The evolution of high and low mass planets embedded in
turbulent magnetised discs has been studied by means of
MHD simulations. For high mass planets, the picture that
emerges is similar to that obtained for viscous, laminar
disc models. For low mass planets, however, the usual type I
migration picture is modified, and the planets undergo a
process of stochastic migration. I will present the results
of recent simulations, and discuss their broader significance
in the context of planet formation.
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