Turbulent Magnetic Dynamos with Halo Lags, Winds, and Jets
  This paper presents scale invariant/self-similar galactic magnetic dynamo
models based on the classic equations, and compares them qualitatively to
recently observed magnetic fields in edge-on spiral galaxies. We classify the
axially symmetric dynamo magnetic field by its separate sources, advected flux
and sub scale turbulence. We neglect the diffusion term under plausible
physical conditions. There is a time dependence determined by globally
conserved quantities. We show that magnetic scale heights increase with radius
and wind velocity. We suggest that AGN outflow is an important element of the
large scale galactic dynamo, based on the dynamo action of increasing sub scale
vorticity. This leads us to {\it predict} a correlation between the morphology
of coherent galactic magnetic field (i.e. extended polarized flux) and the
presence of an AGN.
