deletions | additions       diff --git a/abstract.tex b/abstract.tex  index fb2ea64..7f6d305 100644  --- a/abstract.tex  +++ b/abstract.tex 
...
Most of the emission of jets from pre main-sequence stars is observed in the optical and IR wavelength range. However, in several cases X-ray and UV observations reveal a weak but highly energetic component in those jets. If this component is heated in shocks then the required velocities are of the order 300~km~$^{-1}$ 300~km~s$^{-1}$  for standing shocks and higher for moving shock fronts. In this article we show that a recollimation boundary layer between a fast stellar wind and a more massive disk wind would have the right properties to explain the observed X-ray emission in this scenario.