Fig. 1
Angular velocity Ω = uϕ/r in terms of the Keplerian angular velocity for a central star with mass M∗ = 1.0 M⊙ and five different stellar rotation rates Ω∗, denoted by ω = Ω∗/ΩK(R∗). The plot depicts two regions separated by a light grey bar that differ in the radial scaling and enable us to show both the rapid variation in the BL and the constant overall trend.
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