  The nature of the progenitor systems of Type Ia supernovae is still
uncertain. One way to distinguish between the single-degenerate scenario (SDS)
and double-degenerate scenario (DDS) is to search for the post-impact remnant
star. To examine the characteristics of the post-impact remnant star, we have
carried out three-dimensional hydrodynamic simulations of supernova impacts on
main sequence-like stars. We explore the evolution of the post-impact remnants
using the stellar evolution code MESA. We find that the luminosity and radius
of the remnant star dramatically increase just after the impact. After the
explosion, post-impact companions continue to expand on a progenitor-dependent
timescale of $\sim 10^{2.5-3} $ yr before contracting. It is found that the
time evolution of the remnant star is dependent on not only the amount of
energy absorbed, but also on the depth of the energy deposition. We examine the
viability of the candidate star Tycho G as the possible remnant companion in
Tycho's supernova by comparing it to the evolved post-impact remnant stars in
our simulations. The closest model in our simulations has a similar effective
temperature, but the luminosity and radius are twice as large. By examining the
angular momentum distribution in our simulations, we find that the surface
rotational speed could drop to $\sim 10$ km s$^{-1}$ if the specific angular
momentum is conserved during the post-impact evolution, implying that Tycho G
cannot be completely ruled out because of its low surface rotation speed.
