On the origin of magnetic driven winds and the structure of the galactic
  dynamo in isolated galaxies
  We investigate the build-up of the galactic dynamo and subsequently the
origin of a magnetic driven outflow. We use a setup of an isolated disc galaxy
with a realistic circum-galactic medium (CGM). We find good agreement of the
galactic dynamo with theoretical and observational predictions from the radial
and toroidal components of the magnetic field as function of radius and disc
scale height. We find several field reversals indicating dipole structure at
early times and quadrupole structure at late times. Together with the magnetic
pitch angle and the dynamo control parameters $R_{\alpha}$, $R_{\omega}$ and
$D$ we present strong evidence for an $\alpha^2$-$\Omega$ dynamo. The formation
of a bar in the centre leads to further amplification of the magnetic field via
adiabatic compression which subsequently drives an outflow. Due to the
Parker-Instability the magnetic field lines rise to the edge of the disc, break
out and expand freely in the CGM driven by the magnetic pressure. Finally, we
investigate the correlation between magnetic field and star formation rate.
Globally, we find that the magnetic field is increasing as function of the star
formation rate surface density with a slope between $0.3$ and $0.45$ in good
agreement with predictions from theory and observations. Locally, we find that
the magnetic field can decrease while star formation increases. We find that
this effect is correlated with the diffusion of magnetic field from the spiral
arms to the inter-arm regions which we explicitly include by solving the
induction equation and accounting for non-linear terms.
