Characteristic strain of the GW signal released by the CE merger (in blue) assuming a distance of 1 kpc to the source along the polar axis. 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 (assuming the orbits to be perfectly circular and Keplerian). The black lines show the characteristic strain produced by our toy models.