deletions | additions       diff --git a/We_fix_all_of_the__.tex b/We_fix_all_of_the__.tex  index d091142..29b15ab 100644  --- a/We_fix_all_of_the__.tex  +++ b/We_fix_all_of_the__.tex 
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We fix all of the model parameters except for the metal content ($\bar{Q}=$ 400, 700, 1000, 1300, 1700, 2000). For the initial condition of each model, we relax a smooth Sobolev solution with the corresponding $\bar{Q}$ value, choosing an inflow density which produces the predicted CAK mass loss rate. In Table X we show the resulting mass loss rates under both the smooth Sobolev solution and under the SSF radiative force, across all models.   Figure XX shows simulation snapshots of the radial variation of velocity and density, corresponding to galactic ($\bar{Q} = 2000$), LMC ($\bar{Q} = 1000$), and SMC ($\bar{Q} = 400$) metal content. Each snapshot was taken after $1.5 \times 10^6$ seconds of simulation, so transients from the initial conditions have fully propagated out of the flow. We see a decreasing mass loss rate as predicted by theory, which manifests as reductions in both the velocity and density.   In Figure XX, we compare the measured clumping factor in the two extreme models ($\bar{Q} = 400$, 2000). The low clumping at the base, followed by a peaking and then slow decrease in structure is apparent, as seen in previous work (Owocki, Runacres, etc). Due to the large radial variations in clumping factor, we make conclusions about the mass-loss rate using two radial ranges which are thought to correspond to the major formation zones of $H_{\alpha}$, Range A (1.05 -- 1.5) and Range B (1.5 -- 2 $R_*$), both of which fall into Puls 2006's "Region 2". (NOTE: How much $H_{\alpha}$ emission do we expect outside of this range? personal communication Jon Sundqvist -- not so much in the inner wind)