and ${\cal T}=t c^{3}/GM$. A choice of $Q$ and $g_{\theta}$ now allows to numerically integrate trajectories. We take $Q=5 \times 10^{-2}$, and

$$g_{\theta}=e^{-\left( \frac{\theta- \pi/2}{\sqrt{2} \theta_{0}}   \right)^{2}}$$

![The figure gives trajectories for the complete solution, for a range of initial vertical height positions at $R=2$. The dimensionless parameter of the problem was chosen as $Q=5 \times 10^{-2}$. We see the lowermost two trajectories converging into the central potential, but the six upper ones shooting up into a polar jet, where velocities are over 4 orders of magnitude higher than what was originally present along the disk.](fig1.ps)

with $\theta_{0} = 0.38$ radians, or about 22 degrees. This values is far from representing an extremely flattened disk, and hence one which does not force the jet solution, see eq.(44). With these parameters, and initial conditions specified in dimensionless cylindrical coordinates as $R=2$ and $Z$ ranging from 0.4 to 1.4, we solve eqs.(50) and (51) through a finite differences scheme to plot figure 1. For this case, the two lowermost curves present trajectories which all turn downwards to converge onto the central star. These are solutions which essentially follow the background state, infalling onto the bottom of the potential well. As one raises 