On the Generation of the Largescale and Turbulent Magnetic Fields in the Solar Type Stars
Abstract
It is thought that the large-scale solar-cycle magnetic field is generated in a thin region at the interface of the radiative core (RC) and solar convection zone (SCZ). We show that the bulk of the SCZ virogoursly generates a small-scale turbulent magnetic field. Rotation, while not essential, increases the generation rate of this field.
- Publication:
-
Solar Physics
- Pub Date:
- June 1993
- DOI:
- 10.1007/BF00690652
- Bibcode:
- 1993SoPh..145..207D
- Keywords:
-
- Dynamo Theory;
- Magnetohydrodynamic Turbulence;
- Solar Convection (Astronomy);
- Solar Magnetic Field;
- Stellar Interiors;
- Chromosphere;
- Helices;
- Poloidal Flux;
- Solar Radiation;
- Stellar Rotation;
- Solar Physics;
- Solar Magnetic Field;
- Toroidal Field;
- Poloidal Field;
- Solar Convection Zone;
- Global Magnetic Field