Variations of the median coefficient of accretion C_a and the median coefficient of drag C_d vs. upstream Mach number ﹩{{ \mathcal M }}_{\infty }﹩ for the (Γ_s, γ) = (4/3, 4/3) simulations (top panels) and (Γ_s, γ) = (5/3, 5/3) simulations (bottom panels). C_a (C_d) vs. ﹩{{ \mathcal M }}_{\infty }﹩ curves are shown for each q_r value at which simulations are performed. C_a is obtained by normalizing the mass accretion rate in the system to the HL theory mass accretion rate. C_d is obtained by normalizing the drag force in the system to the HL theory drag force. The C_a and C_d median values are computed in the simulation time range ﹩10{R}_{{\rm{a}}}/{v}_{\infty }\lt t\lt 30{R}_{{\rm{a}}}/{v}_{\infty }﹩. For a fixed, small mass ratio q_r, a higher ﹩{{ \mathcal M }}_{\infty }﹩ corresponds to a steeper upstream density gradient that breaks the symmetry of the flow, causing a reduction in C_a, and a greater quantity of dense material gravitationally focused from the deep stellar interior, which increases C_d.