this case $\theta_{0}$. For the cases presented here values upwards of $10^{3} c$ commonly appear along the jet, much larger than the values of order $c$ present in the disk. These radial velocities are somewhat inexact, but will always present large values for background state configurations which empty towards the poles (c.f. eq.44), and will present larger values as the vertical density gradients increase. Notice that the generic validity of the solution proposed does not require that all of the disk material should loose all of its angular momentum at the critical radius $R_{T}$, only that some of the disk material should loose most of its angular momentum at that point. Any minor, residual angular momentum remaining on the disk fraction which forms the jet will only establish a finite jet cross-sectional area through the appearance of a centrifugal barrier, which will present only a small correction on the scenario given here. Still, the empirical presence of spectroscopically studied accretion disks truncated interior to certain critical radii suggests the very substantial reduction of the shears in that region, as will be the case when a transition to radial flow takes place.

In going back to eqs.(50) and (51) we see 