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Recent follow-up observations of the binary neutron star (NS) merging eventGW170817/SGRB 170817A reveal that its X-ray/optical/radio emissions arebrightening continuously up to $\sim 100$ days post-merger. This late-timebrightening is unexpected from the kilonova model or the off-axis top-hat jetmodel for gamma-ray burst afterglows. In this paper, by assuming that themerger remnant is a long-lived NS, we propose that the interaction between anelectron-positron-pair ($e^+e^-$) wind from the central NS and the jet couldproduce a long-lived reverse shock, from which a new emission component wouldrise and can interpret current observations well. The magnetic-field-inducedellipticity of the NS is taken to be $4 \times 10^{-5}$ in our modeling, sothat the braking of the NS is mainly through the gravitational wave (GW)radiation rather than the magnetic dipole radiation, and the emissionluminosity at early times would not exceed the observational limits. In ourscenario, since the peak time of the brightening is roughly equal to thespin-down time scale of the NS, the accurate peak time may help constrain theellipticity of the remnant NS. We suggest that radio polarization observationsof the brightening would help to distinguish our scenario from other scenarios.Future observations on a large sample of short gamma-ray burst afterglows ordetections of GW signals from merger remnants would test our scenario.

Brightening X-ray/Optical/Radio Emission of GW170817/SGRB 170817A: Results of an Electron-Positron Wind from the Central Engine?