2019MNRAS.485.3816P

The emission process of Fast Radio Bursts (FRBs) remains unknown. We investigate whether the synchrotron maser emission from relativistic shocks in a magnetar wind can explain the observed FRB properties. We perform particle-in-cell (PIC) simulations of perpendicular shocks in cold pair plasmas, checking our results for consistency among three PIC codes. We confirm that a linearly polarized X-mode wave is self-consistently generated by the shock and propagates back upstream as a precursor wave. We find that at magnetizations σ >= 1 (i.e. ratio of Poynting flux to particle energy flux of the pre-shock flow) the shock converts a fraction f_ξ^′^ ~7 ×10^–4/σ ^2 of the total incoming energy into the precursor wave, as measured in the shock frame. The wave spectrum is narrow-band (fractional width <=1-3), with apparent but not dominant line-like features as many resonances concurrently contribute. The peak frequency in the pre-shock (observer) frame is ω^′′^_ peak_ ~3 γ_ s | u_ ω_ p_, where γ_s|u is the shock Lorentz factor in the upstream frame and ω_p the plasma frequency. At σ >= 1, where our estimated ω^′′^_ peak_ differs from previous works, the shock structure presents two solitons separated by a cavity, and the peak frequency corresponds to an eigenmode of the cavity. Our results provide physically grounded inputs for FRB emission models within the magnetar scenario.