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In this paper, we study the dynamics of magnetic storms due to interplanetarycoronal mass ejections (ICMEs). We used multi-epoch superposed epoch analyses(SEAs) with a choice of epoch times based on the structure of the events. Bysorting the events with respect to simple large-scale features (presence of ashock, magnetic structure, polarity of magnetic clouds), this method providesan original insight into understanding the variability of magnetic stormdynamics. Our results show the necessity of seeing ICMEs and their precedingsheaths as a whole since each substructure impacts the other and has aneffect on its geoeffectiveness. It is shown that the presence of a shockdrives the geoeffectiveness of the sheaths, while both the shock and themagnetic structure impact the geoeffectiveness of the ICMEs. In addition, weshowed that the ambient solar wind characteristics are not the same forejecta and magnetic clouds (MCs). The ambient solar wind upstream magneticclouds are quieter than upstream ejecta and particularly slower. We alsofocused on the polarity of magnetic clouds since it drives not only theirgeoeffectiveness but also their temporal dynamics. South–north magneticclouds (SN-MCs) and north–south magnetic clouds (NS-MCs) show no differencein geoeffectiveness for our sample of events. Lastly, since it is well-knownthat sequences of events can possibly induce strong magnetic storms, suchsequences have been studied using superposed epoch analysis (SEA) for thefirst time. We found that these sequences of ICMEs are very usual and concernabout 40 <i>%</i> of the ICMEs. Furthermore, they cause much more intensemagnetic storms than isolated events do

Understanding the variability of magnetic storms caused by ICMEs