For those destabilised triples that remain bound, where are those systems compared to the stability limit? This is quantified by the ratio of a_out/a_in|_crit (that is the stability criterion of Eq. (1) over the current configuration (that is a_out/a_in). When the ratio is larger than 1, the system is considered to be in the dynamically unstable regime. If the ratio is smaller than 1, the system is dynamically stable. On the top we show the systems that remain bound after a Hubble time, on the bottom those systems that remain bound after simulating the dynamically unstable phase for 24 h. Solid, dashed, and dotted line styles represent the models for the initial population of triples OBin, T14 and E09, respectively.