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Supernovae of Type Iax (SNe Iax) are an accepted faint subclass ofhydrogen-free supernovae. Their origin, the nature of the progenitor systems,however, is an open question. Recent studies suggest that the weak deflagrationexplosion of a near-Chandrasekhar-mass white dwarf in a binary system with ahelium star donor could be the origin of SNe Iax. In this scenario, the heliumstar donor is expected to survive the explosion. We use the one-dimensionalstellar evolution codes \textsc{MESA} and \textsc{Kepler} to follow thepost-impact evolution of the surviving helium companion stars. The stellarmodels are based on our previous hydrodynamical simulations of ejecta-donorinteraction, and we explore the observational characteristics of thesesurviving helium companions. We find that the luminosities of the survivinghelium companions increase significantly after the impact: They could vary from$2\mathord,500\,\mathrm{L_{\odot}}$ to $16\mathord,000\,\mathrm{L_{\odot}}$ fora Kelvin-Helmholtz timescale of about $10^{4}\,\mathrm{yr}$. After the starreaches thermal equilibrium, it evolves as an O-type hot subdwarf (sdO) starand continues its evolution along the evolutionary track of a normal sdO starwith the same mass. Our results will help to identify the surviving heliumcompanions of SNe Iax in future observations and to place new constraints ontheir progenitor models.

Long-term evolution of post-explosion Helium-star Companions of Type Iax Supernovae