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The study of short-duration gamma-ray bursts provides growing evidence that agood fraction of double neutron star mergers lead to the formation of stablemillisecond magnetars. The launch of Poynting flux by the millisecond magnetarscould leave distinct electromagnetic signatures that reveal the energydissipation processes in the magnetar wind. In previous studies (Wang & Dai2013b; Wang et al. 2015), we assume that the magnetar wind becomes completelylepton-dominated so that electrons/positrons in the magnetar wind areaccelerated by a diffusive shock. However, theoretical modeling of pulsar windnebulae shows that in many cases the magnetic field energy in the pulsar windmay be strong enough to suppress diffusive shock acceleration. In this paper,we investigate the reverse shock emission as well as the forward shock emissionwith an arbitrary magnetization parameter $\sigma$ of a magnetar wind. We findthat the reverse shock emission strongly depends on $\sigma$, and inparticular, $\sigma \sim 0.3$ leads to the strongest reverse shock emission.Future observations would be helpful to diagnose the composition of themagnetar wind.

Reverse Shock Emission Driven By Post-Merger Millisecond Magnetar Winds: Effects of the Magnetization Parameter