Twists in the flow: Revisiting convective mixing in rotating stellar models - I. Effect on the stellar structure

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Table 1.

Change in overshooting-region mass fraction in rotating models.

Latitudinal	Minimum radiative-zone	Exponential overshoot	Rotational	ΔM_ov/M	ΔM_ov/M
dependence (θ)	mixing (`min_D_mix`)	threshold (`overshoot_D_min`)	mixing	(ZAMS, %)	(TAMS, %)
cos θ = 1	10	0.05	ES	18.7	21.6

$⟨ {cos}^{2} θ ⟩ = \frac{1}{3}$ $Mathematical equation: $ \boldsymbol{\langle \cos^2\theta \rangle = \frac{1}{3}} $$	10	0.05	ES	16.6	19.6
cos θ = 1	0	0.05	ES	20.6	19.5
cos θ = 1	0	1	ES	20.6	19
cos θ = 1	10	0.05	ES+SH+GSF+	18.7	21.6
			DSI+SSI

Notes. ΔM_ov/M, is the relative change in overshooting-region mass fraction due to R-MLT under different model assumptions. The first row corresponds to the fiducial model; deviations in subsequent rows are highlighted in bold.

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