Does mantle convection currently exist on Mercury?

The full equations of convective motion over the age of the solar system can be solved in a few hours (2D) to several weeks (3D) with numerical simulations in Cartesian or spherical geometry. Using the 2D, Cartesian geometry code, ConMan, we model the thermal evolution of Mercury. Our preferred calculation has an initial Rayleigh number of 8 × 104, no mantle internal heating, and a constant core heat flux of 9.75 mW/m2 in a non-Newtonian rheology. These values all fall within the range of previously estimated parameters from 1D calculations, and allow for weak mantle convection to persist until present, supporting the outer core dynamo explanation of Mercuryʹs intrinsic magnetic field. Further, the peak dynamic topography and geoid anomalies from our model are about 179 m and 37 m, respectively—values that are not unrealistic and should be well within the range of observation by the MESSENGER spacecraft. Future spacecraft observations, yielding new and more accurate data, will help us better understand the thermal evolution of Mercury and the origin of its magnetic field.