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The nature of the progenitor systems of Type Ia supernovae is stilluncertain. One way to distinguish between the single-degenerate scenario (SDS)and double-degenerate scenario (DDS) is to search for the post-impact remnantstar. To examine the characteristics of the post-impact remnant star, we havecarried out three-dimensional hydrodynamic simulations of supernova impacts onmain sequence-like stars. We explore the evolution of the post-impact remnantsusing the stellar evolution code MESA. We find that the luminosity and radiusof the remnant star dramatically increase just after the impact. After theexplosion, post-impact companions continue to expand on a progenitor-dependenttimescale of $\sim 10^{2.5-3} $ yr before contracting. It is found that thetime evolution of the remnant star is dependent on not only the amount ofenergy absorbed, but also on the depth of the energy deposition. We examine theviability of the candidate star Tycho G as the possible remnant companion inTycho's supernova by comparing it to the evolved post-impact remnant stars inour simulations. The closest model in our simulations has a similar effectivetemperature, but the luminosity and radius are twice as large. By examining theangular momentum distribution in our simulations, we find that the surfacerotational speed could drop to $\sim 10$ km s$^{-1}$ if the specific angularmomentum is conserved during the post-impact evolution, implying that Tycho Gcannot be completely ruled out because of its low surface rotation speed.

Evolution of Post-Impact Companion Stars in SN Ia Remnants within the Single-Degenerate Scenario