Radio luminosity of the PRS as a function of the lifetime of the PRS, assuming no time evolution of the radio luminosity, for the case where a magnetar giant flare powers a PRS from the interaction with the stellar wind of the companion. Solid and dashed lines correspond to different efficiencies of conversion to radio emission (0.05 and 0.005%, respectively), and different sets of lines correspond to different surface magnetic fields of the neutron star, as shown in the legend. The horizontal grey region indicates the observed PRS luminosity of FRB 20121102A taken from Chen et al. (2022).