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Following the historical observations of GW170817 and its multi-wavelengthafterglow, more radio afterglows from neutron star mergers are expected in thefuture as counterparts to gravitational wave inspiral signals. We wish todescribe these events using our current knowledge of the population of neutronstar mergers coming from gamma-ray burst science, and taking into account thesensitivities of current and future gravitational wave and radio detectors. Wecombine analytical models for the merger gravitational wave and radio afterglowsignals to a population model prescribing the energetics, circum-merger densityand other relevant parameters of the mergers. We report the expecteddistributions of observables (distance, orientation, afterglow peak time/flux,etc.) from future events and study how these can be used to further probe thepopulation of binary neutron stars, their mergers and related outflows duringfuture observing campaigns. In the case of the O3 run of the LIGO-VirgoCollaboration, the radio afterglow of one third of gravitational-wave-detectedmergers should be detectable (and detected if the source is localized thanks tothe kilonova counterpart) by the Very Large Array, and these events should haveviewing angles similar to that of GW170817. These findings confirm the radioafterglow as a powerful insight on these events, though some keyafterglow-related techniques, such as very long baseline interferometry imagingof the merger remnant, may no longer be feasible as the gravitational wavehorizon increases.

Radio afterglows of binary neutron star mergers: a population study for current and future gravitational wave observing runs