Following the detection of the GW170817 signal and its associated electromagnetic emissions, we discuss the prospects of the local Hubble parameter measurement using double neutron stars (DNSs). The kilonova emissions of GW170817 are genuinely unique in terms of the rapid evolution of color and magnitude and we expect that, for a good fraction $gtrsim 50%$ of the DNS events within $sim 200$Mpc, we could identify their host galaxies, using their kilonovae. At present, the estimated DNS merger rate $(1.5^{+3.2}_{-1.2})times 10^{-6} {rm Mpc^{-3} yr^{-1}}$ has a large uncertainty. But, if it is at the high end, we could measure the local Hubble parameter $H_L$ with the level of $Delta H_L/H_Lsim 0.042$ ($1sigma$ level), after the third observational run (O3). This accuracy is four times better than that obtained from GW170817 alone, and we will be able to examine the Hubble tension at $2.1sigma$ level.
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