When a binary star passes close to a massive black hole (BH) at a
galactic centre, it can undergo tidal disruption: one star is ejected
while the other remains on a tightly bound orbit around the BH. Over
time this process produces a cluster of tightly bound stars and
collisional supernovae at the galactic centre. Although the BH tide is
often discussed in the context of stretching objects, the binary
members are not just separated at the BH encounter. Previous point
particle simulations show that the highest ejection velocity are
obtained when binary stars, under the action of the BH tides, get
closer to each other before the binary dissolves. The binaries could
become very compact before the disruption. They might collide and
merge or tidally disrupt each other. We discuss the two kinds of the
collisional events and their implications to Time Domain Astronomy.