Solar magnetism - Observation and theory
Abstract
This introductory review consists of four parts. The first is a discussion of the concentration of magnetic flux into small elements, large electrical conductivity and superadiabatic stratification as the main reasons for these flux tubes, their relationship to the mean field, and the observational evidence for the latter. The second briefly repeats the approximations and merits of kinematic mean-field dynamos. In the form of the alpha-omega dynamo, this theory explains the reversals, latitude migration, dipolar parity, and other properties of the mean solar field. The third part treats the question of flux loss from the convection zone through the buoyancy force, with the conclusion that the dynamo most probably has its main shear region at the bottom of the convection zone or in a transition layer beneath it. The last part discusses further dynamic aspects of the sun's magnetism (e.g., models of limit cycles and models with chaotic behavior) and in particular the question of the phase stability of the solar cycle.
- Publication:
-
Astronomische Nachrichten
- Pub Date:
- 1984
- DOI:
- 10.1002/asna.2113050502
- Bibcode:
- 1984AN....305..215S
- Keywords:
-
- Dynamo Theory;
- Solar Magnetic Field;
- Solar Physics;
- Buoyancy;
- Kinematics;
- Long Term Effects;
- Magnetic Flux;
- Magnetic Variations;
- Solar Physics