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Fig. 2.


Properties of the stellar model with + = 1 M yr−1 rotating at the ΩΓ-limit as a function of the stellar mass (time coordinate in case of constant accretion). Upper panel: stellar structure and the Alfvén radius. Blue areas are convective regions, and the grey area is the radiative zone. The black dotted lines are Lagrangian layers (iso-mass) of log Mr/M = 1, 2, 3, 4, and 5. Second panel: Eddington factor in log(1 − Γ). Grey dotted lines indicate Γ = 0.9 and 0.99. Third panel: constraint we impose on the angular velocity at the surface (ΩΓ-limit, Eq. (1)), as a ratio to the Keplerian velocity. Fourth panel: angular velocity of the envelope (in blue) and of the core (in grey). Fifth panel: angular momentum accretion rate (Keplerian, in grey), the time derivative of the stellar angular momentum (in blue), and the required angular momentum-loss rate (red dashed line) computed with Eq. (3). Last panel: magnetic field that is required at the stellar surface according to Eqs. (4)–(7).

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