The mass accretion rate in our disk is comparable to that of an α-theory with vigorous turbulence (e.g., α ∼ 1). Here, we compare the radial dependence of the mass accretion rate in the wind (﹩{\dot{M}}_{\mathrm{wind}};﹩ dash–dotted blue line), the disk (﹩{\dot{M}}_{\mathrm{disk}};﹩ dashed red line), and in the total system (﹩\dot{M};﹩ thick solid black line), with an analytical prediction for the mass accretion rate given three values for the α prescription (﹩{\dot{M}}_{\mathrm{SS}};﹩ thin solid gray lines). We can see that an α ∼ 1 analytic prediction is closest to the actual mass accretion rate within the system. ﹩{\dot{M}}_{\mathrm{disk}}﹩ roughly obeys a power law with radius ∼r ^0.4. Since the angular momentum transport obeys a ∼r ^0.9 power law (Figure 4), this is consistent with a (sub-)Keplerian specific angular momentum profile ∼r ^0.5.