  Initial results are presented from 3D MHD modelling of stellar-wind bubbles
around O stars moving supersonically through the ISM. We describe algorithm
updates that enable high-resolution 3D MHD simulations at reasonable
computational cost. We apply the methods to the simulation of the astrosphere
of a rotating massive star moving with 30 km/s through the diffuse interstellar
medium, for two different stellar magnetic field strengths, 10 G and 100 G.
Features in the flow are described and compared with similar models for the
Heliosphere. The shocked interstellar medium becomes asymmetric with the
inclusion of a magnetic field misaligned with the star's direction of motion,
with observable consequences. When the Alfvenic Mach number of the wind is
$\leq$10 then the stellar magnetic field begins to affect the structure of the
wind bubble and features related to the magnetic axis of the star become
visible at parsec scales. Prospects for predicting and measuring non-thermal
radiation are discussed.
