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\section{The model}  In this section we develop an analytical model for the stellar wind that expands along the jet axis. The wind is confined by the pressure of the surrounding disk wind. Those two flows a re separated by a contact discontinuity, whose exact position is given by pressure equilibrium between the outer, disk wind component and the inner, stellar wind component.  We show assume that  the energy radiated in stellar wind is initially emitted radially. As it encounters  the convective region contact discontinuity, the velocity component perpendicular  to be proportional the discontinuity is shocked. Thus, our model needs  to distinguish three zones: (i)  the mass in cold pre-shock stellar wind, (ii)  the radiative layer between host post-shock stellar wind, and (iii) the disk wind. Our goal is to calculate the geometrical shape of  the stellar surface wind shock, since this determines the velocity jump across the shock front  and thus  the upper boundary temperature  of the convective zone, as shown in Figure \ref{fig:fig1} post-shock plasma.     The Rankine-Hugoniot jump conditions relate the density, velocity  and in pressure on both sides of  a tabular form, in Table 1. Both {\it tori} strong shock. For ideal gases  and {\it riq} are designed to measure individuals; aggregations non-oblique shocks the conservation  of individuals such as countries, universities, mass, momentum  and departments, energy across the shock  can be characterized by simple summary statistics, such written  as follows \citep[][chap.~7, \S~15]{http://adsabs.harvard.edu/abs/1967pswh.book.....Z, where  the number state before the front  of scientists and their mean {\it riq}. An extension the shock front is marked by the index 0, that behind the shock by index 1:   \begin{eqnarray}   \rho_0 v_0 &=& \rho_1 v_1 \label{RH1}\\   P_0+\rho_0 v_0^2 &=& P_1+\rho_1 v_1^2 \label{RH2}\\   \frac{5 P_0}{2\rho_0}+\frac{v_0^2}{2}&=&\frac{5 P_1}{2\rho_1}+\frac{v_1^2}{2} \ ,\label{RH3}   \end{eqnarray}   where $\rho$ denotes the total mass density  of {\it tori} to measure journals would the gas and $P$ its pressure.     Initially, the stellar wind is relatively cold and thus the thermodynamic pressure can  be straight forward: it would consist neglected, setting $P_0=0$. In the strong shock limit $v_0=4\;v_1$. With these two simplifications, eqn.~\ref{RH3} yields   \begin{equation}   P_1 = \frac{3}{4} \rho_0 \v_0^2 \label{eqn:4}   \end{equation}     In our case we are dealing with an oblique shock (Figure~\ref{fig:sketch}. Equations~\ref{RH1} to \ref{eqn:4} stay valid if only the velocity component perpendicular to the shock front is taken as $v_0$ and $v_0$.   Figure~\ref{fig:sketch} shows the geometry  of the simple removal problem. We use a cylindrical coordinate system with an origin on the central star. We place the $z$-axis along the jet outflow direction and assume rotational symmetry around the jet axis. Thus, the flow can effectively be written in $(r,z)$.     We treat the disk wind as an outer boundary condition with a given pressure profile and concentrate on the description  of the normalization by stellar wind. To simplify the equations we adopt Kompaneets' approximation \citep{http://adsabs.harvard.edu/abs/1960SPhD....5...46K} which states that there is no axial pressure gradient so that  the number pressure profile  of authors. the disk wind, which is given as a boundary condition, extends through all layers of the outflow:   \begin{equation}   P(z,\theta, r) = P(z)\,.   \end{equation}  \begin{table}   \begin{tabular}{lccccc}   \hline   \textbf{Phase} & \textbf{Time} & \textbf{M$_1$} & \textbf{M$_2$} & \textbf{$\Delta M$} & \textbf{P} \\   1 ZAMS & 0 & 16 & 15 & -- & 5.0 \\   2 Case B & 9.89 & 15.92 & 14.94 & 0.14 & 5.1 \\   3 ECCB & 11.30 & 3.71 & 20.86 & 6.44 & 42.7 \\   4 ECHB & 18.10 & -- & 16.76 & -- & -- \\   5 ICB & 18.56 & -- & 12.85 & -- & -- \\   6 ECCB & 18.56 & -- & 12.83 & -- & -- \\   \hline   \end{tabular}   \caption{\textbf{Some descriptive statistics about fruit and vegetable consumption among high school students in the U.S.} While bananas and apples still top the list of most popular fresh fruits, the amount of bananas consumed grew from 7 pounds per person in 1970 to 10.4 pounds in 2010, whereas consumption of fresh apples decreased from 10.4 pounds to 9.5 pounds. Watermelons and grapes moved up in the rankings.}   \end{table}