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Fig. 11


X-ray luminosity vs. rotational period for h Per members, with masses ranging between 1.2 and 1.4 M (blue), and 1.0 and 1.2 M (red), compared with supersaturation behavior predicted from centrifugal stripping models (left panel) or polar updraft migration models (right panel), obtained considering different stellar masses (dashed gray lines in the right panel are computed assuming that the radiative core has a 30% higher rotation than the convective envelope).

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