| Abstrak/Abstract |
The behavior of electron flux was studied by examining 42 geomagnetic storms driven by Co-rotating Interaction Regions (CIR) and 48 geomagnetic storms driven by Coronal Mass Ejections (CME). This study used solar wind parameters (Nsw, Vsw, Psw), the Dst index, electron flux, and the interplanetary magnetic field southward-northward (Bz IMF) during solar cycle 24. The results indicate that the decrease in electron flux before (PRE) and during (POST) both CME-driven and CIR-driven storms is likely related to an increase in solar wind speed. For both types of storms, the decrease in electron flux generally begins almost simultaneously with the onset of the geomagnetic storm. The electron flux then starts to rise after the storm returns to normal conditions. The behavior of electron flux following both CME-driven and CIRdriven
geomagnetic storms involves complex processes. |
