Over the last few years, with the increase of the computational power and the improvement in the observational techniques, there has been a substantial advance in the knowledge of our “Magnetic Star”. However, there is still a considerable number of open questions regarding the magneto-hydrodynamic processes that govern the large scale solar magnetic phenomena, i.e., the 11-years sunspot cycle, the polarity inversions of the magnetic field, or the coronal mass ejection. Here the currently accepted scenario for the solar dynamo process, together with the most recent numerical models and their results are reviewed. Particular attention is addressed to the construction and parallelism implementation of a numerical kinematic dynamo model and the ways by which it can be employed to obtain information about the solar internal structure.