Fig. 4.
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Profile of the squared Brunt–Väisälä frequency N2 and the relative error 
of the adopted approximation (Eq. (42)) as a function of ζ at different colatitudes θf using an ESTER model rotating at 60% of the Keplerian breakup rotation rate (The light orange area indicates the margin of error which we allow and the red hatched area represents the convective region of the star).
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