Thin shell dynamo models consistent with Mercuryʹs weak observed magnetic field

Energetic and magnetostrophic balance arguments show that a dynamo source for Mercuryʹs observed magnetic field is problematic if one expects an Earth-like partitioning of toroidal and poloidal fields. We perform 3-dimensional numerical dynamo simulations to determine if a thin shell dynamo geometry for Mercury could produce non-Earth-like magnetic field partitioning and therefore provide a possible explanation of Mercuryʹs weak observed dipole signature. We examine the ratio of the dipole field at the core–mantle boundary to the toroidal field in the core for various shell thicknesses and Rayleigh numbers and find that some thin shell dynamos can produce magnetic fields with Mercury-like dipolar field intensities. In these dynamos, the toroidal field is produced more efficiently through differential rotation than the poloidal field is produced through upwellings interacting with the toroidal field. The poloidal field is also dominated by smaller-scale structure which was not observable by the Mariner 10 mission, compared to the dipole field.