Fig. 6.

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Illustration for the structure of the system for the magnetic interpretation. The spinning subdwarf (in blue) generates a dipolar magnetic field around it, which is not necessarily aligned with the spin. The wind material in the innermost region, within Kepler radius RK, has no centrifugal support and can fall freely back onto the star, thus forming a dynamical magnetosphere. The material between the Keplerian co-rotation radius RK and the Alfvén radius RA has centrifugal support. It cannot fall back onto the star, thus forming a much denser rigidly rotating magnetosphere. The illustration is inspired by Petit et al. (2013).
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