deletions | additions       diff --git a/Conclusion.tex b/Conclusion.tex  index 3814fad..e1bb6b7 100644  --- a/Conclusion.tex  +++ b/Conclusion.tex 
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There is too much parameter degeneracy to turn the argument around and to derive $\dot M$, $v_\infty$ or $P(z)$ from the fact that we observe X-ray and FUV emission a few tens of AU from the star.  In summary, a fest fast  stellar wind that is collimated by external pressure from the disk wind will form a collimation shock. We derive the geometrical shape and other properties of this shock front and find that this model is a plausible scenario to explain soft X-ray and FUV emission as observed at the base of young stellar jets, specifically in DG~Tau.