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Like most galaxies, the Milky Way harbors a supermassive black hole (SMBH) atits center, surrounded by a nuclear star cluster. In this dense star cluster,direct collisions can occur between stars before they evolve off themain-sequence. Using a statistical approach, we characterize the outcomes ofthese stellar collisions within the inner parsec of the Galactic Center (GC).Close to the SMBH, where the velocity dispersion is larger than the escapespeed from a Sun-like star, collisions lead to mass loss. We find that thestellar population within $0.01$ pc is halved within about a Gyr because ofdestructive collisions. Additionally, we predict a diffuse population ofpeculiar low-mass stars in the GC. These stars have been divested of theirouter layers in the inner $0.01$ pc before migrating to larger distances fromthe SMBH. Between $0.01$ and $0.1$ pc from the SMBH, collisions can result inmergers. Our results suggest that repeated collisions between lower mass starscan 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 Gobjects, dust and gas enshrouded stellar objects, that may result frommain-sequence stellar collisions. Lastly, we comment on uncertainties in ourmodel and possible connections between stellar collisions and the missing redgiants in the GC.

Stellar Collisions in the Galactic Center: Massive Stars, Collision Remnants, and Missing Red Giants