  The strong tidal force in a supermassive black hole's (SMBH) vicinity,
coupled with a higher stellar density at the center of a galaxy, make it an
ideal location to study the interaction between stars and black holes. Two
stars moving near the SMBH could collide at a very high speed, which can result
in a high energy flare. The resulting debris can then accrete onto the SMBH,
which could be observed as a separate event. We simulate the light curves
resulting from the fallback accretion in the aftermath of a stellar collision
near a SMBH. We investigate how it varies with physical parameters of the
system. With all other physical parameters of the system held constant, the
direction of the relative velocity vector at time of impact plays a large role
in determining the overall form of the light curve. One distinctive light curve
we notice is characterized by a sustained increase in the luminosity some time
after accretion has started. We compare this form to the light curves of some
candidate tidal disruption events (TDEs). Stellar collision accretion flares
can take on unique appearances that would allow them to be easily
distinguished, as well as elucidate underlying physical parameters of the
system. There exist several ways to distinguish these events from TDEs,
including the much wider range of SMBH masses stellar collisions may exist
around.
