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We have performed 3D isothermal MHD simulation of a magnetic rotating massivestar with a non-zero dipole obliquity and predicted the radio/sub-mm observablelightcurves and continuum spectra for a frequency range compatible with ALMA.From these results we also compare the model input mass-loss to that calculatedfrom the synthetic thermal emission. Spherical and cylindrical symmetry isbroken due to the obliquity of the stellar magnetic dipole resulting in aninclination and phase dependence of both the spectral flux and inferredmass-loss rate, providing testable predictions of variability for obliquerotator. Both quantities vary by factors between 2 and 3 over a full rotationalperiod of the star, demonstrating that the role of rotation as critical inunderstanding the emission. This illustrates the divergence from a symmetricwind, resulting in a two armed spiral structure indicative of a obliquemagnetic rotator. We show that a constant spectral index, $\alpha$, modelagrees well with our numerical prediction for a spherical wind for$\nu~<~10^{3} \ \mathrm{GHz}$, however it is unable to capture the behavior ofemission at $\nu~>~10^{3} \ \mathrm{GHz}$. As such we caution the use of suchconstant $\alpha$ models for predicting emission from non-spherical winds suchas those which form around magnetic massive stars.

3D MHD simulations and synthetic radio emission from an oblique rotating magnetic massive star