  We performed cosmological, magneto-hydrodynamical simulations to follow the
evolution of magnetic fields in galaxy clusters, exploring the possibility that
the origin of the magnetic seed fields are galactic outflows during the
star-burst phase of galactic evolution. To do this we coupled a semi-analytical
model for magnetized galactic winds as suggested by \citet{2006MNRAS.370..319B}
to our cosmological simulation. We find that the strength and structure of
magnetic fields observed in galaxy clusters are well reproduced for a wide
range of model parameters for the magnetized, galactic winds and do only weakly
depend on the exact magnetic structure within the assumed galactic outflows.
Although the evolution of a primordial magnetic seed field shows no significant
differences to that of galaxy clusters fields from previous studies, we find
that the magnetic field pollution in the diffuse medium within filaments is
below the level predicted by scenarios with pure primordial magnetic seed
field. We therefore conclude that magnetized galactic outflows and their
subsequent evolution within the intra-cluster medium can fully account for the
observed magnetic fields in galaxy clusters. Our findings also suggest that
measuring cosmological magnetic fields in low-density environments such as
filaments is much more useful than observing cluster magnetic fields to infer
their possible origin.
