Non-linear three-mode coupling of gravity modes in rotating slowly pulsating B stars - Stationary solutions and modeling potential

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Table 1.

Model parameters of the MESA model grid.

Model	M_ini (M_⊙)	X_c	Z_ini	f_CBM	$log (\frac{D_{env, \min}}{{cm}^{2} s^{- 1}})$ $\log(\tfrac{{D}_{\mathrm{env, min}}}{\mathrm{cm}^2\,\mathrm{s}^{-1}})$
Fiducial	4.0	0.09	0.014	0.02	2.00
ΔX_c, 1	4.0	0.29	0.014	0.02	2.00
ΔX_c, 2	4.0	0.59	0.014	0.02	2.00
ΔM_ini, 1	6.0	0.09	0.014	0.02	2.00
ΔX_c\|M_ini	6.0	0.29	0.014	0.02	2.00
ΔM_ini, 2	8.0	0.09	0.014	0.02	2.00

Notes.

Columns are initial mass M_ini, core hydrogen mass fraction X_c, initial metallicity Z_ini, exponential overshoot efficiency f_CBM, and the logarithm of the minimal radiative envelope mixing level D_env, min.

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