Magnetic field and their related dynamical effects are thought to be important in stellar radiation zones. For instance, it has been suggested that a dynamo, sustained by a m=1 MHD instability of toroidal magnetic fields (discovered by Tayler in 1973), could lead to a strong transport of angular momentum and of chemicals in such stable regions. We wish here to recall the different magnetic transport and mixing processes present in radiative zone and show how the dynamo can operate by recalling the conditions required to close the dynamo loop (Bpol -> Btor -> Bpol). Helped by high-resolution 3D MHD simulations of the solar radiation zone using the ASH code, we confirm the existence of Tayler's m=1 instability, study its non linear saturation, but we do not detect, up to a magnetic Reylnods number of 10^5, any dynamo action. Finally we summarize our current understanding of magnetic transport mechanisms in stellar radiation regions.