On the Generation of the Solar Magnetic Field in a Region of Weak Buoyancy
Abstract
The possibility that the cyclic magnetic field of the sun can be generated in a layer of weak buoyancy at the lower boundary of the solar convection zone (SCZ) is addressed using an eddy-damped quasi-normal Markovian closure model of the turbulent MHD equations. It is concluded that only models with kinetic energy of turbulent motion larger than roughly 10 to the 6th g/cm/s are viable. The action of differential rotation on this poloidal field generates a toroidal field exceeding the equipartition value which is sufficiently strong to interfere with the transport of heat and is amplified further in the SCZ.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- October 1990
- DOI:
- 10.1086/169308
- Bibcode:
- 1990ApJ...362..709D
- Keywords:
-
- Magnetic Flux;
- Plasma Turbulence;
- Solar Interior;
- Solar Magnetic Field;
- Buoyancy;
- Temporal Distribution;
- Turbulence Effects;
- Solar Physics;
- HYDROMAGNETICS;
- SUN: INTERIOR;
- SUN: MAGNETIC FIELDS