Fig. 3.

Median energy-angle distributions for the same three populations in Fig. 2, in the solar wind frame, for energies of 35–400 eV. We normalize both the upward-going and downward-going halves of the electron distribution by the downward-going electron distribution such that the values for upward-going angles (90–180) show the ratio of upward-going flux at angle 180 — α to downward-going flux at the conjugate angle α. This normalization, unlike that in the lower panels of Figs. 1 and 2, removes both the energy and angle dependence of the incoming population, allowing clear identification of departures from electron reflection expected from an adiabatic model (indicated by values above unity).