The large-scale internal solar magnetic field
Abstract
It is hypothesized that, during the collapse of the protosolar cloud, the magnetic field intensified. In the center of the just-formed, nonturbulent sun, the intensity of the magnetic field was 10,000 to 1 million G. If the sun passed through a stage of turbulent convection, only the field generated by dynamo action would remain. The poloidal magnetic field at this stage could reach 1000-1,000,000 G, but the intensity would decrease to 10-1 G during the decay of turbulent convection. The toroidal magnetic field would remain at 1000-1,000,000 G. It is possible that nonuniform rotation of the radiative region is related to distortions in the angular velocity in the internal convective zone due to magnetic tension.
- Publication:
-
Astronomicheskii Zhurnal
- Pub Date:
- August 1989
- Bibcode:
- 1989AZh....66..809D
- Keywords:
-
- Dynamo Theory;
- Magnetohydrodynamics;
- Solar Interior;
- Solar Magnetic Field;
- Solar Radiation;
- Convection;
- Rotating Matter;
- Star Formation;
- Stellar Evolution;
- Solar Physics