Characteristic strain of the GW signal of the CE merger (in blue) assuming a polar distance of 1 kpc to the source. The sensitivities of LISA (Robson et al. 2019), DECIGO, and BBO (Yagi & Seto 2011) are shown as dashed orange, green, and red lines, respectively. The region shaded in gray represents the frequency range spanning between twice the orbital frequency at the beginning of the simulation and twice the orbital frequency at the moment when the star is disrupted.