Summary of energetic particles following the stream interaction region: (top) EPI-Hi proton fluxes (sunward directed particles in blue, anti-sunward particles in red) from 1–10 MeV, (panel 2) EPI-Lo proton fluxes as a function of energy and time, (panel 3) EPI-Lo proton fluxes as a function as a function of time from 200–500 keV, (panel 4) density measured by SWEAP,(panel 5) solar wind speed measured by SWEAP, and (panel 6) magnetic field measured by FIELDS. This figure is similar to Fig. 2 of Joyce et al. (2021); the only difference is in panel 3, which is shown from 100–500 keV H⁺ in Joyce et al. (2021).