Solar Surface Magneto-Convection
Abstract
We review the properties of solar magneto-convection in the top half of the convection zones scale heights (from 20 Mm below the visible surface to the surface, and then through the photosphere to the temperature minimum). Convection is a highly non-linear and nonlocal process, so it is best studied by numerical simulations. We focus on simulations that include sufficient detailed physics so that their results can be quantitatively compared with observations.
- Publication:
-
Living Reviews in Solar Physics
- Pub Date:
- July 2012
- DOI:
- 10.12942/lrsp-2012-4
- Bibcode:
- 2012LRSP....9....4S
- Keywords:
-
- pores;
- magnetic fields;
- convection;
- solar physics;
- flux emergence;
- sunspots;
- dynamo;
- Magnetic Flux;
- Flux Tube;
- Convection Zone;
- Convective Motion;
- Dynamo Action