  Turbulence generated by large-scale motions during structure formation
affects the evolution of the thermal and non-thermal components of the
intracluster medium.
  As enstrophy is a measure of the magnitude of vorticity, we study the
generation and evolution of turbulence by analysing the Lagrangian history of
enstrophy. For this purpose we combine cosmological simulations carried out
with the ENZO-code with our Lagrangian post-processing tool CRaTer. This way we
are able to quantify the individual source terms of enstrophy in the course of
the accretion of groups onto galaxy clusters. Here we focus on the redshift
range from $z=1$ to $z=0$. Finally, we measure the rate of dissipation of
turbulence and estimate the resulting amplification of intracluster magnetic
fields.
  We find that compressive and baroclinic motions are the main sources of
enstrophy, while stretching motions and dissipation affect most of the ensuing
enstrophy evolution. The rate of turbulent dissipation is able to sustain the
amplification of intracluster magnetic fields to observed levels.
