Convection zones in sun and stars.
Abstract
Aspects of the current understanding of the nature, description and observational properties of solar and stellar convection zones are discussed. The origin of a convective zone as a result of the increase in the luminosity/mass ratio of a star in its center and increases in the opacity in the outer layers of a star is discussed, and the standard mixing length treatment of the ensuing envelope convection is presented. The expected effects of convective motions are examined in order to demonstrate the inadequacy of the standard approach in accounting for the generation of kinetic energy and the transport of angular momentum and magnetic field, and alternative hydrodynamic approaches are described. Observations of solar oscillations and supergranulation and stellar atmospheres, rotation rates and orbital eccentricities which have a bearing on the properties and existence of convection zones are also noted.
- Publication:
-
Solar Phenomena in Stars and Stellar Systems
- Pub Date:
- 1981
- Bibcode:
- 1981ASIC...68..123Z
- Keywords:
-
- Convective Flow;
- Magnetohydrodynamics;
- Mixing Length Flow Theory;
- Stellar Envelopes;
- Stellar Luminosity;
- Stellar Magnetic Fields;
- Angular Momentum;
- Kinetic Energy;
- Solar Oscillations;
- Stellar Atmospheres;
- Stellar Mass;
- Astrophysics;
- Convection:Stars;
- Solar Convective Zones