We present adaptive mesh refinement ( AMR ) hydrodynamical simulations of the interaction between Type Ia supernovae and their companion stars within the context of the single-degenerate model .
Results for 3D red-giant companions without binary evolution agree with previous 2D results by Marietta et al .
We also consider evolved helium-star companions in 2D .
For a range of helium-star masses and initial binary separations , we examine the mass unbound by the interaction and the kick velocity delivered to the companion star .
We find that unbound mass versus separation obeys a power law with index between -3.1 and -4.0 , consistent with previous results for hydrogen-rich companions .
Kick velocity also obeys a power-law relationship with binary separation , but the slope differs from those found for hydrogen-rich companions .
Assuming accretion via Roche-lobe overflow , we find that the unbound helium mass is consistent with observational limits .
Ablation ( shock heating ) appears to be more important in removing gas from helium-star companions than from hydrogen-rich ones , though stripping ( momentum transfer ) dominates in both cases .