Average rpTDE fraction in the loss-cone channel is insensitive to the stellar type or the exact loss-cone boundary β_rpTDE. The four “diagonal” lines are obtained from Equations (18) and (19). In addition, dynamical tides may drive stars from a larger “initial” orbital period T_obt,i to a shorter orbital period T_obt, where the stars repeatedly get disrupted and are observed. As a result, dynamical tides increase the rate of observable rpTDEs by a factor of a few (see Section 2.5). Here the thick blue line is obtained from the light blue line by assuming T_obt = T_obt,i/10.