Comparison between numerical (orange) and analytic solutions (gray lines). We compare density $\stackrel{\sim }{\rho }$ (top row), velocity toward the accretor ${\stackrel{\sim }{v}}^x$ (middle row), and $\stackrel{\sim }{\rho }{\stackrel{\sim }{v}}^x$ (bottom row) from our simulations along the $\stackrel{\sim }{\mathit{y}}$ axis intersecting the inner Lagrangian point ($\stackrel{\sim }{\mathit{y}}=0$) to the corresponding analytic solutions. We consider equal-mass binaries for both adiabatic – without (left column) and with (middle column) the Coriolis force – and isothermal cases with the Coriolis force (right column).