Magnetic effects on fields morphologies and reversals in geodynamo simulations

International audienceThe dynamo eect is the most popular candidate to explain the non-primordial magnetic elds of astrophysical objects. Although many systematic studies of parameters have already been made to determine the dierent dynamical regimes explored by direct numerical geodynamo simulations, it is only recently that the regime corresponding to the outer core of the Earth characterized by a balance of forces between the Coriolis and Lorentz forces is accessible numerically. In most previous studies, the Lorentz force played a relatively minor role. For example, they have shown that a purely hydrodynamic parameter (the local Rossby number Ro) determines the stability domain of dynamos dominated by the axial dipole (dipolar dynamos). In this study, we show that this result cannot hold when the Lorentz force becomes dominant. We model turbulent geodynamo simulations with a strong Lorentz force by varying the important parameters over several orders of magnitude. This method enables us to question previous results and to argue on the applications of numerical dynamos in order to better understand the geodynamo problem. Strong dipolar elds considerably aect the kinetic energy distribution of convective motions which enables the maintenance of this eld conguration. The relative importance of each force depends on the spatial length scale, whereas Ro is a global output parameter which ignores the spatial dependency. We show that inertia does not induce a dipole collapse as long as the Lorentz and the Coriolis forces remain dominant at large length scales