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Recently, the discovery of Galactic FRB 200428 associated with a X-ray burst(XRB) of SGR 1935+2154 has built a bridge between FRBs and magnetar activities.In this paper, we assume that the XRB occurs in the magnetar magnetosphere. Weshow that the observational properties of FRB 200428 and the associated XRB areconsistent with the predictions of synchrotron maser emission atultrarelativistic magnetized shocks, including radiation efficiency, similarenergy occurrence frequency distributions, and simultaneous arrive times. Itrequires that the upstream medium is a mildly relativistic baryonic shellejected by a previous flare. The energy injection by flares responsible for theradio bursts will produce a magnetar wind nebula, which has been used toexplain the persistent radio source associated FRB 121102. We find that theradio continuum around SGR 1935+2154 can be well understood in the magnetarwind nebula model, by assuming the same energy injection rate $\dot{E} \proptot^{-1.37}$ as FRB 121102. The required baryonic mass is also estimated form theobservations of FRB 121102 by GBT and FAST. By assuming the same radiationefficiency $\eta \sim 10^{-5}$, the total baryonic mass ejected from thecentral magnetar is about 0.005 solar mass. This value is much larger than thetypical mass of a magnetar outer crust, but is comparable to the total mass ofa magnetar crust.

Understanding FRB 200428 in the synchrotron maser shock model: consistency and possible challenge