用于海军空间监视系统的无线电干涉仪相位信道合成器模型II

M. Kaufman
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引用次数: 6

摘要

位于华盛顿特区的美国海军研究实验室开发的用于探测地球卫星的空间监视系统在美国南部形成了一道栅栏。四个接收点与三个发射点交替,当卫星穿过围栏时,发射点用无线电能量照亮卫星。反射能量的到达角由复合无线电干涉仪在每个接收站测量。这些信号产生多种通道,通常记录在纸上,用计算尺和/或数学表读取和解析。操作上,分辨率是由计算机完成的。随着卫星人口的增加,过境围栏的数量也大大增加。如果要避免大量积压的数据,就需要在探测过程中实现自动化,以便于相互识别和分类卫星。本报告的目的是描述一种电子系统,该系统自动将几个有噪声的模糊无线电干涉仪相位信道合并为一个无模糊的安静信道。该技术的结果是,给定一个多基线无线电干涉仪系统,通常具有高角分辨率能力,伴随着通常的干涉仪模糊问题,与解码多相位信号输出相关,它可以直接仪器到一个单一的无模糊信号输出,其精度和分辨率与干涉仪中最长的基线成正比,其噪声含量与该基线成反比。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Radio Interferometer Phase-Channel Combiner Mod. II for the Navy Space Surveillance System
The Space Surveillance System developed at the U. S. Naval Research Laboratory, Washington, D. C., for the detection of earth satellites forms a fence across the southern part of the United States. Four receiving sites are alternated with three transmitting sites which illuminate satellites with radio energy as they traverse the fence. The angle of arrival of the reflected energy is measured at each receiving station by a compound radio interferometer. These signals yield a multiplicity of channels which are normally recorded on paper, read and resolved by using slide rules and/or mathematical tables. Operationally the resolution is done by a computer. With the increasing satellite population the number of fence crossings has increased considerably. Automation in the detection process is needed to facilitate identification and sorting of satellites from each other if a large backlog of data is to be avoided. The purpose of this report is to describe an electronic system which automatically combines several noisy ambiguous radio interferometer phase channels into one unambiguous quiet channel. This technique results in that given a multi-baseline radio interferometer system, normally having high angular resolution capability accompanied with the usual interferometer ambiguity problem associated with deciphering the multiple phase signal outputs it can be instrumented directly into a single unambiguous signal output which has an accuracy and resolution proportional to the longest baseline in the interferometer and whose noise content is inversely proportional to this baseline.
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