# Unveiling the Core Patterns of High-Latitude Electron Density Distribution at Swarm Altitude
## 5 Discussion
It is worth noting, however, that the residues obtained from our analysis appear to capture these changes, providing insights into the variations in electron density associated with geomagnetic activity. We now examine the four modes resulting from each decomposition. The first of these modes, reported only for the equinoctial and low geomagnetic activity case in Figure 4, is analogous to the other five configurations (data not shown), and essentially represents a noise component present in the data. Starting from an analysis of the data distribution resulting from an average, this term could be due to small-scale variations in the original distribution. However, the energy associated with this mode is extremely low, and there are no significant structures in its distribution on the MLat-MLT plane. On the other hand, the second mode (for brevity, data are shown only for the equinoctial and low geomagnetic activity configuration in Figure 4) is quite different. As extensively discussed in the previous section, this mode exhibits a spatial structure that closely resembles the orbit of the satellite from which the data were acquired. The average frequency of this mode is consistent across latitudes, and is comparable to the orbital period of the satellite around the Earth. Finally, the third and fourth modes capture our interest because they are intricately linked to dynamic processes occurring within the ionospheric layer under investigation. These modes exhibit a strong dependence on both the season and the level of geomagnetic activity, making them particularly intriguing and worthy of further exploration. To gain insight into the dynamic processes that contribute to the distribution of electron density for these two modes regardless of season or activity level, convection cell structures are overlaid onto the maps depicting these modes. At high latitudes, the ionized region of the upper atmosphere undergoes a dynamic circulation known as convection driven by the interaction of the magnetized solar wind and the Earth's magnetosphere. This convection is important in determining the distribution of electron density in the ionosphere. The convection patterns are twin-celled in nature, with the flow moving away from the Sun at the poles and toward the Sun at lower latitudes. The strength of this circulation is influenced by the north-south component of the IMF (represented as \(B_{z}\)), while any asymmetries between the dawn and dusk regions are associated with the east-west component of the IMF (\(B_{y}\)). In general, convection exhibits a highly dynamic nature, displaying sensitivity to intermittent phenomena such as variations in the IMF and magnetospheric processes such as substorms. One effective method for capturing and analyzing these convection patterns is to utilize data from the Super Dual Auroral Radar Network (SuperDARN). SuperDARN is a widespread network of scientific radars designed to monitor the near-Earth space environment. Each radar within the network is capable of measuring the velocity of ionospheric plasma. By combining data from multiple radars, a comprehensive view of plasma motion in the polar ionosphere can be obtained, enabling studies on the electromagnetic interaction between the solar wind and Earth's magnetosphere [34]. Using a long period of SuperDARN data, a dynamic model of convection can be constructed to enable the precise determination of the electrostatic potential distribution in high latitude regions for a wide range of solar wind, IMF, and dipole tilt parameter values [35].