MHD outflow mechanisms developed mostly for low-mass protostars can be simply scaled up to high mass accretors. Again the high output of UV radiation will increase the ionization fraction and hence, the coupling of magnetic field with the material. The onset of a radiative envelope (e.g. Palla & Stahler 1992) in the star as it adopts a more main sequence structure removes the usual method for the generation of strong stellar surface magnetic fields. This may take away the driving force in the widely used X-wind model for protostellar outflows. Outflow mechanisms driven by magnetic fields generated or dragged in by the disc could still operate if a strong stellar field is absent (Banerjee & Pudritz 2006). Krumholz et al. (2005b) have made an initial investigation of how outflows affect accretion onto massive stars As expected, the punching of holes along the axis by these flows allows the radiation pressure to be relieved in the centre, and accretion to continue to higher masses still.

![SMA image of the 325 GHz dust emission from the massive YSO Cep A2. Dark contours show the integrated emission from the CH$_{3}$CN J=18-17 transition that shows a rotational kinematic signature consistent with a disc origin. 