  Recent surveys have identified seven hypervelocity stars (HVSs) in the halo
of the Milky Way. Most of these stars may have originated from the breakup of
binary star systems by the nuclear black hole SgrA*. In some instances, the
breakup of the binary may lead to a collision between its member stars. We
examine the dynamical properties of these collisions by simulating thousands of
different binary orbits around SgrA* with a direct N-body integration code. For
some orbital parameters, the two stars collide with an impact velocity lower
than their escape velocity and may therefore coalesce. It is possible for a
coalescing binary to have sufficient velocity to escape the galaxy.
Furthermore, some of the massive S-stars near Sgr A* might be the merger
remnants of binary systems, however this production method can not account for
most of the S-stars.
