14.5-14.8 GHz Frequency Sharing by Data Relay Satellite Uplinks and Broadcasting-Satellite Uplinks

Data relay satellites are being developed to provide real-time data links between research satellites in low earth orbits and central data acquisition and processing facilities. Frequency assignments for data relay satellite links will be made in bands allocated internationally to the space research service. One of the bands which will be used lies between 14.5 and 15.35 GHz, where the space research service has had a frequency allocation as a secondary service since 1971. During the General World Administrative Radio Conference of the International Telecommunication Union, held in Geneva in 1979, a primary frequency allocation was made in the band 14.5-14.8 GHz to the fixed-satellite service, specifically for use by earth-to-space links of the broadcasting satellite service. The feasibility of shared band operation is evaluated between data relay satellite uplinks and broadcasting-satellite feeder links in the band 14.5-14.8 GHz. Relationships for predicting interference power levels are formulated, as functions of satellite separation and of earth station separation. Tradeoffs between satellite separation angle and earth station separation are explored, and conclusions are drawn regarding the feasibility of band sharing. Co-channel operation is demonstrated to be technically feasible for typical systems, provided appropriate separations are maintained.     

Geolocation of frequency-hopping transmitters via satellite

An analysis of satellite-communications terminal geolocation performed by means of interception of ground terminal uplink transmissions in which a number of spaceborne interceptors transpond the frequency band of interest to terrestrial location for processing is presented. Interception regions for prototypical terminals and satellites are calculated and the results are presented parametrically as a function of uplink signal-to-noise ratio (SNR). The optimum angular separation of the interceptor satellites is found, and the effect of nonoptimal separation is discussed, as are the practical limitations involved in implementing this geolocation system     

高灵敏GPS接收机抗干扰特性研究

采用圆环阵列天线,利用最小规范算法和线性约束最小方差算法对弱GPS信号的干扰信号进行了抑制,并分别针对固定和可变天线阵元数目以及固定和可变干扰信号等多种情况进行了仿真和分析.GPS信号的功率电平假设为-175dBW,干扰信号的功率值在-100dBW～-140dBW范围内可变.仿真结果表明,圆环天线阵列能精确地判定干扰信号的来波方向,该方法能很好地改善对来波干扰信号的赋零深度.     

镀钴碳纳米管/环氧树脂基复合材料的制备及其微波吸收特性研究

采用化学镀法制备了表面镀钴的多壁碳纳米管，并将其均匀分散在环氧树脂基体中固化成膜，形成镀钴碳纳米管／环氧树脂基复合材料。采用透射电镜、X射线衍射及振动样品磁强计等对镀钴碳纳米管的形貌、微结构与磁性能进行了表征，还采用数字化网络分析仪对该复合材料在0．5～40GHz频段内的微波吸收特性进行了研究。结果表明：在相同的碳管质量分数(1％)和吸波介质层厚度(2．0mm)等条件下，与纯碳纳米管相比，表面镀钴碳纳米管的吸收峰往高频方向移动，吸收强度略有增加，但吸收频带并没有宽化趋势。     

混杂组元低频吸波阵列层板复合材料的吸波性能

采用电磁仿真运算的方法设计了方形和十字形混杂组元低频吸波阵列,采用模压工艺制备了基于混杂组元低频吸波阵列的吸波层板复合材料。研究了各单组元阵列本征吸波特性随单元结构变化的规律和混杂组元低频阵列本征吸收带的叠加效应。吸波性能测试结果表明,不同形状阵列单元的混杂可以有效拓宽阵列的本征吸收带宽,方形和十字形混杂组元阵列为双峰吸收阵列,吸收峰频率分别为3.1与4.5 GHz。混杂组元低频阵列的引入可以有效改善层板低频吸波性能,5 mm厚吸波阵列层板的反射率在2~6 GHz范围内-4.7 d B,6~16 GHz范围内-7 d B,阵列吸波层板的宽频吸波性能显著优于传统的阻抗渐变型吸波层板,阵列吸波层板力学性能与树脂基复合材料层板相当。     

微波在薄层等离子体中传输效应研究

为了准确预测再入飞行过程中等离子体对微波传输特性的影响,采用WKB方法、FDTD方法、平面波理论和薄层等离子体理论4种方法,结合粉末激波管上开展的试验研究了X波段和Ka波段微波在薄层等离子体中的传输效应。对于X波段,试验时激波马赫数为9.6、10.7和10.5;对于Ka波段,试验时激波马赫数为10.5。通过对比与分析获得的主要结论有：当等离子体厚度和入射波波长相近时,薄层等离子体理论计算结果比其它三种方法的计算结果更接近于试验结果;在碰撞频率接近并且电子密度小于临界电子密度的条件下,Ka波段微波信号穿过相同厚度的等离子体比X波段微波信号衰减小得多,具有更强的穿透性;如果等离子体碰撞频率和微波入射频率相同,随着电子密度的增加,微波信号穿过相同厚度的等离子体时衰减变大;当碰撞频率和入射波频率差不多时,共振吸收导致衰减达到最大值。     

球料比对羰基铁粉片型化演变和电磁性能的影响

以无水乙醇为隔离剂,通过湿法球磨制备了片型羰基铁粉,研究了球料比对片型化过程、电磁性能的影响。结果表明：增加球料比,羰基铁粉片型化更充分,晶粒尺寸减小;粒子的各向异性提高了片型羰基铁粉的微波电磁性能。以环氧树脂为基体树脂,填充体积分数30％的吸波剂制备了1．0mm 单层吸波涂层,在 X-Ku 波段反射率小于－7．5dB 的带宽大于10GHz,涂层最小面密度为2．96kg ／m2。     

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.     

Characterization of NAVSTAR GPS and GLONASS on-board clocks

Investigation into navigation satellite on board clock frequency references and performance are reported. The focus is on the stability of the clocks aboard the NAVSTAR GPS (Global Positioning System) and GLONASS satellites as well as those used by their respective maser control stations and associated time scales. Allan-variance techniques have been applied to determine the long-term time-domain behavior of satellite clocks in an attempt to identify different regions of power spectral density. Coupled with analysis of relative-frequency drift over a period of many weeks, this behavior allows the type of satellite onboard standard to be tentatively identified. The known nature of the GPS clocks has shown that the different types of clocks aboard the satellites (crystal, rubidium, and cesium) are distinguishable given a sufficient sample time. The same approach has been applied to the GLONASS satellites, and a comparison of the results obtained from GPS has allowed conjecture on the type of clock used by the GLONASS satellites. It appears that GLONASS has used clocks of the quality of rubidium atomic oscillators since at least 1986, and that the quality and performance of onboard standards have increased steadily with time. Some current satellites perform well enough in terms of frequency drift, flicker FM noise floor, and long-term stability to compare favorably with the cesium beam standards carried on NAVSTAR GPS satellites launched in 1983-84     

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.     

三种纳米碳材料吸波涂层设计及性能

对纳米炭黑(UC)、特导纳米炭黑(L6)、碳纳米管(CNT)三种材料在8～18 GHz波段吸波涂层进行了优化设计及吸波性能分析.结果表明,三种材料的复介电常数随着纳米碳材料质量分数的增加,其实部和虚部均以不同的速度增大.利用理论计算的Cole-Cole图,结合实验测得的复介电常数,求解出这三种材料理想的介电常数,材料的质量分数和吸波涂层的匹配厚度.结果表明,CNT的吸波效果最好,当CNT质量分数为20％涂层、厚度为1.6mm时,反射衰减率在11.2～ 15 GHz均优于-10 dB吸收峰最大值,达到29.6 dB.     

电子回旋共振离子推力器放电室低信号调试

微波输入技术是电子回旋共振离子推力器的关键技术之一,输入微波在推力器放电室内产生谐振的时候,微波功率才能高效地被吸收,从而电离气体,提高电子的能量,增加等离子体的电离度。电子回旋共振离子推力器放电室是一个不规则的微波谐振腔,很难从理论上确定其谐振状态下的结构。本文利用网络分析仪,采用微波无源器件回波损耗的测试方法对放电室进行精确调谐,分析微波谐振频率及带宽,目的在于详细研究放电室的结构尺寸、微波耦合探针形状和尺寸在谐振状态下的匹配性。调试结果表明放电室增加14 mm圆柱段,选择圆柱段长度22 mm和球形直径9 mm的组合探针,可以得到较好的谐振状态,此时腔体的回波损耗为-23 dB,谐振频率4.195 GHz,谐振带宽为0.025 0 GHz,品质因素为167.848。     

Routing in networks of intersatellite links

How to characterize and implement point-to-point (i.e., unicast) routing algorithms is discussed. The characteristics of routing algorithms are first described as well as the specificities of routing in constellations of nongeostationary (NGO) satellites equipped with intersatellite links (ISLs). Then, some of the candidate algorithms displaying the characteristics identified before are simulated and evaluated for different constellations. From the simulation results, it appears that (1) from a routing perspective, constellations are not similar to terrestrial networks, and (2) the constellation geometry has a significant impact on the routing performance.     

Third world radiation threats to satellites

The era of hardening military satellites against nuclear events, lasers, and high-power microwaves, appears to have come to an end. A case is made here for maintaining rudimentary nuclear, laser, and high-power microwave (HPM) hardening requirements in order to protect against developing third world threats. The third world nuclear threat is well known. Less appreciated is the fact that third world laser and microwave threats have changed radically in the past few years     

Susan: A New Doppler Radionavigation System

SUSAN is a novel electronic Doppler navigation system which can be used with moving vehicles including aircraft, missiles, satellites, and ships. The system uses a technique of time delays and frequency multiplication to determine the rates of change of the Doppler frequency component present on a signal received from a moving vehicle. From this information the range and velocity of the vehicle can be determined with respect to a transmitting station whose position or ephemeris is known.     

A low-cost space-based radar system concept

A space-based radar system concept is described that can provide continuous world-wide, all-weather, day-night observation and tracking of ships, aircraft, vehicles and ground facilities of interest. The system employs a constellation of radar satellites in low-earth orbit to provide continuous world-wide target access. The radars employ reflector antennas, TWT transmitters and high frequency (e.g., X band) to achieve long range with relatively low weight, complexity and cost. The radars operate in moving-target-detection (MTD) and synthetic-aperture-radar (SAR) spotlight imaging modes to observe moving and fixed targets, respectively. The system could support a wide range of military, intelligence, law-enforcement and civilian missions     

雷达俯视角对轴对称喷管测试RCS影响研究

为了研究雷达位置以及雷达波段对于轴对称排气系统电磁散射特性的影响，采用步进频率测试系统在暗室中测试了轴对称排气系统的后向雷达散射截面积(RCS)；分析了俯视角对轴对称排气系统后向电磁散射特性的影响。试验结果表明:随着俯视角的增大，轴对称喷管的后向RCS会随之减小，在15°俯视角下排气系统的RCS是0°角下的30%；在不同频段下轴对称喷管的电磁散射特性基本相似。     

Overview of multiple satellite communication networks

Recently interest in packet communications has stimulated an interest in constellations of low altitude satellites. Such a configuration would have less propagation delay and be cheaper to launch than satellites at higher or geosynchronous altitude. However, many more satellites are necessary at low altitude to achieve reasonable coverage of the earth and insure availability of the resource. Further, the geometry of such a constellation would be dynamic with communication links of short duration as the satellites speed past each other or a ground site. The most difficult design issue in these systems is a stable method of routing messages that will sustain a reasonable level of traffic. This paper explores the problems of routing and switching messages through a constellation of low altitude satellites and examines some of the related demands on technology. The dynamic nature of crosslinks, uplinks, and downlinks requires a very agile antenna system, and the volume of information for routing of traffic is overwhelming. Use of some type of facetted phased array antenna is advocated to solve the former problem, but the latter problem is more subtle. Since the volume of ephemeris and constellation data as well as the rate of update is unmanageable, schemes relying on some form of broadcast or random access may be considered. It is concluded that none of the known or examined approaches to routing and switching is completely satisfactory     

一种在紧缩场进行捕获跟踪试验的方法

为满足不断增长的天基中继业务需求,航天器星间链路常使用大口径高增益天线,且配置自动捕获和跟踪设备,以完成对目标航天器的自动跟踪.随着天线口径的增大,对场地空间要求不断增大,地面验证试验变得愈加困难.针对越来越难以实现的捕获跟踪外场试验,提出一种在紧缩场进行捕获跟踪试验的方案,方案详细分析了在紧缩场进行试验的可行性.通过设置跟踪通道校相因子,很好地分离了角误差信号,获得良好的S曲线以及非常小的交叉耦合,从而验证了在紧缩场进行捕获跟踪试验是可行的.相对于传统的远场测试方法,该方法具有不受气候影响、费用低等优点.     

ATS-6 Technical Aspects of the Health/Education Telecommunications Experiment

The Health/Education Telecommunications (HET) Experiment involved six different experiments conducted under the auspices of the Department of Health, Education, and Welfare (HEW) with technical assistance from NASA. The HET Experiment on ATS-6 was operated and controlled from a network coordination center in Denver, Colo., which included a 4-and 6-GHz Earth station. The HET Experiment used remote Earth terminals with 3-m-diameter dishes having a 35 dB gain at 2.5 GHz. In addition, comprehensive terminals operating at both C-band and S-band were used for communications with Alaska. The total network involved a complex of satellite and land links at C-band, S-band, and very high frequency (VHF), using the ATS-1, ATS-3, and ATS-6 satellites. The network performance exceeded expectations with remote terminal operations exhibiting a peak-to-peak signal to weighted rms noise ratio of 49 dB at least 99 percent of the time. The remote site operators performed well and were well motivated although they had little previous technical experience.