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Fig. 2.


Relative difference between the radiative flux of the ω-model and the ESTER model as a function of co-latitude for a 15 M (top) and a 40 M (bottom) ZAMS-star with various angular velocity ratios. The black line corresponds to an evolved 15 M ESTER 2D model with ω = 0.9 and a fractional abundance of hydrogen in the convective core Xcore/X0 = 0.5. X0 is the initial hydrogen mass fraction at ZAMS. The minimum of each curve corresponds to a sign change of FESTER − Fω.

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