The supernova-regulated ISM -- VI. Magnetic effects on the structure of
  the interstellar medium
  We explore the effect of magnetic fields on the vertical distribution and
multiphase structure of the supernova-driven interstellar medium (ISM) in
simulations that admit dynamo action. As the magnetic field is amplified to
become dynamically significant, gas becomes cooler and its distribution in the
disc becomes more homogeneous. We attribute this to magnetic quenching of
vertical velocity, which leads to a decrease in the cooling length of hot gas.
A non-monotonic vertical distribution of the large-scale magnetic field
strength, with the maximum at |z| $\approx$ 300 pc causes a downward pressure
gradient below the maximum which acts against outflow driven by SN explosions,
while it provides pressure support above the maximum.
