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Radically new approach for large antenna in space: the 'RF prism' concept

机译:太空中大型天线的全新方法:“ RF棱镜”概念

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RF prism is a kind of space-borne antenna lens with an illuminator that is not at the end of a boom but on a separate satellite, usually located on the same orbit. This lens deviates the waves towards or away from the Earth; it also needs to amplify and sometimes to change the frequencies. Provided that the illuminating axis and the Earth-sighting axis have incidences on the antenna plane that meet a specific relation, the antenna flatness requirement is relaxed by a factor of 10 at least. Prism therefore eases the deployment of very large antennas in space (20 or 50 m). In the option where the antenna deformation is known, which can be achieved by measuring the illuminating signals, and corrected by phase shifters on the antenna, the relaxation applies to the accuracy of the deformation knowledge and the deformation is no longer a constraint. The antenna panels do not need to be fully joined together and locked in the same plane, which enables two-axis deployment and very compact folding of the antenna. As the flatness constraint intervenes above all on an interpanel scale, the coupling between sides of the prism is typically on a single point per panel with a small rear radiator. The illuminator satellite is kept small since it is not constrained by the illumination function but just by the central payload function moved away from the main satellite. A cluster of illuminators is reproduced transparently into an equivalent cluster of beams, with the cluster apertures modified according to the ratio between the frequencies on illumination side and Earth side. With a high illuminating frequency, the illuminating cluster can be obtained within a single satellite with booms of 1 to 3 m. The illuminators can therefore ensure a close beam pattern while the multi-beam function of the antenna is used to multiply this pattern to provide a broad mosaicing. The internal complexity of the antenna is therefore reduced by a factor equal to the number of illuminators. The concept can be implemented with current technology although it would also benefit from the permanent progress made in active antennas (reduction in mass and thickness).
机译:RF棱镜是一种带照明器的星载天线透镜,该照明器不在吊臂末端,而位于单独的卫星上,通常位于同一轨道上。该透镜使波偏向或远离地球。它还需要放大,有时需要更改频率。假设照度轴和地视轴在天线平面上的入射角满足特定关系,则天线平面度要求至少应放宽10倍。因此,棱镜可以简化非常大的天线在空间(20或50 m)中的部署。在已知天线变形的选项中(可以通过测量照明信号来实现,并通过天线上的移相器进行校正),这种放宽适用于变形知识的准确性,并且变形不再是约束。天线面板不需要完全连接在一起并锁定在同一平面内,这样可以实现两轴部署,并且天线的折叠非常紧凑。由于平坦度约束首先在面板间进行干预,因此棱镜侧面之间的耦合通常在每个面板的单个点上,并且后部辐射较小。照明器卫星保持较小,因为它不受照明功能的限制,而仅受远离主卫星的中央有效载荷功能的限制。照明器的群集透明地复制为等效的光束群集,群集的孔径根据照明侧和地球侧的频率之比进行修改。照明频率高,可以在吊臂为1至3 m的单个卫星中获得照明集群。因此,在使用天线的多波束功能来使该模式倍增以提供宽广的镶嵌效果的同时,照明器可以确保近波束模式。因此,天线的内部复杂度降低了与照明器数量相等的系数。尽管可以从有源天线的不断进步(质量和厚度的减少)中受益,但可以用当前技术来实现该概念。

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