  Like most galaxies, the Milky Way harbors a supermassive black hole (SMBH) at
its center, surrounded by a nuclear star cluster. In this dense star cluster,
direct collisions can occur between stars before they evolve off the
main-sequence. Using a statistical approach, we characterize the outcomes of
these stellar collisions within the inner parsec of the Galactic Center (GC).
Close to the SMBH, where the velocity dispersion is larger than the escape
speed from a Sun-like star, collisions lead to mass loss. We find that the
stellar population within $0.01$ pc is halved within about a Gyr because of
destructive collisions. Additionally, we predict a diffuse population of
peculiar low-mass stars in the GC. These stars have been divested of their
outer layers in the inner $0.01$ pc before migrating to larger distances from
the SMBH. Between $0.01$ and $0.1$ pc from the SMBH, collisions can result in
mergers. Our results suggest that repeated collisions between lower mass stars
can produce massive ($\gtrsim 10$ M$_\odot$) stars, and there may be $\sim 100$
of them residing in this region. We provide predictions on the number of G
objects, dust and gas enshrouded stellar objects, that may result from
main-sequence stellar collisions. Lastly, we comment on uncertainties in our
model and possible connections between stellar collisions and the missing red
giants in the GC.
