A cartoon illustrating the outcomes of binary disruption, leading to rpTDEs and stellar EMRIs. In the first stage, a stellar binary is randomly scattered by background stars and gets disrupted when the pericenter distance r_p approaches r_t,b. Immediately after binary disruption, the captured star has a pericenter distance larger than the stellar tidal radius r_t. In the second stage, the captured star is either (i) randomly scattered by background stars (when t_J ≲  t_GW) and finally ends as an rpTDE when it diffuses to the loss-cone boundary of rpTDEs r_p ≃ 2r_t, or (ii) is driven by gravitational radiation (when t_GW ≲ t_J) to become a stellar EMRI.