HR: 1340h
AN: GP43A-0888    [Abstracts]
TI: A Saturian Dynamo Simulation
AU: * Glatzmaier, G A
EM: glatz@es.ucsc.edu
AF: Univ of California, Santa Cruz, Earth Sciences Department EMS Building, Santa Cruz, CA 95064 United States
AB: A 3D global computer simulation of thermal convection and magnetic field generation in Saturn is presented. Convection takes the form of many isolated small-scale vortices with their axes roughly aligned with the planetary rotation axis. Vorticity is generated and differential rotation is maintained by fluid flowing through the density stratification. The differential rotation manifests itself at the surface as a fairly time independent banded zonal wind profile, similar to Saturn's. This generates multiple, migrating, toroidal magnetic fields directed eastward and westward in both hemispheres. The field above the surface is dominantly an axial dipole.
DE: 0560 Numerical solutions (4255)
DE: 1510 Dynamo: theories and simulations
DE: 1595 Planetary magnetism: all frequencies and wavelengths
DE: 5734 Magnetic fields and magnetism
DE: 6275 Saturn
SC: Geomagnetism and Paleomagnetism [GP]
MN: Fall Meeting 2005