Gary A. Glatzmaier

TL;DR: In this article, the authors presented the first 3D, time-dependent, self-consistent numerical solution of the magneto- hydrodynamic (MHD) equations that describe thermal convection and magnetic field generation in a rapidly rotating spherical fluid shell with a solid conducting inner core.

TL;DR: In this article, numerical modeling of mantle convection in a spherical shell with an endothermic phase change at 670 km depth reveals an inherently three-dimensional flow pattern, containing cylindrical plumes and linear sheets which behave differently in their ability to penetrate the phase change.

TL;DR: In this article, a series of computer simulations of the Earth's dynamo illustrates how the thermal structure of the lowermost mantle might affect convection and magnetic field generation in the fluid core.

TL;DR: In this paper, a numerical model used to simulate global convection and magnetic field generation in stars is described, where the velocity, magnetic field, and thermodynamic perturbations are expanded in spherical harmonics to resolve their horizontal structure and in Chebyshev polynomials to resolve the radial structure.

TL;DR: In this article, three-dimensional simulations of compressible, penetrative convection in rotating spherical shells in both laminar and turbulent parameter regimes are presented, where the convective structure is dominated by ii banana cells, and the turbulent case is much more complex, with an intricate, rapidly evolving down-ow network in the upper convection zone and an intermittent, plume-dominated structure in the lower convection region.