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The occurrence of irregularities is strongly dependent on geomagnetic activity.
The bottom panel of Fig. 2 presents the time evolution of the occurrence of irregularities at the EJC height for the three data sets evaluated in this study.
These three basic differences between the above-mentioned studies highlight the originality of our results, at least with respect to the occurrence of irregularities in the American sector.
Some differences between the occurrence of irregularities in the ROTI maps constructed with the GPS data and the simulated aurora oval shape can be explained by the storm-induced dynamic processes in the ionosphere (e.g., SED, TOI, SAPS, and plasma instabilities), which could not be accounted in the precipitation model.
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When the OLR occurrences are smaller than the occurrences of irregularities, it implies that the gravity wave cannot be the only seed for the RT instability.
The occurrence of the irregularities strongly depended on the geomagnetic activity.
Monitoring the time derivative of TEC (ROT) is useful for tracing the occurrence of ionospheric irregularities.
However, to our knowledge, the expected minimum and maximum in the occurrence of plasma irregularities have not yet been identified.
To identify the occurrence of the irregularities in the density structure, we set the threshold equal to 2 units for RODI and 5 units for ROTI data.
Analysis of the occurrence of ionospheric irregularities was based on daily ROTI maps for the period 2010 to 2013, which included the peak of the 24th solar cycle.
The occurrence of ESF irregularities with σ ≥ 0.3% within ± 15o dip latitudes was derived during magnetic quiet times in the local time range of 1800 2400 h.
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