We present results of 2D and 3D numerical simulations of magnetically confined, radiatively driven stellar winds of massive stars, conducted using the astrophysical MHD code Pluto, with a focus on understanding radio and sub-mm emission. The model assumes that a rigid magnetic field co-rotating with the star completely dominates the stellar atmosphere within the Alfven radius. Radiative driving is implemented according to the Castor, Abbott and Klein theory of radiatively driven winds. Many magnetic massive stars posses a magnetic axis which is inclined with respect to the rotational axis. This misalignment leads to a complex wind structure as magnetic confinement, centrifugal acceleration and radiative driving act to channel the circumstellar plasma into a warped disk whose properties should be apparent at low frequencies. Parameters such as the mass-loss rate, magnetic field strength, rotational period, magnetic and rotational axis misalignment are investigated.