Atlantic Anomaly (SAA), they precipitate there. For this reason, fluxes of quasi-trapped particle in the forbidden zone are low on average, and occasional enhancements quickly decay to a background level within a few hours during periods of geomagnetic quiet. On the other hand, flux enhancements that last for several days are often observed, which indicate external driving [3]. Currently, the catalog of the \(>\)30 keV quasi-trapped electron flux enhancements in the forbidden zone, called forbidden energetic electrons (FEEs), contains more than 700 daily global maps of the flux intensity distribution from 1998 to present and is continuously updated [5]. Statistical studies based on the catalogue [4; 6] revealed close relationships between the frequency of \(>\)30 keV FEE occurrence and the solar and interplanetary parameters on a long time scale (years), and with the dipole tilt angle on a medium time scale (months). Studies of a relation between FEEs and geomagnetic activity [3; 7] concluded that neither the intensity of the storm-time ring current nor the substorm auroral electrojet have a significant effect on the occurrence of FEEs. Moreover, periods of calm are not an exception for FEE increases. A comprehensive analysis of the most prominent FEE case during quiet time revealed its connection with local compressions of the dayside magnetosphere, which were caused by transient foreshock-associated pressure pulses [8]. However, the question of what the specific external drivers of FEE enhancements might be remains open. The special case mentioned motivates us to take a closer look at the solar wind parameters for FEE events in our study. Before going into to the details of the problems associated with FEEs, we should note here that the possible influence of the equatorial electrojet on the dynamics of energetic particles in the inner ERB was studied from early years, e.g., [9; 10; 11]. The role of the SAA area in the ionosphere-magnetosphere coupling is especially important, and we will return to this issue in the Section 4. The next question concerns the source of electron flux enhancements at the lower L-shells. [PERSON] et al. [7] found experimental evidence that the source of these electrons is the inner ERB. Moreover, studies of the inner ERB have shown that the inner belt itself is not in a stationary state, as was long believed, and energetic electron fluxes can suddenly increase not only during major geomagnetic storm [12; 13] but even during weak and moderate storms [14]. Long-term particle measurements by Van Allen Probes and DEMETER also showed the occurrence of rapid increases of tens to hundreds of keV electrons in and below the inner belt [15; 16; 17]. The outer belt has been shown to be the source for the enhancements in the inner belt, while the plasma sheet injections were not necessarily related to this. Flux enhancements in the radiation belts are considered to be of two types: slow and fast. A slow increase occurs over several days and is associated with diffusive radial transport. Observations showed that diffusive transport does not extend inside \(L=2\)[15]. By contrast, fast increase (injection) occurs over hours or even less and is associated with radial drift in crossed electric and magnetic fields (e.g., [18]). Thus, it has been established that the observed increases in the electron fluxes both in the inner belt core and below its edge, in the forbidden zone, are earthward injections [1; 2; 15]. According to observations obtained from Van Allen Probes in highly elliptical orbit, electron injections into the inner belt can occur within 3 h over a relatively short distance of tenths of the L-parameter, while observations from the NOAA/POES low-orbit satellites estimated FEE injections on a 1 h timescale over a distance of -0.1 L. In the current study, we will determine this time experimentally on the basis of detailed analysis. Since the characteristic time of FEE enhancement corresponds to the fast radial transport, an electric drift mechanism was proposed [1].