deletions | additions       diff --git a/Results.tex b/Results.tex  index 9e0b500..bf3ec04 100644  --- a/Results.tex  +++ b/Results.tex 
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The temperature in our fiducial model stays just below 1~MK -- too little to explain X-ray emission in the jets (Fig.~\ref{fig:result}, solid red line), but small changes in the parameters, well within the observational and theoretical constraints, are sufficient, are sufficient to drive the maximal temperatures over 1~MK for a small fraction of the mass loss (other lines in the figure).   \citet{2009A&A...493..579G} \citet{2009A&A...493..579G}  showed that a small faction, about $10^{-3}$, of the total mass loss rate in the outflow is enough to power the observed X-ray emission at the base of DG~Tau's DG~Tau's  jet. All but the fiducial scenario in Fig.~\ref{fig:result} have a significant, but small fraction of the stellar wind that gets heated to $>1.5$~MK $>1.5$~MK  and thus can easily emit X-rays. In this article we concentrate on the stellar wind mass loss, but in the observations the boundary is not that clear. The slower jet components observed further away from the jet axis carry much of the mass flow \citep{2000ApJ...537L..49B}. Their origin is probably the inner region of the disk and not that star \citep{2003ApJ...590L.107A}. Thus, it is fully consistent that our model predicts a mass loss fraction larger than $10^{-3}$ at X-ray emitting temperatures. If the disk wind dominates the mass loss over the stellar wind, then the fraction of hot gas in the (stellar plus inner disk) jet might still be small.