Abstract
About 10% of all OB stars show strong, large‐scale surface magnetic fields. The interaction of the magnetic field and the wind is believed to be the cause for the X‐ray emission shown by these objects. We, therefore, run numerical simulations in two dimensions for a number the O‐type stars and Wolf–Rayet stars to study the interaction of the stellar magnetic fields of these stars with their winds. While weak dipolar magnetic fields leave the wind largely unmodified, and the field opens up and becomes a split monopole, the interaction between magnetic field and outflowing gas is more complex, as the magnetic field remains closed in some regions, causing the outflowing gas to be trapped. We use the Nirvana Magnetohydrodynamics (MHD) code with adaptive mesh refinement to study this interaction with high numerical resolution to model cases with containment parameters up to 104.
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