deletions | additions       diff --git a/disk_winds.tex b/disk_winds.tex  index 4e9523e..02758b1 100644  --- a/disk_winds.tex  +++ b/disk_winds.tex 
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\citet{2009A&A...502..217M} present analytical and numerical solutions for several scenarios that mix an inner, presumably stellar, wind and an outer disk wind. In contrast to our approach, they impose a smooth transition between stellar wind and disk wind, which allows them to model the entire outflow region numerically. With some time variability in the wind launching their models produce promising knot features in the jet. In the context of our analysis, we note that the presure in their models is magnetically dominated and much higher close to the jet axies than at larger radii in apparent contrast to Kompaneet's approximation. However, the an inner jet component as suggested in this article is so narrow that it essentiall stays confind to the innermost resolution elements. The presure at the jet axis is high initially and reaches a plateau after dropping by one to two orders of magnitude. Below we use simple exponential or power-law functions for P(z) that mimic this behaviour.  Similar profiles for the inner density and presure are seen in \citet{Li_Krasnopolsky_Blandford_2006}.     http://adsabs.harvard.edu/abs/2010A%26A...516A...6S   compared this to Bacciotti type HST data, but since X-ray shock not visible there that does not really help us for the context of this article. simulations by competing groups \citep[e.g.]{http://dx.doi.org/10.1086/432040,Li_Krasnopolsky_Blandford_2006,http://adsabs.harvard.edu/abs/2008ApJ...678.1109M}.