Structuring of the ionospheric convection flows associated with enhanced solar wind ULF fluctuations

Recent studies have shown that, regardless of the orientation of the interplanetary magnetic field, high level of ULF wave activity in the solar wind can substantially enhance the ionospheric convection, suggesting that the ULF fluctuations may also be an important contributor to the coupling of the solar wind to the magnetosphere-ionosphere system. The convection enhancements associated with enhanced solar wind ULF power may be related to structuring of the ionospheric flow patterns. In order to have a more accurate understanding of the ionospheric response to the ULF power, our study will focus on both qualitative and quantitative evaluation of the structuring of the polar cap convection. Potential convection maps constructed from SuperDARN radar observations can be used for identification of characteristic features of the convection flow speed associated with solar wind ULF power. Additionally, we can utilize data from a network of ground magnetometers, which can, due to the continuous availability of high latitude station data, facilitate the evaluation of the flow patterns and thus help in the evaluation of the features that are identified from radar observations.