} \right)^{9/16} \nonumber \\
&\simeq 1.2 h^{-3/4} M_{\rm thermal} \simeq 11 \left( \frac{0.054}{h} \right)^{3/4} M_{\rm thermal}  \,.\end{aligned}$$

For $M<M_{\rm repulsion,visc}$, consumption dominates and the planet accretes nearly all the disc gas that tries to diffuse past; for $M > M_{\rm repulsion,visc}$, repulsion dominates and the planet’s accretion rate falls below the disc accretion rate. The above expression for $M_{\rm repulsion, visc}$ depends on our assumption that planetary accretion follows our Hill scaling $A_{\rm Hill} \propto m^{2/3}$ for super-thermal masses. As discussed in section \[sec:oom\], this assumption might not be correct. If instead of $A_{\rm Hill}$ we use $A_{\rm TW} = 0.29 \,\Omega r^2 \,m^{4/3}/h^2$ as found from the 2D numerical simulations of @tw_2002, we would find $A_{\rm TW}/(3\pi B) \simeq 4 \,( M_\mathrm{p}/M_\mathrm{J} )^{-2/3} ( h/0.054)$, in which case the mass above which repulsion dominates would change to $M_{\rm repulsion,visc,TW} \simeq 9 \, M_{\rm J} \,[r / (10 \, {\rm au})]^{3/8}$. This is nearly twice the value of $M_{\rm repulsion,visc}$ given by (\[eqn:repulsionmass\]), and would imply a more extended consumption-dominated growth phase. Insofar as our nominal model adopts $A_{\rm Hill}$ which leads to a more limited consumption-dominated growth phase, the planet masses we compute for our viscous disc model are 