Flux as detected by PSP in the outbound part of each orbit, compensated for by R^{−2 5}, grouped by orbital groups. Individual encounters within a group are distinguished by markers of different shape or color. The solid lines are the power-law least squares fits to the observed flux, an exponent of which is shown in the top left corner of each panel. To demonstrate the approximate accuracy of the R^{−2 5} scaling, the dashed lines are the power-law fits of the data, with the exponent offset by ±0.3 from the least squares fit.