To generate a self-sustained magnetic field on terrestrial planets, the convection of a metallic liquid outer core is necessary (Breuer, 2019). Liquid core convection may be driven by thermal buoyancy from superadiabatic heat flows (thermal dynamo) across the core-mantle boundary (CMB) or by compositional buoyancy from the exsolution of light elements (e.g., O, C, and Si) at the inner-core boundary (ICB) (chemical dynamo;