  Type Ia supernovae are thought to be caused by thermonuclear explosions of a
carbon-oxygen white dwarf in close binary systems. In the single-degenerate
scenario (SDS), the companion star is non-degenerate and can be significantly
affected by the explosion. We explore this interaction by means of
multi-dimensional adaptive mesh refinement simulations using the FLASH code. We
consider several different companion types, including main-sequence-like stars
(MS), red giants (RG), and helium stars (He). In addition, we include the
symmetry-breaking effects of orbital motion, rotation of the non-degenerate
star, and Roche-lobe overflow. A detailed study of a sub-grid model for Type Ia
supernovae is also presented. We find that the dependence of the unbound
stellar mass and kick velocity on the initial binary separation can be fitted
by power-law relations. By using the tracer particles in FLASH, the process
leading to the unbinding of matter is dominated by ablation, which has usually
been neglected in past analytical studies. The level of Ni/Fe contamination of
the companion that results from the passage of the supernova ejecta is found to
be a $\sim 10^{-5} M_{\odot}$ for the MS star, $\sim 10^{-4} M_{\odot}$ for the
He star, and $\sim 10^{-8} M_{\odot}$ for the RG. The spinning MS companion
star loses about half of its initial angular momentum during the impact,
causing the rotational velocity to drop to a quarter of the original rotational
velocity, suggesting that the Tycho G star is a promising progenitor candidate
in the SDS.
