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Could a change in magnetic field geometry cause the break in the wind-activity relation?

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Figure

Table 1. Properties of the stars considered in this work. Rotation periodsthe remaining values are from WoodProt were derived in the associated ZDI work (references in Table 2), while 2004, Wood & Linsky 2010, Woodet al
Figure 1. Mass-loss rates per surface area versus X-ray fluxes showing only the stars for which we have reconstructed surface fields
Figure 2. Relation between Fx and ⟨B2tor⟩ does not show a break at Fx ∼106 erg cm−2 s−1

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