Note that the Yale group computed the evolution of angular momentum using a simplified description of the action of meridional circulation, which was considered as a diffusive rather than as an advective process.

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The potential effect of internal gravity waves produced by the convective stellar core should be modest, although it remains to be quantified.

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... $\sqrt{\ell \left(\ell +1 \right)}$

This is the theoretical dependence. Damping can be enhanced by turbulence, which would reduce the surface amplitude of the mode (see e.g. Andersen 1996).

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... coefficient

The Gaussian we use here is quite thin. Far from a sharp shear layer, the convolution we are using would not alter the turbulent viscosity from that obtained with Eq. (5).

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... rotation

This mode does not carry angular momentum.

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... species

This adds to the indirect effect described above, that is, modification of the rotation profile which changes rotational mixing.

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... applied

However, the initial rotation profile has a surface convection zone rotating slower than the radiative interior.

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... moderate

This is the same as was used by TKZ.

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... smaller

In TKZ, the local turbulence was fixed (as in Eq. (4)) and did not depend on the local shear rate.

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... models

We showed in Talon & Charbonnel (2003) that in the type of star we consider for this full evolutionary computation (i.e., Pop I main sequence star with a mass of 1.2 $M_\odot$ ) the depth and structure of the convective envelope, and thus the wave characteristics, do not vary significantly over a main sequence lifetime. It is thus justified to perform the first test with the spectrum characteristics of the ZAMS models.

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