deletions | additions       diff --git a/We_use_the_numerical_hydrodynamics__.tex b/We_use_the_numerical_hydrodynamics__.tex  index dcf25b4..6679849 100644  --- a/We_use_the_numerical_hydrodynamics__.tex  +++ b/We_use_the_numerical_hydrodynamics__.tex 
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The line driving computations have been only slightly modified to port it from Fortran 77 to Fortran 90. The basic method remains the same as in Owocki 1991a, and Owocki \& Puls 1996. Line driving in these winds relies on Doppler shifting to leverage the absorption from optically thick lines, but this results in strong non-local effects within the wind. To capture this phenomenon without doing computationally expensive radiation transport, we use the Smooth Source Function method (SSF) which accounts for absorption between the wind and star, as well as radial, scattered diffuse radiation. We also apply the Eddington limb darkening described in Sundqvist 2013.  TWO OR THREE PARAGRAPHS DESCRIBING \subsection{Line Strength}  \textit{Not sure how to approach this section -- recap Sundqvist 2013? Go into more detail about the line strength cutoff? Express concern about Qmax and clumping}  \begin{itemize}  \item  CAK LINE LIST EXPONENT AND EXPONENTIAL CUTOFF QMAX. WE'VE THOUGHT ABOUT THIS A LOT, MIGHT AS WELL WRITE DOWN SOME OF IT. line list (some justification or citation that our exponent is correct)  \item Talk about Qbar, Qmax, cite Gayley, and discuss linear relationship with metallicity.  \end{itemize}  \subsection{Boundary Conditions}  \begin{itemize}  \item Fix density by computing mCAk mass loss rate, apply Qmax cutoff correction  \item Describe simulation grid and starting radius at sonic point  \item Lower boundary perturbations, cite empirical evidence for it, justify our choices.  \end{itemize}