Solar model computed with MESA. Left: Effective Rossby number as defined by Stevenson (1979) in Eq. (47) in the Sun’s convective zone. The region at the base of the convective zone and at the poles have the lowest Rossby number, then is the most affected by rotation. Centre: The same figure, but for the modulation of the convective velocity in the framework of R-MLT of Augustson & Mathis (2019). The convective velocity is diminished by 50% in the lowest Rossby number region, at the base of the convective zone. Right: Modification of the convective wave number with rotation, following Augustson & Mathis (2019). In the lowest Rossby number zone, the size of the convective eddies is the most diminished.