  Supernovae are the dominant energy source for driving turbulence within the
interstellar plasma. Until recently, their effects on magnetic field
amplification in disk galaxies remained a matter of speculation. By means of
self-consistent simulations of supernova-driven turbulence, we find an
exponential amplification of the mean magnetic field on timescales of a few
hundred million years. The robustness of the observed fast dynamo is checked at
different magnetic Reynolds numbers, and we find sustained dynamo action at
moderate Rm. This indicates that the mechanism might indeed be of relevance for
the real ISM.
  Sensing the flow via passive tracer fields, we infer that SNe produce a
turbulent alpha effect which is consistent with the predictions of quasilinear
theory. To lay a foundation for global mean-field models, we aim to explore the
scaling of the dynamo tensors with respect to the key parameters of our
simulations. Here we give a first account on the variation with the supernova
rate.
