Threedimensional model for generation of the mean solar magnetic field
Abstract
A threedimensional (nonaxisymmetric) model for the solar mean magnetic field generation is studied. The sources of generation are the differential rotation and mean helicity in the convective shell. The system is described by two equations of the first order in time and the fourth order in space coordinates. The solution is sought for in the form of expansion over the spherical functions Y(m)_{n.} The modes of different m are separated. A finitedifference scheme similar to the PeacemanRachford scheme is constructed in order to find coefficients of the expansion depending on the time and radial coordinates. It is shown that a mode with a smaller azimuthal number m is primarily excited. The axisymmetric mode m = o describes the 22 year solar cycle oscillations. The modes of m o have no such periodicity, they oscillate with a period of rotation of the low boundary of the solar convective shell. The solutions which are symmetric relative to the equator plane are excited more easily compared with the antisymmetrical ones. The results obtained are confronted to the observational picture of the nonaxisymmetric largescale solar magnetic fields.
 Publication:

Astronomische Nachrichten
 Pub Date:
 1985
 DOI:
 10.1002/asna.2113060402
 Bibcode:
 1985AN....306..177I
 Keywords:

 Mathematical Models;
 Solar Magnetic Field;
 Solar Physics;
 Three Dimensional Models;
 Convection;
 Dynamo Theory;
 Finite Difference Theory;
 Harmonics;
 Solar Rotation;
 Solar Physics