卫星微波信标天线与地面站引导雷达圆锥扫描天线的极化失配分析

目标信号和雷达天线之间的极化失配,导致接收机输出的误差信号电压中除基波正规分量外,还包含基波交叉分量和二次谐波分量等,降低了测角精度。通过对线极化目标信号和椭圆极化雷达天线匹配情况的分析和计算,获得了有关的公式和曲线。还对椭圆极化目标信号和椭圆极化雷达天线情况作了阐述。公式和曲线可作为选定卫星天线或地面站雷达天线椭圆极化率的参考依据。     

S波段超小型锁相信标机的设计与实现

介绍一种新研制的超小型信标机 ,该机采用锁相环技术 ,输出信号质量高。信标机安装在氢气球悬挂的金属铝球内 ,可综合检验同一场区内的引导雷达、脉冲雷达、遥测跟踪站等设备的动态跟踪性能 ,实现测控系统的动态联调和合练。     

Design of a 40/50 GHz satellite ground station for fade mitigation experiments

Due to the increasing demand in satellite capacity, driven by applications such as high-definition television (HDTV), 3D-TV and interactive broadband services, higher frequency bands will have to be exploited. The capacity on Ku-band is already becoming scarce and Ka-band systems are more commonly used. It can be expected that 40 and 50 GHz (Q and V band) will have to be used in the future. At these frequencies the wave propagation effects have a significant impact on the performance. The traditional approach of implementing large fade margins in the system design is not suitable as it leads to expensive ground terminals. Fade mitigation by adaptive coding and modulation (ACM) is a cost-efficient method. To investigate the Q/V-band for future commercial exploitation, ESA's ALPHASAT satellite will provide experimental payloads for communications and wave propagation experiments. In Graz a Q/V-band ground station is currently under development. It will be equipped with a 3 m tracking antenna, a 50 W Klystron amplifier and a 290 K LNA. Fade mitigation experiments will be conducted, initially using DVB-S2 modems which allow to vary the modulation scheme, the Forward Error Correction code and the symbol rate under control of the ACM computer. In addition, uplink power control can be combined with the ACM methods. A specially developed signal analyser provides precise measurement of the signal/noise ratio. In addition, propagation data will be available from a beacon receiver, also developed by Joanneum Research. Important goals of the experiment are to investigate the reliability of links under realistic operating conditions using ACM and to develop efficient ACM and signal/noise ratio measurement algorithms which can be later implemented in optimised modems for Q/V-band.The paper describes the ground station design and addresses the planned fade mitigation experiments.     

Beacon Monitoring: Reducing the Cost of Nominal Spacecraft Operations

Beacon monitoring is an architecture for augmenting on-board health assessment software with the following elements: a transmitter that periodically broadcasts this health assessment to the ground, a network of globally distributed low-cost monitoring stations that relays the health assessment to mission control, and an automated mission control system for notifying on-call operators and initiating appropriate response actions. While beacon monitoring is often cited as a means of lowering nominal monitoring costs for particular missions, these claims have typically been qualitative and undiscriminating in nature. This study introduces modeling and experimentation as means of providing a more fundamental validation of the cost-effectiveness of beacon monitoring. Results include simple quantitative estimates of first-order performance metrics, experimental data that verifies predicted performance and validates the use of beacon monitoring for a test mission, and a method for assessing the value of beacon monitoring for general satellites missions.     

Policy issues in communicating with ETI

Two possible scenarios for the detection of extraterrestrial intelligence are presented and the issues they would raise discussed. The article then goes on to examine operational questions and reply policy in the event of contact being made. Questions of how such contact should be announced to the world--and by whom; who should send a reply; how it would be designed and what it would say, are explored. Creating a beacon actively to beam a message into the galaxy could provide a test case for international consultation and cooperation in responding to ETI.     

全相参雷达信标

为缩短雷达的研制周期、节约经费，研制了一种全相参雷达信标，用于对全相参宽频带自适应频率捷变脉冲压缩雷达进行测试。介绍了全相参雷达信标的关键技术及其实现方法。外场试验表明，该信标设备的设计原理是可行的，效果也是明显的。     

Communications transponder performance for Japanese Communications Satellite-2 and prospects for future systems

Communications transponder for the Japanese Communications Satellite-2 (CS-2a and 2b) to be launched into a geostationary orbit by N-II launch vehicle in February and August, 1983, has been developed. The transponder is provided with six-channel K-band ($\text{30}\text{20}\text{GHz}$) transponder including beacon transmitter, which operates in the highest frequency ranges ever utilized on an operational communications satellite, and two-channel C-band ($\text{6}\text{4}\text{GHz}$) transponder. Receiver front end of the K-band transponder consists of a direct mixer followed by a 1.8 GHz IF amplifier and provides 8 dB noise figure. 20 GHz output power is 4 W by final amplification at 5-W TWTA. C-band transponder provides 4 dB noise figure and 4.3-W output power. Key factors for future high capacity transponder are also presented.     

Propagation experiment with Japanese satellite,ETS-II (KIKU-2)

The first Japanese geostationary satellite, Engineering Test Satellite Type II [Kiku-2], has been successfully placed at 130°E at the beginning of March 1977.Using beacon transmitters at three coherent frequencies of 1.7, 11.5 and 34.5 GHz which are installed in ETS-II, the Radio Research Laboratories (RRL) of the Ministry of Posts and Telecommunications (MOPT) conduct propagation experiments to obtain preliminary information for the Experimental Communication Satellite (ECS) experiment.The experimental system for propagation experiment with ETS-II is composed of a main receiving station, a rain radar, a radio-meter, meteorological instruments and data handling computers.The receiving data, including signal levels of co- and cross-polarization in these frequencies and phase differences between each of these frequencies and polarization, are sampled every 200 msec.The satellite-to-Earth propagation experiment at the highest frequency has been satisfactorily started on 11 March 1977.     

A search for optical beacons: implications of null results

Over the past few years a series of searches for interstellar radio beacons have taken place using the Parkes radio telescope. Here we report hitherto unpublished results from a search for optical beacons from 60 solar-type stars using the Perth-Lowell telescope. We discuss the significance of the null results from these searches, all of which were based on the interstellar contact channel hypothesis. While the null results of all searches to date can be explained simply by the nonexistence of electromagnetically communicating life elsewhere in the Milky Way, four other possible explanations that do not preclude its existence are proposed: (1) Extraterrestrial civilizations desiring to make contact through the use of electromagnetic beacons have a very low density in the Milky Way. (2) The interstellar contact channel hypothesis is incorrect, and beacons exist at frequencies that have not yet been searched. (3) The search has been incomplete in terms of sensitivity and/or target directions: Beacons exist, but more sensitive equipment and/or more searching is needed to achieve success. (4) The search has occurred before beacon signals can be expected to have arrived at the Earth, and beacon signals may be expected in the future. Based on consideration of the technology required for extraterrestrial civilizations to identify target planets, we argue that the fourth possibility is likely to be valid and that powerful, easily detectable beacons could be received in coming centuries.     

"Signal" search for intelligence in the galactic nucleus with the array of the Lowlands

In August, 1981, the Westerbork Synthesis Radio Telescope was used for 4 h to search for narrowband pulsing radio beacons in the direction of the Galactic Center. By using both the spatial discrimination and temporal stability available to an interferometric measurement, weak intermittent signals can be detected even in the face of the strong, naturally caused radiation from this region. A radio beacon within our bandwidth, centered on the 21 cm neutral hydrogen line, would be recognizable if it had a repetition period between 40 sec and 1/2 h. The rms sensitivity to point sources was approximately 50 mJy/cycle, and the detection limit was 500 mJy/cycle. The limit degrades for pulse widths < 0.02s. No repetitive signals were found. For a swept, narrow-band radio beacon constrained to the Galactic Disk (beamwidth = 0.02 rad), our detection limit corresponds to a transmitter power of 10(11) MW at the Galactic Center.     

车载遥测站天线标校复查中存在的问题及对策

车载遥测跟踪站天线展开后,需要进行远场标校复查。由于受标校距离、天线仰角以及周围环境等各种条件的限制,使得主天线、引导天线的光电轴匹配检查难以保证精度要求,从而影响跟踪性能。针对这些问题,本文提出在近场条件下直接悬挂信标机进行标校复查,以保证光电轴匹配精度。并针对YQ- 312 S频段遥测跟踪车载站的实际推出角度转换公式。最后给出实例     

激光模拟单粒子效应设备及试验研究进展综述

单粒子效应的脉冲激光模拟方法是单粒子效应地面模拟试验中近年来才发展起来的一种方法。文章主要介绍了脉冲激光模拟单粒子效应的基本原理、特点及国内外研究进展。研究表明脉冲激光模拟是一种有效、安全、经济、方便的地面模拟单粒子效应的方法,在器件单粒子效应危害评估及电路加固验证方面具有明显的优势。     

Analysis of the orbital motion of the asteroid Apophis’ satellite

We have analyzed the orbital disturbed spacecraft motion near an asteroid. The equations of the asteroidocentric spacecraft motion have been used with regard to three perturbations from celestial bodies, the asteroid’s nonsphericity, and solar radiation pressure. It has been shown that the orbital parameters of the main spacecraft and a small satellite with a radio beacon can be selected such that the orbits are rather stable for a fairly long period of time, i.e., a few weeks for the main spacecraft with an orbit initial radius of ~0.5 km and a few years before approaching Apophis with the Earth in 2029, for a small satellite at an orbit initial radius of ~1.5 km. The initial orientation of the spacecraft orbital plane perpendicular to the sunward direction is optimal from the point of view of the stability of the spacecraft flight near an asteroid.     

Space-VLBI: a new possibility to complement terrestrial microwave surveys

Previous suggestions of using space-VLBI for SETI are critically reviewed and some new suggestions presented. It is pointed out that the highly stable standard frequency uplink to the satellites can be considered as an active beacon of the terrestrial technical civilisation.     

Short-pulse SETI

While most optical SETI experiments are configured to detect nanosecond pulses, the majority of their counterpart radio searches integrate for seconds to minutes, looking for unchanging narrow-band carriers or slowly pulsed modulation. The former approach is suggested as an effective way to stand out against stellar photon noise, while the latter approach is dictated by the dispersive effects of the interstellar medium as well as the high visibility of narrow-band signal components.In this paper, we consider effective signal strategies for those that produce, rather than simply search for, optical and radio beacons—signals that are designed to elicit responses from technological civilizations. By considering the communication problem from the point of view of the transmitters, rather than the receivers, we deduce some likely signal characteristics for beacons, and concommitant new strategies for SETI.     

分布式SAR相位同步误差的影响分析与试验验证

相位同步是分布式SAR系统必须考虑的突出问题之一。建立了双向脉冲交换相位同步全数字仿真模型,仿真得到相位同步误差信号。基于全数字仿真系统分析了不同类型相位同步误差对InSAR测高性能的影响。最后利用地面半实物仿真试验得到实际分布式SAR系统相位同步误差及其对InSAR测高的影响,实测相位同步误差标准差为2.6度,引起的InSAR相对测高精度损失在厘米量级;并且半实物试验结果与全数字试验结果一致,表明了相位同步方案及其影响分析的正确性。本文工作对分布式SAR相位同步分系统的设计与实现具有重要指导意义。     

Preferred frequencies for SETI observations

SETI observational programs conducted over the last two decades, and most of those planned for the near future, have concentrated on searching for signals at microwave frequencies. Considerations of signal-to-noise ratio at the receiving end indicate that this is the correct approach if the broadcasting society is not concerned with directionality and transmits into a fairly large solid angle. However, if that society desires to transmit only a highly directional beacon, then it is not now possible, given our lack of knowledge of advanced space technology, to predict reliably whether microwave or infrared wavelengths are to be preferred in an optimum search program. Given the realities of current terrestrial technology, either the centimeter or millimeter domain is to be preferred to the infrared, independent of considerations of directionality. In any event, there does not appear to be any cosmically unique (“magic”) frequency at which to conduct SETI.     

脉冲激光试验在宇航器件和电路系统抗单粒子效应设计中的初步应用

抗单粒子效应加固是宇航器件研发和卫星电路系统设计面临的重要难题.准确、有效的单粒子效应试验评估对此问题的解决有巨大帮助.中国科学院空间科学与应用研究中心于近十年在国内自主发展了用于单粒子效应评估的脉冲激光试验相关装置、试验技术和方法,对宇航器件和卫星电路开展了初步应用.通过脉冲激光试验,能够快速甄别、定位宇航器件试样的...     

高重复频率DPL激光辐照光学薄膜元件温升规律实验研究

光学薄膜是激光系统中最易损坏的薄弱环节。在高重复频率脉冲激光辐照下光学薄膜表面温度急剧上升,导致膜层应力、结构发生变化,最后出现宏观的灾难性损伤。文章采用红外热像仪实时测量了重复频率10 kHz 的DPL脉冲激光辐照下光学薄膜元件表面激光辐照中心点的温度变化,分析了影响薄膜元件温度变化的众多因素。结果表明,采用热导率较大的材料作基板的薄膜样品表面的温升较低;基板厚度越大的薄膜样品表面温升越低;薄膜表面激光辐照中心点的温度与样品的吸收峰值功率密度呈线性关系。     

脉冲激光诱发65nm体硅CMOS加固触发器链的单粒子翻转敏感度研究

针对65 nm体硅CMOS工艺触发器链,利用脉冲激光研究了敏感节点间距、加固结构和测试数据类型等因素对电路的单粒子翻转效应（SEU）敏感度的影响。研究表明:敏感节点间距增大可有效提高双互锁存（dual interlocked storage cell, DICE）结构触发器链的抗SEU性能,但当敏感节点间距较大（如＞4.0 μm）时,间距增大的器件加固效果减弱;触发器单元中NMOS管经保护漏结构加固、PMOS管经保护环结构加固后其SEU敏感度明显降低;不同数据测试模式下触发器链的SEU敏感度不同,这可能与不同模式下单元中的敏感晶体管类型不同有关。此外,脉冲激光作为一种地面模拟手段,可有效用于确定单粒子敏感器件设计的最佳间距和验证防护效果。