  We present results of 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 the rotational
variability of radio and sub-mm emission. 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
observable properties should be apparent in multiple wavelengths. This
structure is analysed to calculate free-free thermal radio emission and
determine the characteristic intensity maps and radio light curves.
