deletions | additions       diff --git a/Wind speed.tex b/Wind speed.tex  index 9f1e6f7..e60715a 100644  --- a/Wind speed.tex  +++ b/Wind speed.tex 
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\subsection{wind \subsection{Wind  speed} The launching mechanism of the stellar wind in CTTS is uncertain. For a solar-type wind, it is not unreasonable to expect similar wind speeds. The solar wind consists of a slow wind with a typical velocity of 400~km~s$^{-1}$ and a fast wind around 750~km~s$^{-1}$ \citep{adsabs.harvard.edu/abs/2005JGRA..11007109F}. The relative contribution and the launching position of the two types changes over the solar cycles, but the slow wind often emerges from regions near the solar equtor and fast wind is generally associated with coronal holes \citep{1999GeoRL..26.2901G,2003A&A...408.1165B,2009LRSP....6....3C}. Despite these differences, the total energy flux in the solar wind is almost independent of the lattitude, because the slower wind is denser than the faster wind \citep{2012SoPh..279..197L}.   In our model, we use a spherically symmetric stellar wind with a constant velocity. For a solar-type wind this works well to derive the shape of the shock front because eqn.~\ref{eqn:r0} contains the total energy flux $\dot E = \rho v^2_\infty \propto \dot M v_\infty$. However, a lower wind velocity and higher density at the equator would lead to lower post-shock temperatures with a higher emission measure close to the disk plane.