An algorithm to detect high‐speed ionospheric flow channels (FCs) in the polar cap was applied to data from the Longyearbyen radar of the Super Dual Auroral Radar Network. The Longyearbyen radar is at high latitude (78.2°N, 16.0°E geographic coordinates) and points northeast; therefore, it is in an ideal position for measuring zonal flows in the polar cap. The algorithm detected 998 events in the dayside polar cap region over 2 years of observations. The detected FCs typically were between 200 and 300 km latitudinal width, 1.1–1.3 km s⁻¹ peak velocity, and 3 min in duration. The FC location shows an interplanetary magnetic field (IMF) By dependency, moving dawnward/duskward for a +By/−By. The FC monthly occurrence shows a bimodal distribution with peaks around the spring and autumn equinoxes, likely due to increased coupling between the solar wind‐magnetosphere‐ionosphere system at these times. The highest peak velocities show an absence of broad FC widths, suggesting that as the flow speed increases in the polar cap, the channels become more localized and narrow.

中文翻译：

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极地盖流道及其IMF依赖关系的统计研究

一种用于检测极盖中高速电离层流道（FC）的算法已应用于来自超级双极光雷达网络的Longyearbyen雷达的数据。Longyearbyen雷达处于高纬度（北纬78.2°，东经16.0°），指向东北。因此，它处于测量极帽中纬向流量的理想位置。经过2年的观察，该算法在白天的极地上限区域检测到998个事件。检测到的FC通常在200至300 km的横向宽度之间，峰值速度为1.1–1.3 km s ^-1，持续时间为3分钟。FC位置显示了星际磁场（IMF）依存关系，朝着/朝上移动+ By / -通过。FC的月度出现双峰分布，在春季和秋季的春分点附近出现峰值，这可能是由于此时太阳风-磁层-电离层系统之间的耦合增加。最高峰速度显示不存在较宽的FC宽度，这表明随着极帽中流速的增加，通道变得更加局部且狭窄。