## 5 Conclusions  
We have studied the flux enhancements of the \(>\)30, \(>\)100, and \(>\)300 keV quasi-trapped electrons (FEE) below the inner radiation belt (\(L<\) 1.2) during three super storms in 2001, 2004, and 2024. These FEE enhancements were the first observed after the super storm onset. We showed that the enhancements were rapid and can be explained by the inward radial transport provided by the electric drift mechanism. Using particle measurements from the NOAA/POES satellite fleet, we determined a timescale of electron injection that indicates the characteristic rate of electric drift, and then calculated the magnitude of the electric field corresponding to this rate. Analysis of the interplanetary parameters showed that the abrupt changes in the solar wind dynamic pressure may cause the FEE enhancements. The type of interplanetary structure was a magnetic cloud and an interplanetary sheath with Bz > 0. Our results are summarized below:  
1. The occurrence of the FEE increases does not show any preference for any phase (early/maximum in main and recovery phases) of the super storms that confirms the results of previous studies. 2. No FEE enhancements were observed during SSC/SI of the super storms. 3. The FEE enhancement in each super storm was found to be associated with the abrupt change of the solar wind pressure. 4. It was revealed that the sign of the solar wind pressure jump determines the local time sector in which injections can occur: the nighttime FEE injection is observed under a positive jump, and vice versa. 5. The increases in the fluxes of the energetic quasi-trapped electrons occur within 20 min after the impact of a pressure jump. 6. The results substantiate the conclusion about the action of the electric drift mechanism. The dynamics of FEE injection with a characteristic time of \(\sim\)20 min is required for an electric field of about 10 mV/m in order to move electrons from the L-shell 1.2 to 1.1. The nature of the electric field is rather inductive (transient), because a sharp pressure jump causes a geomagnetic field to change rapidly over time, and IMF conditions for penetration of the enhanced large-scale convection field are inconsistent with either daytime or nighttime first injections. The following supporting information can be downloaded at: [[https://www.mdpi.com/article/10.3390/universe11070226/s1](https://www.mdpi.com/article/10.3390/universe11070226/s1)]([https://www.mdpi.com/article/10.3390/universe11070226/s1](https://www.mdpi.com/article/10.3390/universe11070226/s1)). [PERSON] conceptualized the idea, performed the formal analysis and wrote the original draft of the manuscript. [PERSON] developed the data analysis software and contributed to the interpretation of the results. All authors contributed to the editing of the final manuscript. All authors have read and agreed to the published version of the manuscript. This research received no external funding. All the data used in this study are publicly available. The NOAA/POES data were obtained from [[https://www.ngdc.noaa.gov/stp/satellite/poes/](https://www.ngdc.noaa.gov/stp/satellite/poes/)]([https://www.ngdc.noaa.gov/stp/satellite/poes/](https://www.ngdc.noaa.gov/stp/satellite/poes/)), accessed on 15 March 2025. The solar wind parameters were obtained from NASA Goddard Space Flight Center's CDAWeb [[https://cdaweb.gsfc.nasa.gov](https://cdaweb.gsfc.nasa.gov)]([https://cdaweb.gsfc.nasa.gov](https://cdaweb.gsfc.nasa.gov)), accessed on 15 April 2025, geomagnetic indices [[http://supermag.jhuapledu/](http://supermag.jhuapledu/)]([http://supermag.jhuapledu/](http://supermag.jhuapledu/)) (accessed on 4 July 2025). The author is grateful to the NOAA team for providing experimental data on energetic particles measured by the POES and MetOp satellites. The author is grateful to the CDAWeb team for providing free public database of the solar wind from ACE and Wind monitors. We gratefully acknowledge the SuperMAG and INTERMAG collaborators.