## 5 Swarm Ne Disturbances during Nighttime of the 2016-2017 Winter and M5+ Earthquakes  
The high-pass filtered (at 500 km wavelength \(\approx\) 65 s period) in situ measured Ne in the 91 orbital passes of each of the three satellites are analyzed spectrally via STFT, and the spectrograms are prepared in the same way as in Figures 4-6. However, the presentation of 273 spectrograms in this research paper would be impossible. Therefore, the spectrograms have been sampled at a 300 km wavelength (-40 s), and the maxima from the vectors of the sampled PSDs have been collected as daily time series. These maxima are presented with the use of a light-blue area plot, and we also call these \"Swarm Ne PSD\" to maintain consistency along the entire study. Swarm Ne PSD values are applied in the assessment of Swarm's sensitivity to seismic activity in the region over time. The selection of a 300 km wavelength is a preliminary choice, and it does not mean that 300 km is the most representative frequency domain wavelength for SIID detection. However, this wavelength looks to be approximately located in the middle of the disturbances found in Figures 4-6 and it is suspected to be sensitive to seismic activity. Therefore, Swarm Ne PSD sampled at 300 km from the spectrograms is used as an indicator of Swarm's sensitivity to the seismic record, F10.7, EPB, and geomagnetic ap and Dst indices. Additionally, observing a high sensitivity of the LPs and quite dynamic changes in Swarm disturbances over the tectonic plate boundary, and assuming a complex and long-term evolution of seismic activity, the 5-, 7-, and 10-day moving averages are also calculated from Swarm Ne PSD to reveal the more long-term character of the Ne changes. Averaging in time can also mitigate two other disadvantages: strong short-term Ne variations affecting the correlated temporal Ne change and differences between the longitudes of consecutive orbital footprints. The 10-day averages are plotted as bold blue lines in Figures 7-15. The earthquakes are visualized by their depths and magnitudes. The magnitudes are multiplied by 10 to easily maintain the consistency of the axes in Figures 7-15. The ap index and the Dst index are multiplied by two due to the same reason. The 5-, 7-, and 10-day moving averages are also calculated for ap and Dst indices, and their 10-day averages are similarly plotted in Figures 7-15 using green and orange bold lines, respectively. The F10.7 parameter in the solar flux units (SFUs) originally have a compatible scale here, but the numbers of Swarm epochs with confirmed and unconfirmed plasma bubbles along the individual tracks have to be divided by 10. They are drawn in the bottom direction to be more readable amongst the other parameters. Furthermore, the Swarm Ne PSD maxima and their moving averages have arbitrary and nonrelated scales that are used to clearly visualize their most interesting relative variation. This does not affect the results, as the scaling has no influence on the correlation observation. The scales of Swarm Ne PSD and its moving average are equal for Figures 7, 8 and 10-12 (equatorial latitudes), increased six times in Figure 9 (high latitudes) in comparison to Figures 7 and 8, and increased a hundred times in Figures 13-15 (daytime, sampling at higher frequency), because the signals at different wavelengths have different amplitudes. Based on the earthquake magnitude and depth and knowing that the shallowest earthquakes are the ones that are most suspected of affecting the ionosphere [(23)], we calculated an equivalent of the so-called cumulative Benioff strain, which corresponds to the cumulative (square root sum) of the seismic energy [(66; 67; 68)]. The quantity calculated in this study is a kind of weighted cumulative sum, because the square roots of energy approximation are divided by the focal depths, i.e., \(cs=\sum_{i=1}^{n}\sqrt{10^{M(i)}}/H(i)\), where n is the number of earthquakes in the selected time window, and \(H(i)\) are their focal depths.