A simple numerical model of the self-excitation of the magnetic field
by chaotic motion of a highly conductive fluid is being developed. It
is based on the following approach to simulating the turbulent dynamo
generation of magnetic fields: the fluid is divided into cells and eac
h cell acts as a machine that can randomly amplify or destroy a given
magnetic field. The random amplification models the effects of a chaot
ic fast dynamo and the random destruction models the effects of reconn
ection. Uncorrelated and correlated processes are considered. Effects
of non-linearity, diffusion, and correlation between cells in time and
space are also included. Numerical results are presented from one- an
d two-dimensional models and possible applications to the generation a
nd spatial-temporal distribution of solar, planetary and interplanetar
y magnetic fields are discussed.