deletions | additions       diff --git a/mass loss rates.tex b/mass loss rates.tex  index 1db7e0e..0e0bcff 100644  --- a/mass loss rates.tex  +++ b/mass loss rates.tex 
...
Typical mass loss rates found in the literature for CTTS outflows are in the range $10^{-10}-10^{-6}M_{\odot}\textrm{ yr}{-1}$ \citep{1999A&A...342..717B,2006A&A...456..189P}. No outflow at all is detected in non-accreting, disk-less T Tauri stars (weak-line TTS or WTTS), \citet{2006ApJ...646..319E} measure values down to $10^{-10}$~M$_{\odot}$~yr$^{-1}$ for some CTTS, but only upper limits for WTTS. In the specific case of the well-studied jet from DG~Tau \citet{1997A&A...327..671L} calculate the mass loss rate as $6.5\cdot 10^{-6}$~M$_{\odot}$~yr$^{-1}$; \citet{1995ApJ...452..736H}  obtain $3\cdot 10^{-7}$~M$_{\odot}$~yr$^{-1}$ and, further out in the jet, \citet{2000A&A...356L..41L} find $1.4\cdot 10^{-8}$~M$_{\odot}$~yr$^{-1}$.   \citet{2009A&A...493..579G} show that a mass loss below $10^{-10}$~M$_{\odot}$~yr$^{-1}$ is sufficient to explain the X-ray emission from the jet as shock heating, and it is possible that the optical jet further out entrains some disk wind material, so it might not track the stellar mass loss correctly.  Therefore, we conservatively We  use $2\cdot 10^{-10}$~M$_{\odot}$~yr$^{-1}$, a value on the low end of the suggested mass loss rates, $10^{-8}$~M$_{\odot}$~yr$^{-1}$  as fiducial stellar mass loss in the remainder of the article. This will contribute only a fraction to the total mass loss of the system, since the disk wind, though slower, operates over a much larger area.  Figure~\ref{fig:dot_m} shows how a larger mass loss rate and therefore a higher density and ram pressure in the stellar wind pushes the shock front out to larger radii and heights. The different shape of the shock front also influences the post-shock temperatures. In the high mass loss rate scenario (black dotted line) the shock front reaches its maximum radius at 400~AU 100~AU  and most of the spherically symmetric wind passes the shock front at shallow angles, so this scenario has the highest fraction of low temperature material.