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The results of 3D numerical simulations modelling the twisting of a coronal loop due to photospheric vortex motions are presented. The simulations are carried out using an initial purely axial field and an initial equilibrium configuration with twist, Φ = LB θ /rBz < Φcrit. The non-linear and resistive evolutions of the instability are followed. The magnetic field is twisted by the boundary motions into a loop which initially has boundary layers near the photospheric boundaries as has beendoi:10.1051/0004-6361:20020491 fatcat:7l4wflg6unhgdmxiicoyk3tdcm