Fig. 9.
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Influence of the stellar magnetic field strength, B⋆, initial rotation period, and viscous α parameter on the results for both metallicities Z = 1 Z⊙ (solid lines) and Z = 0.2 Z⊙ (dashed lines). The cyan, magenta, and orange lines show models MC1, MC2, and MC3, respectively. Panel a: same as Fig. 6. Panel b: same as Fig. 8 but without the post-disk contraction.
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