Solar-wind properties in vicinity of shock #1 (indicated by the vertical red line). Panel a) shows |B| in black, and its RTN components in red, blue, and green. Panel b) shows the Proton-Alpha Sensor (PAS) energy-per-charge spectrum (assuming a charge of one) and shows that the proton-velocity distribution is well captured in energy space. The more abundant protons are visible via the horizontal red line; alpha particles are seen via the yellow line around 10³ “V” before the shock. Panel c) shows proton density (temperature) in black (red). Panel d) shows radial proton velocity in red and total proton speed in black. Panel e) shows the T (blue) and N (green) components of the proton velocity. Vertical dashed lines indicate the times (1) to (9) at which the reduced velocity-distribution functions are shown in Fig. 5.