Overview of the outcome of triple evolution. About 2–4% of triples destabilise by themselves during their evolution (top panel). These triples commonly consist of three MS stars or contain one or two giant stars (middle right panel). The outcome of the destabilised phase is often an ejection of one of the stars, but collisions are common as well (middle left panel). Collisions preferably occur between MS stars (bottom panel). Fractions are based on our most advanced N-body simulations that includes stellar evolution.