  Magnetic Towers represent one of two fundamental forms of MHD outflows.
Driven by magnetic pressure gradients, these flows have been less well studied
than magneto-centrifugally launched jets even though magnetic towers may well
be as common. Here we present new results exploring the behavior and evolution
of magnetic tower outflows and demonstrate their connection with pulsed power
experimental studies and purely hydrodynamic jets which might represent the
asymptotic propagation regimes of magneto-centrifugally launched jets.
High-resolution AMR MHD simulations (using the AstroBEAR code) provide insights
into the underlying physics of magnetic towers and help us constrain models of
their propagation. Our simulations have been designed to explore the effects of
thermal energy losses and rotation on both tower flows and their hydro
counterparts. We find these parameters have significant effects on the
stability of magnetic towers, but mild effects on the stability of hydro jets.
Current-driven perturbations in the Poynting Flux Dominated (PDF) towers are
shown to be amplified in both the cooling and rotating cases. Our studies of
the long term evolution of the towers show that the formation of weakly
magnetized central jets within the tower are broken up by these instabilities
becoming a series of collimated clumps which magnetization properties vary over
time. In addition to discussing these results in light of laboratory
experiments, we address their relevance to astrophysical observations of young
star jets and outflow from highly evolved solar type stars.
