Parker's model in geodynamo

M. Reshetnyak

Institute of Physics of the Earth, 10 B.~Gruzinskaya str., Moscow 123995, Russia

Abstract
It is considered how information on geostrophic flows in the planetary cores obtained from 3D simulations in a sphere can be used in a 2D Parker's geodynamo model with simple forms of the α-quenching. Using cluster computer systems, the dependence of the dynamo equations' solution on the magnitudes of the α- and ω-effects is studied. It is shown that geostrophical flow can produce the well-known Z-structure of the poloidal magnetic field without the feed-back of the magnetic field onto the large-scale velocity field. The influence of the fluctuations of the α-effect on the magnetic field generation, its spectral properties in respect to geodynamo applications is also discussed. Figs 4, Refs 24.