Relativistic electrons cause internal charging on satellites and are a significant space weather hazard. In this study we analyse approximately 20 years of data from the US Global Positioning System (GPS) satellite NS41 to determine the conditions associated with the largest daily averaged fluxes of E = 2.0 MeV relativistic electrons. The largest flux events at L = 4.5 and L = 6.5 were associated with moderate to strong coronal mass ejection (CME)-driven geomagnetic storms. However, the majority of the fifty largest flux events at L = 4.5 (30 out of 50) and L = 6.5 (37 out of 50) were associated with high speed solar wind streams from coronal holes. Both solar drivers are thus very important for relativistic electron flux enhancements in GPS orbit. The 1 in 3 year flux level was not exceeded following any of the fifteen largest geomagnetic storms as monitored by the Dst index (Disturbance storm time index), showing that the largest geomagnetic storms, most often associated with extreme space weather, do not result in significantly larger relativistic electron flux events in GPS orbit.

The datasets include a summary plot of the month associated with the largest flux of 2.0 MeV electrons in GPS orbit during the study period (Figure 1) and a summary plot of the month associated with the largest geomagnetic storm during the study period (Figure 2). The fifty largest 2.0 MeV flux events at L = 4.5 as a function of the minimum Dst of the associated storm are provided in Figure 3.csv, the peak 2.0 MeV electron fluxes associated with the fifteen largest geomagnetic storms at L = 4.5 as a function of the minimum Dst of each of the storms are provided in Figure 4.csv, and the fifty largest 2.0 MeV flux events at L = 4.5 and the sunspot number are provided as a function of time in Figure 5_events.csv and Figure_5_sunspots.csv respectively. The characteristic widths of the fifty largest flux enhancements at L = 4.5 and L = 6.5 are provided in Figure 6.csv. Finally, the fifty largest 2.0 MeV flux events at L = 6.5 as a function of the minimum Dst of the associated storm are provided in Figure 7.csv, the peak 2.0 MeV electron fluxes associated with the fifteen largest geomagnetic storms at L = 6.5 as a function of the minimum Dst of each of the storms are provided in Figure 8.csv, and the fifty largest 2.0 MeV flux events at L = 6.5 and the sunspot number as a function of time are provided in in Figure 9_events.csv and Figure_9_sunspots.csv respectively.

The research leading to these results has received funding from the Natural Environment Research Council (NERC) grants NE/V00249X/1 (Sat-Risk), NE/X000389/1 and NE/R016038/1.