  In our Galactic Center, about 10,000 to 100,000 stars are estimated to have
survived tidal disruption events, resulting in partially disrupted remnants.
These events occur when a supermassive black hole (SMBH) tidally interacts with
a star, but not enough to completely disrupt the star. We use the 1D stellar
evolution code Kepler and the 3D smoothed particle hydrodynamics code Phantom
to model the tidal disruption of 1, 3, and 10 solar mass stars at zero-age
(ZAMS), middle-age (MAMS), and terminal-age main-sequence (TAMS). We map the
disruption remnants into Kepler in order to understand their post-distribution
evolution. We find distinct characteristics in the remnants, including
increased radius, rapid core rotation, and differential rotation in the
envelope. The remnants undergo composition mixing that affects their stellar
evolution. Whereas the remnants formed by disruption of ZAMS models evolve
similarly to unperturbed models of the same mass, for MAMS and TAMS stars, the
remnants have higher luminosity and effective temperature. Potential
observational signatures include peculiarities in nitrogen and carbon
abundances, higher luminosity, rapid rotation, faster evolution, and unique
tracks in the Hertzsprung-Russell diagram
