deletions | additions       diff --git a/our_equations.tex b/our_equations.tex  index 393ee84..9fdd255 100644  --- a/our_equations.tex  +++ b/our_equations.tex 
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\label{eqn:RH3}\frac{5 P_0}{2\rho_0}+\frac{v_0^2}{2}& = &\frac{5 P_1}{2\rho_1}+\frac{v_1^2}{2} \ .  \end{eqnarray}  We assume that the stellar wind before the shock front is relatively cool \textbf{(this assumption is justified in Section~\ref{sect:T_0})}  and thus the thermodynamic pressure can be neglected, setting $P_0=0$. The shock front settles at a position where the pressure of the stellar wind equals the post-shock pressure, which in turn determines the position of the contact discontinuity, such that the post-shock pressure equals the confining external pressure of the disk wind $P(z)$ .   In our case we are dealing with an oblique shock (Figure~\ref{fig:sketch}). Equations~\ref{eqn:RH1} to \ref{eqn:RH3} stay valid if only the velocity component perpendicular to the shock front is taken as $v_0$.