## 5 Conclusions  
By examining seven years of Swarm L2\(-\)IBI data, we studied the occurrence rate of the equatorial plasma bubbles (EPBs) during different levels of geomagnetic storms. The main findings can be summarized in the following:  
1. The majority of IBIs are observed within \(\pm\)20\({}^{\circ}\) latitude around the dip equator. The IBIs observed during moderate and super storms spread over a large range of longitude in comparison with the IBIs observed during intense storms, which are concentrated within limited longitudes over the SAA. The numbers of IBIs in the northern hemisphere are always slightly larger than their corresponding southern hemispheric numbers at all longitudes during super, intense, and moderate geomagnetic storms. 2. During super and intense storms, the number of IBIs at the altitudes of Swarm B is larger than those observed at the altitudes of Swarm A and C. During moderate storms the majority number of IBIs are observed by Swarm A and C. Irrespective of storm type, the plasma bubble events have a noticeable longitudinal distribution, as the majority of IBI events are observed within the longitudinal sector (0\({}^{\circ}\) E and 110\({}^{\circ}\) W), where the SAA is located. 3. The number of IBI events at low altitudes (\(<\)470 km) is larger than those observed at higher altitudes (\(>\)500 km) and the probability of finding IBIs at higher altitudes increases with the increase in the level of the geomagnetic storm. No correlation was found between the duration time (scale) of the IBIs and the altitudes because the duration time of IBIs has a random distribution at both altitudes for all types of storms. The duration time only tends to have a significant enhancement over the SAA region. 4. The local time variation of IBI events shows distinguished patterns over different types of storms. During super storms, the maximum number of IBIs detected by Swarm A and C appeared within the pre-midnight hours (21:00-24:00 LT) and shifted to sunset hours (18:00-21:00 LT) for Swarm B. On the other hand, during intense storms, the probability of observing IBIs by Swarm (A, C) in post-midnight hours (24:00-6:00 LT) is larger in comparison with the super storms. The occurrence rate of IBIs during moderate storms increases with approaching the pre-midnight (21:00-24:00 LT) time. Moreover, the number of IBIs at the altitudes of Swarm A and C is always larger than those observed by Swarm B. In addition, the number of events detected by the three satellites within the post-sunset is larger than those observed within the pre-midnight period. 5. The occurrence rate of IBIs with duration times \(>\)100s is larger during super storms while the moderate storms showed a larger percentage than intense storms. So, no correlation was found between the duration time of IBIs and the type of geomagnetic storm. The duration time of IBIs only increases from the sunset until midnight, and also over the SAA region. Also, the most remarkable point is the absence of sunset IBI events during the winter months. In addition, the majority of super storm IBIs are only observed within the pre-midnight period during summer months and within the sunset period during equinoxes. 6. The seasonal variations of IBIs indicated that the numbers of IBIs in the equinoxes are always larger than those in the summer and winter months. This seasonal variation is independent of the altitude of Swarm satellites. Moreover, the number of IBIs has two crests: one at 20:00 LT and the other at 22:00 LT during months 9-11. 7. COSMIC electron density at the F2 layer peak height (hnr2) layer showed that, during super storms, the \(n_{e}\) data are dramatically decreased/depleted in comparison with moderate and intense storms. The hnr2 is displaced to higher altitudes (~400 km) not only during the main phase of super storms but during intense storms and in the recovery phase of super storms, it is observed at lower altitudes in comparison with moderate storms. * 8.