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\section{Summary and conclusion}
\label{sect:conclusion}
In a CTTS system stellar wind and disk wind interact. The high pressure of the disk wind can
collimate confine the
free stellar wind into a
directed jet. This collimation builds up a narrow, jet-like region, bound by an elongated shock
surface within the stellar wind and for surface. For reasonable parameters of $\dot M$, $v_\infty$, $\omega_0$ and $P(z)$ the shock surface encloses a region only
few several AU wide
and a few but tens of
AU extended AUs along the jet axis.
Paper~I shows that the post-shock cooling zone behind this shock front is of similar size.
This The shock surface is so small that it cannot be resolved with current instrumentation and therefore cannot be seen directly as
a cavity in the disk wind. A small fraction of the stellar wind is shocked to X-ray emitting temperatures $>1$~MK.
Paper~I showed that a shock with these properties is required to explain the observed X-ray emission in the CTTS
DG~Tau and here we now explain how these DG~Tau. We show that such a shock
properties naturally
arise arises in a scenario where the stellar wind is
collimated confined by
the an external presure and feeds the innermost layers of the jet.
Furthermore, \citet{2013A&A...550L...1S} observed C\;{\sc iv} emission in DG Tau that is formed at cooler temperatures than
the those required for X-ray emission and that is too luminous to be explained by cooled X-ray plasma alone. Our solutions to the ODE almost all have more plamsa heated to 0.5~MK
then than to 1~MK and can
thus in principle explain these observations as well.
However, more detailed numerical simulations of the post-shock cooling zone and the shape of the contact discontinuity between the disk wind and the post-shock stellar wind are required to check
weather whether the physical
extend extent of the cooling region behind the shock front and the position of the peak C\;{\sc iv} emission can be matched to the observations at the same time.
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 AUs from the star.
In summary, a fast stellar wind that is
collimated confined by
an 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 viable explanation of the soft X-ray and FUV emission
as observed at the base of young stellar jets, specifically in DG~Tau.
Acknowledgement: This work is supported in part by XXX (Hans) and NSF AST1313083 and NASA NNX14AB38G (ZYL).
