Type Ia supernova research is one of the most forward projects in astrophysics and basic physics in 21st century. Type Ia supernovae (SNe Ia) are used as cosmic distance indicators because their luminosity can be calibrated based on the empirical relation between light curve shape and peak luminosity. This leads to the discovery of the accelerating expansion of the present Universe, providing the evidence for the existence of dark energy. This is a great discovery, not only in astronomy, but also in physics. However，the nature of progenitors and the explosion physics of SNe Ia remain unclear. SNe Ia are widely believed to be arisen from thermonuclear explosions of carbon-oxygen white dwarfs (C-O WDs) by accreting material from their non-degenerate (i.e., single degenerate scenario [SD]) or degenerate (i.e., double degenerate scenario [DD]) companion stars. One of obvious differences between SD and DD scenario is that the SD model predict the companion star would survive from the explosion, but the DD model leaves no companion remnant after the explosion. Therefore, it is a promising approach to distinguish and identify the SD and DD model by directly searching for the surviving companion star in galactic SN Ia remnant. In present paper, based on the SD progenitor model, we performed three dimensional hydrodynamical simulations of the impact of SN Ia explosion on their companion stars employing the smoother particle hydrodynamics (SPH) method. We investigated the details of the interactions between the SN Ia ejecta and the companion star. We presented some peculiar characteristics and observable qualities of surviving companion stars of SNe Ia.
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