Based on the observations of Ionospheric Bubble Index (IBI) data from the Swarm mission, the characteristics of plasma bubbles are investigated during different types of geomagnetic storms recorded from 2014 to 2020. The geometrical constellation of the Swarm mission enabled us to investigate the altitudinal profile of the IBIs during different activity levels in a statistical mean. Results show that the majority of IBIs associated with moderate storms are observed at low altitudes and the probability of observing IBIs at high altitudes (Swarm-B) increases with the increase in storm level. This is confirmed by observing the F2 layer peak height (hmF2) during super storm events at larger altitudes using COSMIC data. The maximum number of IBIs is recorded within the South Atlantic Anomaly (SAA) region with a long duration time and tends to increase only during dusk time. Both the large duration time and number of IBIs over the South Atlantic Anomaly (SAA) suggest that the gradient in the electron density and the depression in the magnetic field are the main factors controlling IBI events. Also, the IBIs at high altitudes are larger at sunset and at low altitudes pre-midnight. In addition, the occurrence of IBIs is always larger in the northern hemisphere than in the southern hemisphere irrespective of the type of storm, as well as during the summer months. Moreover, there is no correlation between the duration time of IBIs and both the altitudinal observation of the IBIs and the storm type. Seasonal occurrence of IBIs is larger during equinoxes and vice versa during solstices irrespective of both the type of storm and the altitude of the satellite. The large number of IBIs during equinoxes agrees with the previous studies, which expect that the large electron density is a developer of steeper . Large occurrences of super storm IBIs observed within the pre-midnight during summer and at sunset during equinoxes are a novel observation that needs further investigation. Also, the majority of IBIs are observed a few hours after geomagnetic substorms, which reflects the role of the Disturbance Dynamo Electric Field (DDEF) as a main driver of IBIs.

中文翻译：

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不同类型地磁暴群的星群观测到的等离子体气泡的统计分析

基于对Swarm任务的电离层气泡指数（IBI）数据的观察，研究了2014年至2020年记录的不同类型的地磁暴期间的等离子体气泡特征。Swarm任务的几何构象使我们能够研究高度剖面统计活动中不同活动水平下IBI的变化。结果表明，与中度风暴有关的大多数IBI都在低海拔处观察到，而在高海拔处观测IBI的可能性（Swarm-B）则随着风暴水平的增加而增加。通过使用COSMIC数据在较大高度的超级风暴事件中观察F2层峰值高度（hmF2）可以确认这一点。IBI的最大数量记录在南大西洋异常（SAA）区域内，持续时间很长，并且仅在黄昏时间有增加的趋势。大持续时间和南大西洋异常（SAA）上的IBI数量均表明，电子密度梯度和磁场下降是控制IBI事件的主要因素。同样，高空的IBI在日落时和午夜前的低空时更大。另外，不管风暴的类型如何，以及在夏季，北半球的IBI发生总是比南半球大。此外，IBI的持续时间与IBI的高度观测值和风暴类型之间都没有相关性。不论暴风雨的类型和卫星的高度如何，在春分期间，IBI的季节性发生都较大，反之亦然。在春分点期间，大量的IBI与先前的研究一致，后者期望大的电子密度是更陡峭的显影剂。在夏季的午夜之前和春分时的日落时分，观察到大量的超级风暴IBI是一种新颖的观测，需要进一步研究。此外，大多数IBI都在地磁亚暴发生几小时后观察到，这反映了扰动发电机电场（DDEF）作为IBI的主要驱动力。他们期望大的电子密度是陡峭的显影剂。在夏季的午夜之前和春分时的日落时分，观察到大量的超级风暴IBI是一种新颖的观测，需要进一步研究。此外，大多数IBI都在地磁亚暴发生几小时后观察到，这反映了扰动发电机电场（DDEF）作为IBI的主要驱动力。他们期望大的电子密度是陡峭的显影剂。在夏季的午夜之前和春分时的日落时分，观察到大量的超级风暴IBI是一种新颖的观测，需要进一步研究。此外，大多数IBI都在地磁亚暴发生几小时后观察到，这反映了扰动发电机电场（DDEF）作为IBI的主要驱动力。