  The star S0-2, which is orbiting Sgr A* with a 15-yr period, almost certainly
did not form in situ. We propose that it was injected into this close orbit by
the tidal disruption of a massive-star binary, whose primary was more massive
than S0-2 and at least 60 Msun. From numerical integrations we find that 1-2%
of incoming binaries with closest approach equal to 130 AU leave the secondary
in an orbit with eccentricity within 0.01 of that of SO-2. If additional stars
are found orbiting Sgr A* with relatively short periods, they could be used to
probe the formation of massive stars in the Galactocentric region, even though
the massive stars themselves have long since perished.
