Characteristic strain of the GW signal released by the merger of two main-sequence stars (in blue) assuming a distance of 1 kpc to the source along the polar axis. The LISA sensitivity from Robson et al. (2019) is shown by the dashed orange line. 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 the star is disrupted (assuming the orbits to be perfectly circular and Keplerian).