Kinematic Numerical Simulations of the Solar Dynamo: Dependence on α and Ω Values

We investigated the generation of dynamo waves in the solar convection zone through a numerical simulation. We integrated the axisymmetric alpha-Omega kinematic dynamo equations in a spherical geometry, where the alpha- and Omega-profiles depend on the spatial coordinates. The model results show that the fundamental parameter that determines the behavior of the system is the product between the characteristic intensities of the alpha and Omega contributions. In particular, we found three different regimes in which the system exhibits different behaviors: a regime without a dynamo effect, one with an exponential amplification of the magnetic field, and one with dynamo waves.