Schematic of our proposed scenario. Hadronic particles with position r(t) (shown in red) are initially shocked by the SNR forward shock R_SNR, fs. They then travel from the reservoir region (volume V_Res, shown in blue) between the R_SNR, fs and the PWN radius to the pulsar wind termination shock R_WTS. Following re-acceleration, they advect outwards with the pulsar wind (velocity v_W, shown by the green arrow) to hit the reservoir region from which they originated. The black star denotes the pulsar’s position. In a system as old as Crab, the supernova reverse shock R_SNR, rs still travels outwards.