# Unveiling the Core Patterns of High-Latitude Electron Density Distribution at Swarm Altitude
## 5 Discussion
In our case, we obtained representative average convection motions that reflect the interplanetary conditions underlying the originated data by calculating the mean values of the x-component of the solar wind velocity (\(v_{sw,x}\)), the y- and z-components of the magnetic field, and the dipole tilt for each of the six different datasets analyzed and presented in Figure 1. The obtained values, which refer to the time intervals used to build the different datasets, were then incorporated into the CS10 model [36], enabling us to obtain the average trends of the electrostatic potential distribution. Table 1 reports the values of the solar wind velocity, the two components of the magnetic field, and the dipole tilt used in the different cases. Figure 6 illustrates the spatial and temporal distributions of the electron density for the third and fourth fundamental modes obtained from decomposition during low geomagnetic activity. The figure consists of six maps, with each pair representing the III and IV modes for the analyzed equinoctial, summer, and winter periods. Each map includes the average electrostatic potential level curves overlaid on top of the electron density spatiotemporal distribution. Similarly, Figure 7 follows the same structure as Figure 6 with a focus on the period of high geomagnetic activity. \begin{table}
\begin{tabular}{c c c c c} \hline
**Condition** & \(\mathbf{v}_{sw,x}\) **(km/s)** & **IMF B\({}_{y}\) (nT)** & **IMF B\({}_{z}\) (nT)** & **Dipole Tilt** \\ \hline Equinoxes, SME \(\leq\) 70 nT & \(-\)367 & \(-\)0.13 & 1.36 & 0\({}^{\circ}\) \\ Equinoxes, SME \(\geq\) 230 nT & \(-\)482 & 0.10 & \(-\)2.08 & 0\({}^{\circ}\) \\ Summer, SME \(\leq\) 70 nT & \(-\)355 & 0.19 & 1.17 & 10\({}^{\circ}\) \\ Summer, SME \(\geq\) 230 nT & \(-\)451 & \(-\)0.36 & \(-\)2.06 & 10\({}^{\circ}\) \\ Winter, SME \(\leq\) 70 nT & \(-\)366 & \(-\)0.67 & 0.88 & \(-\)10\({}^{\circ}\) \\ Winter, SME \(\geq\) 230 nT & \(-\)491 & 0.24 & \(-\)1.66 & \(-\)10\({}^{\circ}\) \\ \hline \end{tabular}
\end{table} 
Table 1: Interplanetary parameters and dipole tilts used as input values for the SuperDARN model relative to each one of the seasonal and geomagnetic activity conditions considered in the present study. Figure 6: Polar view of the III and IV fundamental modes obtained from the MEMD of electron density distribution during the equinoctial (first row), summer (second row), and winter (third row) periods under low geomagnetic activity in the Northern Hemisphere. SuperDARN polar potential maps obtained using the statistical convection model CS10 are superimposed on each mode as level curves. Maps are represented in the QD–magnetic latitude (MLat) and MLT reference system. The concentric circles are plotted in 10\({}^{\circ}\) intervals, with the outermost circle corresponding to 50\({}^{\circ}\). We begin with the fourth mode and its relationship to the season and geomagnetic activity, as well as the structure of the convection cells superimposed on each map. Here, we are specifically looking at all of the electron density maps shown in the right column of Figures 6 and 7. The electron density spatiotemporal distribution exhibits a clear day-night difference. The spatiotemporal distribution during equinoxes shows higher density values within the MLT interval between 7:00 and 20:00, with a peak occurring between 11:00 and 18:00. This pattern is consistent across all studied latitudes. This day-night asymmetry is primarily attributed to the interaction between solar radiation and the Earth's atmosphere. During the day, solar radiation provides a significant amount of energy that ionizes the upper atmosphere, resulting in higher electron density in the F-layer. Conversely, during the night solar radiation is absent or significantly reduced, leading to a decrease in ionization and electron production. Another contributing factor to the day-night asymmetry is the recombination effect that takes place during the night.