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An ultra-stripped supernova (SN) is an explosion of a helium or C+O starwhose outer envelope has been stripped away by a companion neutron star. Adouble neutron star (DNS) binary is believed to be left after the explosion,which will emit the gravitational wave later at the coalescence. Recentdetections of a few candidates for the ultra-stripped SN have constrained theproperties of the explosion and the progenitor, but little information is givenas to whether the remnant DNS binary will merge within the cosmic age. A largefraction of the material stripped away from the helium star through the binaryinteraction is expected to escape from the system and form circumstellarmaterial (CSM). The CSM should be traced by radio emission induced by thecollision with the SN ejecta. Based on the stellar evolution models previouslydeveloped, we calculate the expected radio luminosities from ultra-strippedSNe. We find that high radio luminosity at its maximum can be an indicator ofsmall separation of a DNS binary leading to its merger within the cosmic age.Our results can be used to optimize the strategy for the radio follow-upobservations such as observational epochs and frequencies.

Radio Emission from Ultra-stripped Supernovae as Diagnostics for Properties of the Remnant Double Neutron Star Binaries