Ratio of rotation rate between the convective core and the near-core radiative interior probed by gravity modes, as a function of the central hydrogen abundance in mass fraction for models without internal magnetic fields. The effect of initial rotation rates (top), metallicity (middle), and initial mass (bottom) are illustrated in each panel. All models are computed assuming uniform rotation as an initial condition, except for the model in light-blue dashed line in the top panel where we assumed that initially the convective core rotates faster than the near-core regions.