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We explore the electromagnetic counterparts that will associate with binaryneutron star mergers for the case that remnant massive neutron stars survivefor $\gtrsim 0.5\,$s after the merger. For this study, we employ the outflowprofiles obtained by long-term general-relativistic neutrino-radiationmagneto-hydrodynamics simulations with a mean field dynamo effect. We show thata synchrotron afterglow with high luminosity can be associated with the mergerevent if the magnetic fields of the remnant neutron stars are significantlyamplified by the dynamo effect. We also perform a radiative transfercalculation for kilonovae and find that for the highly amplified magnetic fieldcases, the kilonovae can be bright in the early epoch, while it shows theoptical emission rapid declining in a few days and the long-lasting ($\sim10\,{\rm d}$) emission very bright in the near-infrared wavelength. All thesefeatures have not been found in GW170817, indicating that the merger remnantneutron star formed in GW170817 might have collapsed to a black hole withinseveral hundreds ms or magnetic-field amplification might be a minor effect.

Electromagnetic counterparts of binary neutron star mergers leading to a strongly magnetized long-lived remnant neutron star