“…For each of the 109 forward shocks, the driver for each shock was assessed by examining the temporal profile of the solar-wind speed v sw , the magnetic-field strength B mag , the proton temperature T p in comparison with the solarwind speed, the orientation of the magnetic field, the fluctuation level of the magnetic field, the presence or absence of a bidirectional electron strahl, and the presence of magnetic sector reversals. Only 7 of the 107 shocks were consistent with the shock being driven by the interaction of a high-speed stream with slower plasma [shock numbers 7, 11, 26, 35, 38, 42, and 105 in Table 1 of Borovsky (2020d)]; 100 shocks were not consistent with this. Of the 100 shocks, 42 had drivers that were identifiable as coronal mass ejections and 58 had drivers that were not seen or that could not be clearly identified as a coronal mass ejection.…”