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Solid body rotation is set at the zero age main sequence (ZAMS). Convective regions are calculated using the mixing length theory (MLT) in the \citet{Henyey:1965} formulation with $\alphaMLT=1.6$. Transport of angular momentum in convective regions is accounted for using the resulting MLT diffusion coefficient (turbulent diffusivity), which is generally very high and leads to rigid rotation in convective zones. While this seems to be the case in the Sun, another possible treatment of rotating convective zones is adopting a constant specific angular momentum \citep[See e.g.][]{Kawaler:2005}. We ran calculations with this assumption and found that it does not affect our conclusions. The boundaries of convective regions are determined using the Ledoux criterion. Semiconvection is accounted for in the Langer prescription \citep{Langer:1983,Langer:1985} with an efficiency $\alphasc$ = 0.003.   A step function overshooting extends for 0.2 pressure scale heights   the mixing region beyond the convective boundary during core H-burning. %MC: Check if it's also extending core He-burning  We also account for gravitational settling and chemical diffusion \citep{Paxton:2011}. Figure~\ref{kipp} shows Kippenhahn diagrams for the $1.5\msun$ $1.5\mso$  model.