Mass loss and magnetospheres of massive stars

Abstract

About ten percent 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 and outflowing gas can be trapped. We use the Nirvana MHD code with adaptive mesh refinement to study this interaction with high numerical resolution to model cases with confinement parameters up to $10^4$.

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Cited by in corpus (6)

• The Magnetic Early B-type Stars IV: Breakout or Leakage? H$\alpha$ emission as a diagnostic of plasma transport in centrifugal magnetospheres
• A short and sudden increase of the magnetic field strength and the accompanying spectral variability in the O9.7V star HD54879
• Simulations of the line-driven instability in magnetic hot star winds
• Magnetic field geometry and magnetospheric environment of the strongly magnetic Of?p star NGC 1624-2
• Hot-star wind models with magnetically split line blanketing
• Intrinsic polarization of Wolf-Rayet stars due to the rotational modulation of the stellar wind