We continue simulations of SN-driven turbulence in the ISM under conditions representative for the outer gas disks. Especially the role of shear in radial and vertical direction should be investigated. X-shaped halo magnetic fields are possibly a consequence of MRI-modes, which will be studied by global disk simulations. The local box simulations provide the input of the sub-grid physics for global models of galaxies. After the successful implementation in the M-Gadget code we propose simulations of global galaxy evolution models within a cosmological context. We expect a better understanding for the magnetisation of the IGM and a possible dynamic effect of the magnetic fields in the halo, where the Alfvén velocity is of the order of the circular velocity.
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