Volume rendering of radial magnetic field
A simulation of the convection-driven flow of an electrically conductive fluid in a rotating spherical shell. The fluid motion generates a self-sustaining magnetic field. Such simulations are used to approximate conditions, which generate planetary and solar magnetic fields. This particular solution is a community benchmark for testing different computational methods, and is stationary aside from azimuthal drift. The image shows evolution of radial velocity from initial to steady state from left to right. The small inset image at the center provides the section of sphere being displayed in larger images.