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There is accumulating evidence that at least a fraction of binary neutronstar mergers result in rapidly spinning magnetars, with subrelativisticneutron-rich ejecta as massive as a small fraction of solar mass. The ejectacould be heated continuously by the Poynting flux emanated from the centralmagnetars. Such Poynting flux could become lepton-dominated so that a reverseshock develops. It was demonstrated that such a picture is capable ofaccounting for the optical transient PTF11agg (Wang & Dai 2013b). In this paperwe investigate the X-ray and ultraviolet (UV) radiation as well as the opticaland radio radiation studied by Wang & Dai (2013b). UV emission is particularlyimportant because it has the right energy to ionize the hot ejecta at times$t\lesssim 600$ s. It is thought that the ejecta of binary neutron star mergersare a remarkably pure sample of r-process material, about which ourunderstanding is still incomplete. In this paper we evaluate the possibility ofobservationally determining the bound-bound and bound-free opacities of ther-process material by timing the X-ray, UV, and optical radiation. It is foundthat these timings depend on the opacities weakly and therefore only looseconstraints on the opacities can be obtained.

Reverse Shock Emission and Ionization Break Out Powered by Post-merger Millisecond Magnetars