Abstract: We present an extensive study on the dynamo origin of solar-type star's magnetism, based on a large series of 3D MHD numerical simulations with the ASH code performed within the pan-European ERC project Whole Sun. We assess how the combination of rotation and convection via the Rossby number influences the type of magnetism established (short or long cycles, statistically steady activity) and their expected differential rotation (solar-like, anti-solar, cylindrical or almost solid). This large survey allows us to explain why the Sun possesses a long decadal cycle and a conical differential rotation. We further assess the amount of energy needed to maintain such angular velocity profiles and magnetic activity. We find that between 0.1 and 3% of the stellar luminosity can be converted into magnetic energy, giving plenty of energy for surface eruptive events to occur. We also compute the magnetic energy spectra and show that the dipole and quadrupole magnetic fields do not collapse in amplitude when the rotation regime becomes anti-solar in agreement with spectropolarimetric observations, and as such cannot simply explain a break of gyrochronology for large Rossby number.
Finally, we discuss various scaling laws that this study allows to derive and that could be tested with dedicated observations, completing the current observational database. In particular, 2 regimes at low and high Rossby number seems particularly interesting to further quantify and model.
I will perhaps also briefly describe our new Dyablo AMR code for stellar convection and dynamo.