS-6) is sensitive to signals in the range of 10 dBW radiated in the direction of the satellite. Signals in the range of 10-30 dBW have been recorded over various parts of the United States.     

认知无线电网络中基于几何规划的分布式功率控制

功率控制对于允许次用户和主用户之间频谱共享的认知无线电网络来说是关键的,针对具有干扰限制的认知网络最大总容量得到一种最优的分步式功率控制策略,对于系统效用的非凸性,引入几何规划把非凸最优化问题转换为凸最优化问题,引入辅助变量和额外等式约束,把效用之间的关联转化为约束之间的关联,提出了功率控制策略的解决方法,显示了整体最...     

三星定位原理研究

双星定位系统只需要两颗同步卫星便可以为用户提供定位服务,但却存在着用户位置易暴露和用户数量易饱和这两大缺陷。建议采用三颗同步导航卫星像GPS卫星那样向用户播发导航电文,用户接收机根据这些导航电文信息以及气压高度表信息,像GPS接收机那样解算用户位置,从而克服了双星定位的两大缺陷。仿真表明本定位原理行之有效。     

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。     

Optimal Terminal Rendezvous as a Stochastic Differential Game Problem

The optimal terminal rendezvous of two satellites in orbit about the Earth is studied using a stochastic model and formulating the rendezvous as a game problem. Each satellite has noise-corrupted output measurements and uses a Kalman filter to generate the best estimate of the states describing the rendezvous. The optimal control for the satellites is determined. A comparison is made in terms of dimensionality and complexity to a deterministic solution of the rendezvous problem.     

基于多机协作的认知无人机网络能效联合优化

针对无人机（UAV）通信网络中频谱资源紧缺的问题,构建基于认知无线电的多无人机通信网络,通过多机协作频谱感知有效探索授权频谱。提出一种基于Bisection算法的迭代算法,通过联合优化感知时间和判决门限对构建的复杂非凸问题求解,显著提高了无人机次级认知网络的能量效率（EE）。分析了无人机飞行过程中能效的变化情况,仿真结果表明,存在最优感知时间使能效获得最大值,且判决门限的选择会影响该能效最优值;提出的高能效迭代算法具有较好收敛性,有效提高了认知无人机网络的能量利用率。     

耦合均衡论和隐式约束伴随方法的翼型气动多目标优化设计

通过耦合Nash竞争对策和伴随方法来研究气动多目标优化问题,其中对策论是描述现实世界中包含有矛盾、冲突、对抗、合作等诸因素的数学模型的数学理论与方法。将对策论的方法应用于互为冲突的多目标气动优化设计中,寻找各冲突目标之间的平衡解。计算结果表明：Nash均衡论可以很好地处理多目标优化问题,并且能自然地运用于并行环境。     

近地卫星严格回归轨道保持控制

研究了近地卫星基于严格回归参考轨道的轨道保持控制方法：将卫星编队理论引入单星绝对轨道保持控制,提出了"虚拟卫星编队"的概念,分析了卫星轨道相对于参考空间轨迹在轨道摄动情况下的偏离状态及变化趋势,然后根据卫星编队相对运动学,推导出了偏离状态与虚拟卫星编队构形参数之间的对应关系,并设计了以轨道参数超调、偏置及阈值触发为特征的管道保持控制策略。数值仿真结果表明,使用该控制策略能够将卫星轨道保持在以空间参考轨迹为中心的轨道管道内,并且有效减少了因周期性轨道摄动波动造成的管道保持控制量和控制频次。研究成果对于有空间轨迹回归要求的卫星轨道保持控制具有指导意义。     

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。     

Photoelectron Counting Statistics and Error Performance of m-Distributed Optical Signal

By the term "m-distributed optical signal" we mean a noise-like optical signal whose envelope (or intensity) fluctuation probability is modeled by Nakagami's "m-distribution." Using the m-distribution which has been widely used as an analytical model of the fading envelope in radio communications, it is shown that one can generally analyze the statistical properties such as the photoelectron count probabilities and error probabilities for the wider class of noise-like optical signals; some numerical results are also given.     

21世纪AMSS／GNSS空间段发展方向兼论卫星资源国际共享问题

航空移动卫星系统（ＡＭＳＳ）空间段采用单一的ＧＥＯ轨道卫星，未来将有ＭＥＯ和ＬＥＯ轨道卫星加入运行，仍然不排斥ＧＥＯ轨道卫星的使用。全球导航卫星系统（ＧＮＳＳ）空间段采用ＭＥＯ轨道卫星，未来将仍然以ＭＥＯ为主，可能有ＨＥＯ轨道卫星加入运行。２１世纪的空间段将为不同轨道卫星的多星座组合，采用一星多用、星座共用，形成多功能卫星和多功能星座。和平时期卫星资源的国际民间共建共营共享将更为普遍，要有全球观点，国内各行各业要有全局观点，对监测和增强系统统一筹建共用系统，防止分散投资、重复建设     

Urban area performance of GPS receiver with simultrac capability

The theory of operation, practical applications, and technical performance of a Global Positioning System (GPS) receiver designed for urban area use are presented. The receiver tracks as many as eight satellites, or all visible satellites, and uses the signals of the four best satellites to ascertain its location. If visibility of one satellite is blocked, one of the additional satellites can be used to provide continuous navigation. Component-level system design choices are shown to support superior automotive vehicle location performance, including optimum mobile communication with satellites and ground-based relays     

Type IV solar radio emission

Conclusion We have got a reasonably clear idea of the various forms under which the type IV continuum emission may appear. Also we can imagine what kind of processes come into play during a type IV event. But the insight gained so far applies to the general case. Individual cases are widely different, and we are still far from understanding why a given event behaves as it does. For instance, why are metric responses lacking at a certain big microwave outburst, or why is the decimetric component particularly strong or prolonged on certain occasions? One can imagine that such questions would receive an answer if one were allowed to see the configuration of magnetic lines of force above the activity region !Does the type IV event tell us a fine story of the interplay of energetic particles and streams of particles with coronal magnetic fields ? Maybe the story would be a fine one if the language could be understood. At present we know only a few words of it; for this reason to us the story is very fragmentary. First of all, however, the message should be recorded far more completely than has been done so far. The number of observations that should be made of one and the same event is tremendous; the program comprises:1) spectral observations from 1000 Mc/s down to the lowest frequencies; 2) single frequency observations at a great many wavelengths covering the whole radio spectrum; 3) measurements of polarization and 4) determinations of position and angular extent in at least every octave of the whole radio spectrum.Especially as regards the latter two points, the present situation is still very unsatisfactory, though good work has been done already in Japan. The realization of a complete recording of phenomena during a type IV event calls for a combined effort of several observatories.Very encouraging are the established relations between solar type IV events and terrestrial phenomena. From an analysis of solar cosmic ray events as recorded on several places on the earth, interesting inferences have been drawn regarding the travelling conditions of particles in interplanetary space (cf. Carmichael, 1962). Likewise, one may expect interesting information on the behaviour of interplanetary particle clouds of solar origin from (interferometric) observations of decametric radio emission on the occasion of type IV events.The occurrence of a major type IV event enables forecasters to predict successfully geomagnetic and ionospheric storms. Type IV events will determine at what times certain space research experiments will be launched in the next solar cycle. One should like to be able to indicate the probability for the occurrence of type IV solar radio flares themselves. It is known that these flares generally occur in complex sunspot groups; but a complex sunspot group does not of necessity imply the occurrence of a type IV flare. Observations of coronal condensations at microwave frequencies with a high resolution interferometer may help sorting out those centres of activity that are most likely to produce type IV flares.     

Photoemission Phenomena in the Solar System

Much of what we know about the atmospheres of the planets and other bodies in the solar system comes from detection of photons over a wide wavelength range, from X-rays to radio waves. In this chapter, we present current information in various categories—measurements of the airglows of the terrestrial planets, the dayglows of the outer planets and satellites, aurora throughout the solar system, observations of cometary spectra, and the emission of X-rays from a variety of planetary bodies.     

A Concept of Position Fixing by a Passive Mode Navigation Satellite System

A position fix in a passive mode using satellites usually necessitates an expensive computer or lengthy hand calculation. This is the largest drawback of passive navigation and it would be more desirable if the user could find his position by a mere glance at a chart and table, as one uses Loran. The first step toward this goal is to use a synchronous satellite because it simplifies the problem. The next step is to find the position of the user by a Loran type of chart, which is universal, and correct this apparent position by looking at a special table which is made according to the amount of perturbation of both the satellite and the user's position. An example of the position fix along the route between Yokohama to Hawaii is shown. The concept can be extended to orbiting satellites due to the rules which govern the motion of satellites, if the fix accuracy is in the order of 2 to 5 miles. This method should be more accurate than the common sextant and more practical due to the fact that the satellite can be used at any time and in any weather. As a total system, it will be better than Omega because it could provide additional navigation information such as communication or traffic control by using satellites.     

The Juno Gravity Science Instrument

The Juno mission’s primary science objectives include the investigation of Jupiter interior structure via the determination of its gravitational field. Juno will provide more accurate determination of Jupiter’s gravity harmonics that will provide new constraints on interior structure models. Juno will also measure the gravitational response from tides raised on Jupiter by Galilean satellites. This is accomplished by utilizing Gravity Science instrumentation to support measurements of the Doppler shift of the Juno radio signal by NASA’s Deep Space Network at two radio frequencies. The Doppler data measure the changes in the spacecraft velocity in the direction to Earth caused by the Jupiter gravity field. Doppler measurements at X-band (\(\sim 8\) GHz) are supported by the spacecraft telecommunications subsystem for command and telemetry and are used for spacecraft navigation as well as Gravity Science. The spacecraft also includes a Ka-band (\(\sim 32\) GHz) translator and amplifier specifically for the Gravity Science investigation contributed by the Italian Space Agency. The use of two radio frequencies allows for improved accuracy by removal of noise due to charged particles along the radio signal path.     

Thermal Evolution and Magnetic Field Generation in Terrestrial Planets and Satellites

Of the terrestrial planets, Earth and Mercury have self-sustained fields while Mars and Venus do not. Magnetic field data recorded at Ganymede have been interpreted as evidence of a self-generated magnetic field. The other icy Galilean satellites have magnetic fields induced in their subsurface oceans while Io and the Saturnian satellite Titan apparently are lacking magnetic fields of internal origin altogether. Parts of the lunar crust are remanently magnetized as are parts of the crust of Mars. While it is widely accepted that the magnetization of the Martian crust has been caused by an early magnetic field, for the Moon alternative explanations link the magnetization to plasma generated by large impacts. The necessary conditions for a dynamo in the terrestrial planets and satellites are the existence of an iron-rich core that is undergoing intense fluid motion. It is widely accepted that the fluid motion is caused by convection driven either by thermal buoyancy or by chemical buoyancy or by both. The chemical buoyancy is released upon the growth of an inner core. The latter requires a light alloying element in the core that is enriched in the outer core as the solid inner core grows. In most models, the light alloying element is assumed to be sulfur, but other elements such as, e.g., oxygen, silicon, and hydrogen are possible. The existence of cores in the terrestrial planets is either proven beyond reasonable doubt (Earth, Mars, and Mercury) or the case for a core is compelling as for Venus and the Moon. The Galilean satellites Io and Ganymede are likely to have cores judging from Galileo radio tracking data of the gravity fields of these satellites. The case is less clear cut for Europa. Callisto is widely taken as undifferentiated or only partially differentiated, thereby lacking an iron-rich core. Whether or not Titan has a core is not known at the present time. The terrestrial planets that do have magnetic fields either have a well-established inner core with known radius and density such as Earth or are widely agreed to have an inner core such as Mercury. The absence of an inner core in Venus, Mars, and the Moon (terrestrial bodies that lack fields) is not as well established although considered likely. The composition of the Martian core may be close to the Fe–FeS eutectic which would prevent an inner core to grow as long as the core has not cooled to temperatures around 1500 Kelvin. Venus may be on the verge of growing an inner core in which case a chemical dynamo may begin to operate in the geologically near future. The remanent magnetization of the Martian and the lunar crust is evidence for a dynamo in Mars’ and possibly the Moon’s early evolution and suggests that powerful thermally driven dynamos are possible. Both the thermally and the chemically driven dynamo require that the core is cooled at a sufficient rate by the mantle. For the thermally driven dynamo, the heat flow from the core into the mantle must by larger than the heat conducted along the core adiabat to allow a convecting core. This threshold is a few mW?m^?2 for small planets such as Mercury, Ganymede, and the Moon but can be as large as a few tens mW?m^?2 for Earth and Venus. The buoyancy for both dynamos must be sufficiently strong to overcome Ohmic dissipation. On Earth, plate tectonics and mantle convection cool the core efficiently. Stagnant lid convection on Mars and Venus are less efficient to cool the core but it is possible and has been suggested that Mars had plate tectonics in its early evolution and that Venus has experienced episodic resurfacing and mantle turnover. Both may have had profound implications for the evolution of the cores of these planets. It is even possible that inner cores started to grow in Mars and Venus but that the growth was frustrated as the mantles heated following the cessation of plate tectonics and resurfacing. The generation of Ganymede’s magnetic field is widely debated. Models range from magneto-hydrodynamic convection in which case the field will not be self-sustained to chemical and thermally-driven dynamos. The wide range of possible compositions for Ganymede’s core allows models with a completely liquid near eutectic Fe–FeS composition as well as models with Fe inner cores or cores in with iron snowfall.