type of model naturally furnishes a tight disk-jet connection (c.f. eq. 44) e.g., as now firmly established in microquasars and AGN jets (see e.g. Marscher et al. 2002, Chatterjee et al. 2009). In the above systems bursts of enhanced jet activity are seen to follow temporal dips in disk luminosity output after small characteristic delay times. In the present model, such a situation would be expected if the critical radius for transition to radial flow in the disk made a sudden transition to higher values. Again, the drop in disk output might not reflect the disk material disappearing (in this case being swallowed by the central black hole, as sometimes proposed), but simply fading from view as heating mechanisms shut down, then naturally enhancing jet activity as the effective $\dot{M}_{a}$ increases.

Particular Solutions
====================

In order to present a sample of the trajectories expected in the model, we turn to the full solution to the problem, eqs.(21) and (22), but written in dimensionless form:

$$\frac{d {\cal R} }{d {\cal T}} =\frac{-1}{ {\cal R}^{1/2}}+Q {\cal R}^{1/2} \left(\frac{3 cos^{2}(\theta)-1}{g_{\theta}} \right),$$

$$\frac{d \theta}{d {\cal T}} =- \frac{6}{5}Q {\cal R}^{1/2} \left(\frac{sin(\theta)cos(\theta)}{g_{\theta}} \right).$$

The above remain in spherical coordinates, where ${\cal R} = r c^{2}/GM$ 