shown in Figure \[fig:sigma\_detailed\] conform to the analytic considerations of section \[sec:oom\]. For $M_{\rm p} = 0.3 \, M_{\rm J}$ (top panel), conditions are consumption-limited: $\Sigma_+/\Sigma_{\rm p} \sim A_{\rm Bondi}/(3\pi\nu)$ (equation \[eqn:oom2\] in the limit $A_{\rm Bondi}/(3\pi) > B > \nu$) and the surface density of the entire interior disc is depressed relative to the same disc without a planet by a factor of $\Sigma_+ / \Sigma_- \sim \dot{M}_+ / \dot{M}_- \simeq A_{\rm Bondi}/(3\pi B)$ (equations \[eqn:mdot-0\] and \[eqn:mdot-\]). By comparison, for $M_{\rm p} = 10 \, M_{\rm J}$ (bottom panel), the gap is more nearly symmetric, $\Sigma_+/\Sigma_- \sim 1$ (equations \[eqn:mdot-0\] and \[eqn:mdot-\_Hill\]), and deep and repulsion-dominated, $\Sigma_+/\Sigma_{\rm p} \sim B/\nu$ (equation \[eqn:oom2\] in the limit $B > A_{\rm Hill}/(3\pi) > \nu$).

So long as consumption is stronger than repulsion in the sense that $A/(3\pi) > B$—a condition that we have shown always obtains for sub-thermal masses accreting at the Bondi rate, and for sufficiently low-mass super-thermal masses accreting at the Hill rate ($M < M_{\rm repulsion,visc}$)—repulsion does not much affect the gap surface density $\Sigma_{\rm p}$. Figure \[fig:m\_final\_visc\] demonstrates that different choices for the repulsion coefficient $B = \{10^{-2}, 10^{-3}, 10^{-4}\}\times A_{\rm Bondi}$ all yield practically the same 